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    December 24

    As Long As We Got Each Other

    As Long As We Got Each Other

    Show me that smile again
    Oh, show me that smile
    Don't waste another minute on your cryin'
    We're nowhere near the end
    We're nowhere near
    The best is ready to begin

    All in a cloudy daze
    I look into your eyes and see them shining out
    Holding you close this way
    Holding you this way
    Is like having summer everyday
    Ooh, ooh

    As long as we got each other
    We got the world spinnin' right in our hands
    Baby, you and me
    We gotta be
    The luckiest dreamers who never quit dreamin'

    As long as we keep on givin'
    We can take anything that comes our way
    Baby, rain or shine
    All the time
    We got each other
    Sharin' the laughter and love

    Promise me here and now
    Nothing but jokes
    Will never come between us
    You can depend on me
    'Cause I need you like the air I breathe
    Oh, oh

    As long as we got each other
    We got the world spinnin' right in our hands
    Baby, you and me
    We gotta be
    The luckiest dreamers who never quit dreamin'
    As long as we keep on givin'
    We can take anything that comes our way
    Baby, rain or shine
    All the time
    We got each other
    Sharin' the laughter and love

    As long as we got each other
    We got the world spinnin' right in our hands
    Baby, you and me
    We gotta be
    The luckiest dreamers who never quit dreamin'

    As long as we keep on givin'
    We can take anything that comes our way
    Oh, baby, rain or shine
    All the time
    We got each other
    Sharin' the laughter and love

    涡 街 流 量 计 原理

    http://www.chinaflow.com.cn/basic/wojie1.htm

    http://www.sensorok.com/tech/wjllyl37.htm

    涡街流量计的原理

        1.卡门涡街的产生与现象

        为说明卡门涡街的产生,我们来考虑粘性流体绕流圆柱体的流动.当流体速度很低时,流体在前驻点速度为零,来流沿圆柱左右两侧流动,在圆柱体前半部分速度逐渐增大,压力下降,后半部分速度下降,压力升高,在后驻点速度又为零.这时的流动与理想流体统流圆柱体相同,无旋涡产生,如图3—7a所示.

        随着来流速度增加,圆柱体后半部分的压力梯度增大,引起流体附面层的分离,如图3—7b所示.当来流的雷诺数Re再增大,达到40左右时,由于圆柱体后半部附面层中的流体微团受到更大的阻滞,就在附面层的分离点S处产生一对旋转方面相反的对称旋涡.如图3-7c所示.

    在一定的留诺数Re范围内,稳定的卡门涡街的及旋涡脱落频率与流体流速成正比.

    图3-7   圆柱绕涡街产生示意图

    2.卡门涡街的稳定条件

    并非在任何条件下产生的涡街都是稳定的.冯·卡门在理论上已证明稳定的涡街条件是:涡街两列旋涡之间的距离为h,单列两涡之间距离为 ,若两者之间关系满足

                             =1

                  或                  h / =0. 281                     (3-24)

    时所产生的涡街是稳定的。

        3.涡街运动速度

    为了导出旋涡脱落频率与流速之间的关系,首先要得到涡街本身的运动速度 .为便于讨论,我们假定在旋涡发生体上游的来源是无旋、稳定的流动,即其速度环量为零.从汤姆生定理可知,在旋涡发生体下游所产生的两列对应旋涡的速度环量 ,必然大小相等,方向相反,其合环量为零,由于对应两涡的旋向相反,速度环量大小相等,所以在整个涡群的相互作用下,涡街将以一个稳定的速度 向上游运动.从理论计算可得. 的表示式为

                  tan h                                 (3-25)

    对于稳定的涡街,将式(3-25)代入,有:

                = tan h(0. 281 )=                        (3-26)

    4.流体流速与旋涡脱落频率的关系

        从前面讨论可知,当流体以流速u流动时,相对于旋涡发生体,涡街的实际向下游运动速度为u-ur.如果单列旋涡的产生频率为每秒f个旋涡,那么,流速与频率的关系为

                           u-ur = fl                        (3-27)

        将式(3-26)代入,可得到流速u与旋涡脱落频率f之间的关系.但是,在实际上不可能测得速度环量 的数值,所以只能通过实验来确定来流速度u与涡街上行速度ur之间的关系,确定因注形旋涡发生体直径d与涡街宽度h之间的关系,有:

    h=1. 3d                        (3-28)

    ur=0. 14u                       (3-29)

    将式(3-24),(3-27),(3-28),(3-29)联立,可得:

                      f=        (3-29’)

                      0. 2u / d

    也可将上式写成:

                      St= 0. 2                        (3-30)

    St称为斯特罗哈数.从实验可知,在雷诺数Re为3×l02-3×l05范围内,流体速度u与旋涡脱落频率的关系是确定的.也就是说,对于圆柱形旋涡发生体,在这个范围内它的斯特罗哈数St是常数,并约等于0.2,与理论计算值吻合的很好.对于圆柱型式的旋涡发生体,其斯特罗哈数St也是常数,但有它自己的数值.图3-8为圆往型旋涡发生体产生的涡街结构.

    根据以上分析,从流体力学的角度可以判定涡街流量计测量的上下限流量为:Re=3×102-2×l05.当雷诺数更大时,圆柱体周围的边界层将变成紊流,不符合上述规律,并且将会是不稳定的.

    图3-8     涡街结构示意图

    5.流体振动原理

        当涡街在旋涡发生体下游形成以后,仔细观察其运动,可见它一面以速度u-ur平行于轴线运动,另外还在与轴线垂直方向上振动.这说明流体在产生旋涡的同时还受到一个垂直方向上力的作用.下面讨论这个垂直方向上力的产生原因及计算方法.

    同前讨论,假定来流是无旋的,根据汤姆生定律:沿封闭流动流线的环量不随时间而改变.那么,当在旋涡发生体右(或左)下方产生一个旋涡以后,必须在其它地方产生一个相反的环量,以使合环量为零.这个环量就是旋涡发生体周围的环流.根据茹科夫斯基的升力定理,由于这个环量的存在,会在旋涡发生体上产生一个升力,该升力垂直于来流方向.设作用在旋涡发生体每单位长度上的升力为L,有:

                     L= u                             (3-31)

    式中   ――流体密度;

            u――来流速度;

    * ――旋涡发生体的速度环量.

        从前面的讨论中可以得到以下关系,

    *   =2 ur;ur=K1u; =K2d ;

        将上述关系代入式(3—1),并令系数K=2 K1K2,则有:

                        L=K du2                             (3-32)

        这就是作用在旋涡发生体上的升力.由于旋涡在旋涡发生体两侧交替发生,且旋转方向相反,故作用在发生体上的力亦是交替变化的.而流体则受到发生体的反作用力,产生垂直于铀线方向的振动,这就是流体振动的原理.

        从上述分析可以知道:交替地作用在旋涡发生体上升力的频率就是旋涡的脱落频率.通过检测该升力的变化频率,就可以得到旋涡的脱落频率,从而可得流体的流速值。

        6.流量公式

    涡街流量计是一种速度式流量计,它测的是流体的流速u.为得到流量值,必须乘以流通截面积A.对于不同形式的旋涡发生器,它的流通截面积计算是不同的.以下仅举圆柱形流通截面积A可表示为

                      A≈ (1-1. 25 )                     (3-33)

    由此可得流量公式为

                     qv=Au= (1-1. 25 )             (3-34)

    从该式可知,流量qv与旋涡脱落频率f在一定雷诺数范围内成线性关系。因此,也将这种流量计称为线性流量计。

    The Ideal Gas Law

    The Ideal Gas Law

    The Ideal Gas Law

    The volume (V) occupied by n moles of any gas has a pressure (P) at temperature (T) in Kelvin. The relationship for these variables, P V = n R T,where R is known as the gas constant, is called the ideal gas law or equation of state. Properties of the gaseous state predicted by the ideal gas law are within 5% for gases under ordinary conditions. In other words, given a set of conditions, we can predict or calculate the properties of a gas to be within 5% by applying the ideal gas law. How to apply such a law for a given set of conditions is the focus of general chemistry.

    At a temperature much higher than the critical temperature and at low pressures, however, the ideal gas law is a very good model for gas behavior. When dealing with gases at low temperature and at high pressure, correction has to be made in order to calculate the properties of a gas in industrial and technological applications. One of the common corrections made to the ideal gas law is the van der Waal's equation, but there are also other methods dealing with the deviation of gas from ideality.

    The Gas Constant R

    Repeated experiments show that at standard temperature (273 K) and pressure (1 atm or 101325 N/m2 ), one mole (n = 1) of gas occupies 22.4 L volume. Using this experimental value, you can evaluate the gas constant R,
        P V   1 atm 22.4 L
    R = --- = ------------
        n T   1 mol 273 K
    
      = 0.08205 L atm / (mol·K)
    

    When SI units are desirable, P = 101325 N/m2 (Pa for pascal) instead of 1 atm. The volume is 0.0224 m3. The numberical value and units for R is

         101325 N/m2 0.0224 m3
    R = ----------------------
           1 mol 273 K
    = 8.314 J / (mol·K)
    Note that 1 L atm = 0.001 m3 x 101325 N / m2 = 101.325 J (or N m). Since energy can be expressed in many units, other numerical values and units for R are frequently in use.

    For your information, the gas constant can be expressed in the following values and units.

    R = 0.0805 L atm / mol·K        Notes:
      = 8.3145 L kPa / mol·K        1 atm = 101.32 kPa
      = 8.3145    J  / mol·K        1 J = 1 L kPa 
      = 1.987   cal  / mol·K        1 cal = 4.182 J
      = 62.364 L torr/ mol·K        1 atm = 760 torr
    
    The gas constant R is such a universal constant for all gases that its values are usually listed in the "Physical Constants" of textbooks and handbooks. It is also listed in
    Constants of our HandbookMenu at the left bottom. Although we try to use SI units all the time, the use of atm for pressure is still common. Thus, we often use R = 8.314 J / (mol·K) or 8.3145 J / mol·K.

    The volume occupied by one mole, n = 1, of substance is called the molar volume, Vmolar = V / n. Using the molar volume notation, the ideal gas law is:

    P Vmolar = R T

    Applications of the Ideal Gas Law

    The ideal gas law has four parameters and a constant, R,

    P V = n R T, and it can be rearranged to give an expression for each of P, V, n or T. For example, P = n R T / V,   (Boyles law)
    P = (n R / V) T   (Charles law)
    These equations are Boyles law and Charles law respectively. Similar expressions can be derived for V, n and T in terms of other variables. Thus, there are many applications. However, you must make sure that you use the proper numerical value for the gas constant R according to the units you have for the parameters.

    Furthermore, n / V is number of moles per unit volume, and this quantity has the same units as the concentration (C). Thus, the concentration is a function of pressure and temperature,

    C = P / R T. At 1.0 atm pressure and room temperature of 298 K, the concentration of an ideal gas is 0.041 mol/L.

    The Avogadros law can be further applied to correlate gas density d (weight per unit volume or n M / V) and molecular mass M of a gas. The following equation is easily derived from the ideal gas law:

              n M
       P M =  --- R T
               V 
    
    Thus, we have P M = d R T / M
    d = n M / V - definition, and
    d = P M / R T
    M = d R T / P

    Example 1

    An air sample containing only nitrogen and oxygen gases has a density of 1.3393 g / L at STP. Find the weight and mole percentages of nitrogen and oxygen in the sample.

    Solution


    From the density d, we can evaluate an average molecular weight (also called molar mass). P M = d R T
    M = 22.4 * d

      = 22.4 L/mol * 1.3393 g/L
      = 30.0 g / mol
    Assume that we have 1.0 mol of gas, and x mol of which is nitrogen, then (1 - x) is the amount of oxygen. The average molar mass is the mole weighted average, and thus, 28.0 x + 32.0 (1 - x) = 30.0
    - 4 x = - 2
    x = 0.50 mol of N2, and 1.0 - 0.50 = 0.50 mol O2
    Now, to find the weight percentage, find the amounts of nitrogen and oxygen in 1.0 mol (30.0 g) of the mixture. Mass of 0.5 mol nitrogen = 0.5 * 28.0 = 14.0 g
    Mass of 0.5 mol oxygen = 0.5 * 32.0 = 16.0 g
    Percentage of nitrogen = 100 * 14.0 / 30.0 = 46.7 % Percentage of oxygen = 100 * 16.0 / 30.0 = 100 - 46.7 = 53.3 %

    Discussion
    We can find the density of pure nitrogen and oxygen first and evaluate the fraction from the density.

    d of N2 = 28.0 / 22.4 = 1.2500 g/L
    d of O2 = 32.0 / 22.4 = 1.4286 g/L
    1.2500 x + 1.4286 (1 - x) = 1.3393
    Solving for x gives
    x = 0.50 (same result as above)

    Exercise
    Now, repeat the calculations for a mixture whose density is 1.400 g/L.

    Example 2

    What is the density of acetone, C3H6O, vapor at 1.0 atm and 400 K?

    Solution


    The molar mass of acetone = 3*12.0 + 6*1.0 + 16.0 = 58.0. Thus, d = P M / R T
      = (1.0 * 58.0 atm g/mol) / (0.08205 L atm / (mol K) * 400 K)
      = 1.767 g / L

    Exercise
    The density of acetone is 1.767 g/L, calculate its molar mass.

    Confidence Building Questions

    • What is the variable n stand for in the ideal gas law, P V = n R T?
    • Hint . . .number of moles of gas in a closed system.

      Skill:
      Describe the ideal gas law.

    • A closed system means no energy or mass flow into or out of a system. In a closed system, how many independent variables are there among n, T, V and P for a gas?
    • Note: an independent variable can be of any arbitrary values. Hint . . .one

      Skill:
      The ideal gas equation shows the interdependence of the variables. Only one of them can be varied independently.

    • What is the molar volume of an ideal gas at 2 atm and 1000 K?
    • Hint . . .41.0

      Skill:
      Evaluate molar volume at any condition.

    • A certain amount of a gas is enclosed in a container of fixed volume. If you let heat (energy) flow into it, what will increase?
      (In a multiple choice, you may have volume, pressure, temperature, and any combination of these to choose from.)
    • Hint . . .Both pressure and temperature will increase.

      Skill:
      Explain a closed system and apply ideal gas law.

    • For a certain amount (n = constant) of gas in a closed system, how does volume V vary with the temperature? In the following, k is a constant depending on n and P.
      a. V = k T
      b. V = k / T
      c. T V = k
      d. V = k T2
      e. V = k
    • Hint . . .a

      Skill:
      Explain Charles law.

    • Boyles law is P V = constant. A sketch of P vs V on graph paper is similar to a sketch of the equation x y = 5. What curve(s) does this equation represent? a. a parabola
      b. an ellipse
      c. a hyperbola
      d. a pair of hyperbola
      e. a straight line
      f. a surface
      Hint . . .d

      Skill:
      Apply the skills acquired in Math courses to chemical problem solving.

    • For a certain amount of gas in a closed system, which one of the following equation is valid? Subscripts 1 and 2 refer to specific conditions 1 and 2 respectively. a. P1 V1 T1 = P2 V2 T2
      b. P1 V1 T2 = P2 V2 T1
      c. P1 V2 T1 = P2 V1 T2
      d. P2 V1 T1 = P1 V2 T2
      e. P1 V2 / T1 = P2 V1 / T2
    • Hint . . .b

      Skill:
      Rearrange a mathematical equation.

    • The gas constant R is 8.314 J / mol·K. Convert the numerical value of R so that its units are cal / (mol·K). A unit conversion table will tell you that 1 cal = 4.184 J. Make sure you know where to find it. During the exam, the conversion factor is given, but you should know how to use it.
    • Hint . . .1.987 cal/(mol K).

      Skill:
      Use conversion factors, for example:

              1 cal
      8.314 J ------- = ? cal
              4.184 J 
      

    • At standard temperature and pressure, how many moles of H2 are contained in a 1.0 L container?
    • Hint . . .0.045 mol/L

      Discussion:
      There are many methods for calculating this value.

    • At standard temperature and pressure, how many grams of CO2 is contained in a 3.0 L container? Molar mass of CO2 = 44.
    • Hint . . .5.89 g in 3 L

      One method:
      It contains n = 1 atm * 3 L / (0.08205 L atm / (mol·K) * 273 K)

    • What is the pressure if 1 mole of N2 occupy 1 L of volume at 1000 K?
    • Hint . . .82.1 atm

      Discussion:
      Depending on the numerical value and units of R you use, you will get the pressure in various units.
      At 1000 K, some of the N2 molecules may dissociate. If that is true, the pressure will be higher!

    • What is the temperature if 1 mole of N2 occupy 100 L of volume has a pressure of 20 Pa (1 Pa = 1 Nm-2 )?
    • Hint . . .240 K

      Discussion:
      At T = 240 K, ideal gas law may not apply to CO2, because this gas liquifies at rather high temperature. The ideal gas law is still good for N2, H2, O2 etc, because these gases liquify at much lower temperature.

    December 21

    X-ray photoelectron spectroscopy

    X-ray photoelectron spectroscopy
    Basic components of a monochromatic XPS system.
    Enlarge
    Basic components of a monochromatic XPS system.

    X-ray Photoelectron Spectroscopy (XPS) is a quantitative spectroscopic technique that measures the empirical formula, chemical state and electronic state of the elements that exist within a material. XPS spectra are obtained by irradiating a material with a beam of X-rays while simultaneously measuring the kinetic energy (KE) and number of electrons that escape from the top 1 to 10 nm of the material being analyzed. XPS requires ultra-high vacuum (UHV) conditions.

    XPS is a surface chemical analysis technique that can be used to analyze the chemistry of the surface of a material in its "as received" state, or after some treatment such as: fracturing, cutting or scraping in air or UHV to expose the bulk chemistry, ion beam etching to clean off some of the surface contamination, exposure to heat to study the changes due to heating, exposure to reactive gases or solutions, exposure to ion beam implant, exposure to UV light, for example.

    • XPS is also known as ESCA, an abbreviation for Electron Spectroscopy for Chemical Analysis.
    • Detection limits for most of the elements are in the parts-per-thousand (PPTh) range.
    • XPS is routinely used to analyze inorganic compounds, metal alloys, semiconductors, polymers, pure elements, catalysts, glasses, ceramics, paints, papers, inks, woods, plant parts, make-up, teeth, bones, human implants, bio-materials, viscous oils, glues, ion modified materials and many others.
    Wide Scan Survey Spectrum for all elements.
    Enlarge
    Wide Scan Survey Spectrum for all elements.
    High Resolution Spectrum for Si(2p) signal.
    Enlarge
    High Resolution Spectrum for Si(2p) signal.

    XPS is used to measure:

    • elemental composition of the surface (1–10 nm usually)
    • empirical formula of pure materials
    • elements that contaminate a surface
    • chemical or electronic state of each element in the surface
    • uniformity of elemental composition across the top the surface (aka, line profiling or mapping)
    • uniformity of elemental composition as a function of ion beam etching (aka, depth profiling)

    XPS can be performed using either a commercially built XPS system, a privately built XPS system or a Synchrotron-based light source combined with a custom designed electron analyzer. Commercial XPS instruments in the year 2005 used either a highly focused 20 to 200 micrometer beam of monochromatic aluminum K-alpha X-rays or a broad 10-30 mm beam of non-monochromatic (achromatic or polychromatic) magnesium X-rays. A few, special design XPS instruments can analyze volatile liquids or gases, materials at low or high temperatures or materials at roughly 1 torr vacuum, but there are relatively few of these types of XPS systems.

    Because the energy of a particular X-ray wavelength equals a known quantity, we can determine the electron binding energy (BE) of each of the emitted electrons by using an equation that is based on the work of Ernest Rutherford (1914):

    Ebinding = Ephoton - Ekinetic - Φ

    where Ebinding is the energy of the electron emitted from one electron configuration within the atom, Ephoton is the energy of the X-ray photons being used, Ekinetic is the kinetic energy of the emitted electron as measured by the instrument and Φ is the work function of the spectrometer.

    History of XPS

    In 1887, Heinrich Rudolf Hertz discovered the photoelectric effect. Twenty years later, in 1907, P.D. Innes experimented with a Rontgen tube, Helmholtz coils, a magnetic field hemisphere (electron energy analyzer) and photographic plates to record broad bands of emitted electrons as a function of velocity, in effect recording the first XPS spectrum. Other researchers, Moseley, Rawlinson and Robinson, independently performed various experiments trying to sort out the details in the broad bands. Due to the wars, research on XPS came to a halt. After WWII, Kai Siegbahn and his group in Sweden developed several significant improvements in the equipment and in 1954 recorded the first high energy resolution XPS spectrum of cleaved sodium chloride (NaCl) revealing the potential of XPS. A few years later in 1967, Siegbahn published a comprehensive study on XPS bringing instant recognition of the utility of XPS. In cooperation with Siegbahn, Hewlett-Packard in the USA produced the first commercial monochromatic XPS instrument in 1969. Siegbahn received the Nobel Prize in 1981 to acknowledge his extensive efforts to develop XPS into a useful analytical tool.

    Physics of XPS

    Rough diagram showing physics of photon induced electron emission (photoemission) in XPS.
    Enlarge
    Rough diagram showing physics of photon induced electron emission (photoemission) in XPS.

    A typical XPS spectrum is a plot of the number of electrons detected (Y-axis, abscissa) versus the binding energy of the electrons detected (X-axis, ordinate). Each element produces a characteristic set of XPS peaks at characteristic binding energy values that directly identify each element that exist in or on the surface of the material being analyzed. These characteristic peaks correspond to the electron configuration of the electrons within the atoms, e.g., 1s, 2s, 2p, 3s, etc. The number of detected electrons in each of the characteristic peaks is directly related to the amount of element within the area (volume) irradiated. To generate atomic percentage values, each raw XPS signal must be corrected by dividing its signal intensity (number of electrons detected) by a "relative sensitivity factor" (RSF) and normalized over all of the elements detected.

    To count the number of electrons at each KE value, with the minimum of error, XPS must be performed under ultra-high vacuum (UHV) conditions because electron counting detectors in XPS instruments are typically one meter away from the material irradiated with X-rays.

    It is important to note that XPS detects only those electrons that have actually escaped into the vacuum of the instrument. The photo-emitted electrons that have escaped into the vacuum of the instrument are those that originated from within the top 10 to 12 nm of the material. All of the deeper photo-emitted electrons, which were generated as the X-rays penetrated 1–5 micrometers of the material, are either recaptured or trapped in various excited states within the material. For most applications, it is, in effect, a non-destructive technique that measures the surface chemistry of any material.

    Components of an XPS system

    The main components of an XPS system include: a source of X-rays, an ultra-high vacuum (UHV) stainless steel chamber with UHV pumps, an electron collection lens, an electron energy analyzer, mu-metal magnetic field shielding, an electron detector system, a moderate vacuum sample introduction chamber, sample mounts, a sample stage and a set of stage manipulators.

    Monochromatic aluminum K-alpha X-rays are normally produced by diffracting and focusing a beam of non-monochromatic X-rays off of a thin disc of natural, crystalline quartz with a <1010> lattice. The resulting wavelength is 8.3386 angstroms (0.83386 nm) which corresponds to a photon energy of 1486.7 eV. The energy width of the monochromated X-rays is 0.16 eV, but the common electron energy analyzer (spectrometer) produces an ultimate energy resolution on the order of 0.25 eV which, in effect, is the ultimate energy resolution of most commercial systems. When working under everyday conditions, the typical high energy resolution (FWHM) is usually 0.4-0.6 eV.

    Non-monochromatic magnesium X-rays have a wavelength of 9.89 angstroms (0.989 nm) which corresponds to a photon energy of 1253 eV. The energy width of the non-monochromated X-ray is roughly 0.70 eV, which, in effect is the ultimate energy resolution of a system using non-monochromatic X-rays. Non-monochromatic X-ray sources do not difract out the other nearby X-ray energies and also allow the full range of high energy Bremsstrahlung X-rays (1–12 keV) to reach the surface. The typical ultimate high energy resolution (FWHM) for this source is 0.9–1.0 eV, which includes with the spectrometer-induced broadening, pass-energy settings and the peak-width of the non-monochromatic magnesium X-ray source.

    Uses and capabilities

    Fundamental XPS Data from pure elements, oxides and compounds.
    Enlarge
    Fundamental XPS Data from pure elements, oxides and compounds.

    XPS is routinely used to determine:

    • what elements and the quantity of those elements that are present within ~10 nm of the sample surface
    • what contamination, if any, exists in the surface or the bulk of the sample
    • empirical formula of a material that is free of excessive surface contamination
    • the chemical state identification of one or more of the elements in the sample
    • the binding energy (BE) of one or more electronic states
    • the thickness of one or more thin layers (1–8 nm) of different materials within the top 10 nm of the surface
    • the density of electronic states

    Capabilities of advanced systems

    • measure uniformity of elemental composition across the top the surface (aka, line profiling or mapping)
    • measure uniformity of elemental composition as a function of depth by ion beam etching (aka, depth profiling)
    • measure uniformity of elemental composition as a function of depth by tilting the sample (aka, angle resolved XPS)

    Industries that use XPS

    Adhesion, Agriculture, Automotive, Battery, Beverage, Biotech, Canning, Catalyst, Ceramic, Chemical, Computer, Cosmetic, Electronics, Environmental, Fabrics, Food, Fuel cells, Geology, Glass, Laser, Lighting, Lubrication, Magnetic memory, Mineralogy, Mining, Nuclear, Packaging, Paper and wood, Plating, Polymer and plastic, Printing, Recording, Semiconductor, Steel, Textiles, Thin-film coating, Welding

    Routine limits of XPS

    Quantitative accuracy:

    • Quantitative accuracy depends on several parameters such as: S/N, peak intensity, accuracy of relative sensitivity factors, correction for electron transmission function, surface volume homogenity, correction for energy dependency of electron mean free path, and degree of sample degradation due to analysis.
    • Under optimum conditions, the quantitative accuracy of the atom % values calculated from the Major XPS Peaks is 90-95% of the atom % values of each major peak. If a high level quality control protocol is used, the accuracy can be further improved.
    • Under routine work conditions, where the surface is a mixture of contamination and expected material, the accuracy ranges from 80-90% of the value reported in atom % values.
    • The quantitative accuracy for the weaker XPS signals, that have peak intensities 10-20% of the strongest signal, are 60-80% of the true value.

    Analysis times

    • 1–10 minutes for a survey scan that measures the amount of all elements, 1–10 minutes for high energy resolution scans that reveal chemical state differences, 1–4 hours for a depth profile that measures 4–5 elements as a function of etched depth (usual final depth is 1,000 nm)

    Detection limits

    • 0.1–1.0 atom % (1 atom% = 1 part per thousand (PPTh) = 1,000 PPM). Ultimate detection limit for most elements is approximately 100 ppm, which requires 8–16 hours.)

    Analysis area limits

    • Analysis area depends on instrument design. The minimum analysis area ranges from 10 to 200 micrometres. Largest size for a monochromatic beam of X-rays is 1–5 mm. Non-monochromatic beams are 10–50 mm in diameter.

    Sample size limits

    • Older instruments accept samples: 1x1 to 3x3 cm. Very recent systems can accept full 300 mm wafers and samples that are 30x30 cm.

    Degradation during analysis

    • Depends on the sensitivity of the material to the wavelength of X-rays used, the total dose of the X-rays, the temperature of the surface and the level of the vacuum. Metals, alloys, ceramics and most glasses are not measurably degraded by either non-monochromatic or monochromatic X-rays. Some, but not all, polymers, catalysts, certain highly oxygenated compounds, various inorganic compounds and fine organics are degraded by either monochromatic or non-monochromatic X-ray sources.
    • Non-monochromatic X-ray sources produce a significant amount of high energy Bremsstrahlung X-rays (1–15 keV of energy) which directly degrade the surface chemistry of various materials. Non-monochromatic X-ray sources also produce a significant amount of heat (100 to 200 °C) because the anode that produces the X-rays is typically only 1to 5 cm away from the sample. This level of heat, when combined with the Bremsstrahlung X-rays, acts synergistically to increase the amount and rate of degradation for certain materials. Monochromatic X-ray sources, because they are far away (50–100 cm) from the sample, do not produce any heat effects. Monochromatic X-ray sources are monochromatic because the quartz monochromator system diffracted the Bremsstrahlung X-rays out of the X-ray beam which means the sample only sees one X-ray energy, for example: 1.486 keV if aluminum K-alpha X-rays are used.
    • Because the vacuum removes various gases (eg O2, CO) and liquids (eg water, alcohol, solvents) that were initially trapped within or on the surface of the sample, the chemistry and morphology of the surface will continue to change until the surface achieves a steady state. This type of degradation is sometimes difficult to detect.

    Materials routinely analyzed by XPS

    Inorganic compounds, metal alloys, semiconductors, polymers, pure elements, catalysts, glasses, ceramics, paints, papers, inks, woods, plant parts, make-up, teeth, bones, human implants, bio-materials, viscous oils, glues, ion modified materials

    Organic chemicals are not routinely analyzed by XPS because they are readily degraded by the either the energy of the X-rays or the heat from non-monochromatic X-ray sources.

    Related methods

    • UPS, Ultra-violet photoelectron spectroscopy (aka PES)
    • PES, Photo-electron spectroscopy (aka UPS)
    • ZEKE, Zero Electron Kinetic Energy spectroscopy
    • AES, Auger electron spectroscopy (AES)

    Literature references

    • Handbooks of Monochromatic XPS Spectra, Volumes 1-5, B. Vincent Crist, published by XPS International, LLC, 2005, Mountain View, CA, USA
    • Surface Analysis by Auger and X-ray Photoelectron Spectroscopy, ed. John T. Grant and David Briggs, published by IM Publications, 2003, West Chester, UK
    • Practical Surface Analysis by Auger and X-ray Photoelectron Spectroscopy, ed. Martin P. Seah and David Briggs, published by Wiley & Sons, 1983, Chichester, UK ISBN 0-471-26279-X
    • Practical Surface Analysis by Auger and X-ray Photoelectron Spectroscopy, 2nd edition, ed. Martin P. Seah and David Briggs, published by Wiley & Sons, 1992, Chichester, UK
    • Surface Chemical Analysis -- Vocabulary, ISO 18115 : 2001, International Standards Organization, TC/201, Switzerland, [1]
    • Handbook of X-ray Photoelectron Spectroscopy, C.D.Wagner, W.M.Riggs, L.E.Davis, J.F.Moulder, and G.E.Mullenberg, published by Perkin-Elmer Corp., 1979, Eden Prairie, Minn, USA
    • Handbook of X-ray Photoelectron Spectroscopy, J.F.Moulder, W.F.Stickle, P.E.Sobol, and K.D.Bomben, published by Perkin-Elmer Corp., 1992, Eden Prairie, Minn, USA

    See also

    External links

    • The Science of Spectroscopy - supported by NASA. Spectroscopy education wiki and films - introduction to light, its uses in NASA, space science, astronomy, medicine & health, environmental research, and consumer products.

    Instrument suppliers

    • JEOL, Japan [2]
    • Omicron, Germany [3]
    • Shimadzu-Kratos, USA [4]
    • Specs, Germany [5]
    • Thermo Electron, USA [6]
    • Ulvac-Phi, Japan [7]

    Reference data sources

    • XPS International, USA [8]
    • NIST, US Government, USA [9]
    • LaSurface, France [10]

    Service labs - companies

    • Materials Analysis Services, USA [11]
    • Evans Analytical Group, USA [12]
    • Ulvac-PHI, USA [13]
    • RBD Enterprises, USA [14]


    This entry is from Wikipedia, the leading user-contributed encyclopedia. It may not have been reviewed by professional editors (see full disclaimer)

    宇宙学

    基础帖之——宇宙学
    来自维基百科,自由的百科全书

    宇宙学天体物理学的分支,它是研究宇宙大尺度结构和宇宙形成及演化等基本问题的学科。宇宙学的研究对象是天体运动和它的第一起因,在人类历史的很长一段时期曾是形而上学的一部份。作为科学,宇宙学起源于哥白尼原则牛顿力学,它们指出天体和地球上的物体遵守同样的物理原理并解释了天体的运动。现在这一分支被称为天体力学。一般认为,物理宇宙学起源于二十世纪的爱因斯坦广义相对论和对极远天体的天文观测。

    二十世纪的科技进步使对宇宙起源的猜测成为可能。它也帮助建立了被绝大多数宇宙学家公认作理论和观测基础的大爆炸理论。(虽然职业宇宙学家认为大爆炸理论给观测以最好的解释,一些人至今仍在鼓吹另类宇宙学如等离子体宇宙学和稳恒态宇宙学。)大致来说,物理宇宙学处理的对象是宇宙中最大的物体(如星系,星系团,超团),最早形成的物体(如类星体)和几乎均匀的最早期宇宙(大爆炸,宇宙暴涨,微波背景辐射)。

    宇宙学是比较特别的学科。它从粒子物理实验,粒子物理唯象学,甚至弦理论中汲取了许多结果。它的其他来源包括天体物理,广义相对论和等离子体物理的研究。

    发展历史

    现代宇宙学是沿着观测和理论的辐辙发展起来的。1915年爱因斯坦提出了广义相对论。因为那时的物理学家有一种偏见,认为宇宙是静态的、无始无终的,爱因斯坦在他的方程中加入了一个宇宙学常数项。这个物质加宇宙学常数的稳恒态爱因斯坦宇宙模型是不稳定的,它最终总会膨胀或收缩。广义相对论的宇宙学解是由弗里德曼发现的,现在被称为弗里德曼-罗伯森-沃克宇宙。它描写的是膨胀或收缩的宇宙。

    1910年斯里菲和威兹用多普勒现象来解释观测到的涡状星云的红移。这意味着这些星云正离我们远去。虽然人们可以测量天体的视角大小,但是却很难知道它们的实际大小和亮度,这使得测量天体的距离异常得困难。斯里菲和威兹没有意识到这些星云其实是河外星系,也没有意识这个发现对宇宙学的意义。1927年,一位比利时的天主教神甫勒玛泰独立地发现了弗里德曼-罗伯森-沃克解并在涡状星云的观测基础上提出宇宙起源于原初原子爆炸的假说。1929年哈勃为这个假说提供了观测依据。他证明了涡状星云是一些星系并通过观测仙王变星来测量了它们的距离。他同时还发现了星系红移和亮度之间的关系,认为这一关系的起源是因为在所有方向星系离我们远去的速度正比于它们的距离。这个关系被称为哈勃定律,它其实只在最近才被确认,哈勃的数据误差很大。

    给定宇宙学原理,哈勃定律意味着宇宙是在膨胀的。有两种可能可以解释这个现象,其一是由伽莫夫提出的大爆炸理论,另一种理论是霍义耳的稳恒态模型。在此模型中,星系互相远离时不停地有新物质产生,在任何时间宇宙大致是一样的。

    许多年来这两者互有支撑依据。但是从1965年发现微波背景辐射以来,观测结果越来越倾向于支持前一种理论。1960年代以前,许多宇宙学家认为弗里德曼宇宙开始时的无限致密奇点是数学上的理想化,宇宙也应在到达此热致密状态之前从收缩转换到从新膨胀。这就是托尔曼的振荡宇宙模型。但是霍金彭罗斯证明了这个模型是不可能工作的,他们指出了奇点是广义相对论的一个特征。从此以来大多数宇宙学家开始接受宇宙在有限时间以前开始演化的大爆炸理论。

    研究领域

    以下所列的是宇宙学研究的一些最活跃的领域,大致按时间顺序排列。这个单子不包括大爆炸宇宙学。它可以参见宇宙时间表

    极早期宇宙

    虽然大爆炸理论看起来可以解释从10 &#8722; 33秒钟开始的早期热宇宙,它却面临着许多困难。其中之一是现今的粒子物理理论不能为宇宙的平坦性、均匀型和各向齐性(参阅宇宙学原理)提供一个令人满意的答案。另外,大统一模型预言了宇宙中有磁单极,它们也没有被观察到。宇宙暴涨解决了这些问题。它的物理模型虽然很简单,但是却没有被粒子物理所证实,其主要困难在于如何调和它和量子场论的矛盾。一些宇宙学家认为弦理论膜宇宙学能为解决宇宙学原理提供另一方案。

    宇宙学的另一主要问题是解释为什么粒子要多于反粒子。X射线观测表明宇宙并不是由物质和反物质的区域组成的。它的主要组成是物质。这个问题称为重子不对称性,解释这种现象的理论被称为重子产生。重子产生理论是由萨哈罗夫1967年提出的,它的必要条件中包括物质和反物质间的电荷-宇称对称性的破缺。粒子加速器只观测到很小的电荷-宇称对称破坏,不能解释宇宙的重子不对称性。宇宙学家和粒子物理学家希望能发现电荷-宇称破坏的其它来源。

    重子产生和宇宙暴涨都与粒子物理有密切的联系。这些问题的解决答案可能会产生于高能理论和实验而不是于天文观察中。

    大爆炸核合成过程

    大爆炸核合成是关于元素在早期宇宙形成的理论。当宇宙演化到大约三分钟时,它已经足够冷却,这时核聚变及核合成过程就终止了。因为大爆炸核合成过程持续的时间极为短暂,从质子和中子出发,它的主要合成成品是轻元素如氘、氦-4和锂。其它元素则极为微量。(重元素主要是由星体如超新星中的核反应而形成的。)虽然在1948年伽莫夫阿尔菲赫尔曼就已经提出了这个理论的基本观点,由于在此理论中轻元素的丰度与早期宇宙的物理性质关系密切,它至今仍然是检验大爆炸时期物理理论的极灵敏的探针。比如,它可以用来检验等效原理暗物质中微子物理。

    宇宙微波背景辐射

    宇宙微波背景辐射是指退耦过程(即大爆炸所产生的光辐射停止与带电离子的汤普生散射原子第一次形成这一过程)所残余的辐射。这种辐射是由彭齐亚斯和威尔逊在1965年发现的。它具有几乎完美的2.7K黑体辐射谱,只在十万分之一内偏离各向同性。宇宙学家们可以用描写早期宇宙细微起伏演化的宇宙学微扰理论来精确地计算辐射的角度功率谱。最近的卫星(COBE和 WMAP)和地面及气球(DASI,CBI和Boomerang)实验也测量了此功率谱。这些工作的目的是为了更精确地测量Λ-冷暗物质模型的参数,同时也为了检验大爆炸模型和新物理模型的预言。例如,最近WMAP的测量就为中微子的质量提供了限制。

    更新的实验的目的则是测量微波背景谱的极化。它将为微扰理论提供更多的证据,也将为宇宙暴涨和所谓的次级非各向同性(如由背景辐射和星系和星系团相互作用引起的散亚耶夫-泽尔多维奇效应和萨克斯-沃尔夫效应)提供信息。

    大尺度结构的形成和演化

    理解最早和最大结构(如类星体,星系,星系团和超团)的形成和演化是宇宙学的核心课题之一。宇宙学家们研究的是一种由下至上有层次的结构形成模型。在此模型中,小物体先形成,而大的物体如超团还在形成过程中。研究宇宙中结构最直接了当的方法是普查可见的星系,从而构造一个星系的立体图像并测量物质功率谱。这就是斯隆数码巡天和2dF星系红移巡天的研究方案。

    理解结构形成的一个重要工具是模拟。宇宙学家们用它来研究宇宙中物质的引力堆积和线状结构,超团和空穴的形成。因为宇宙中冷暗物质要比可见的重子物质多许多,所以大多数模拟只计入它们。这种处理对理解最大尺度的宇宙是足够了。更先进的模拟已经开始计入重子的效应,它们也开始研究星系的形成。宇宙学家们检查这些模拟是否与星系普查的结果一致。如果不一致,则研究偏差的原因。

    宇宙学家还用其它互补的方法来测量宇宙遥远处的物质分布和再电离过程。这些方法包括:

    莱曼阿尔法谱线森林。通过测量气体对遥远类星体所发射光的吸收来测量早期宇宙中中性氢原子的分布。

    中性氢原子的21厘米吸收线也提供了灵敏的测试。

    由于暗物质的引力透镜效应而引起的对遥远物象的扭曲,即所谓的弱透镜效应。

    这些方法都将帮助宇宙学家解决第一代天体如何形成这一问题。

     暗物质

    大爆炸核形成、宇宙微波背景辐射和结构形成的研究证据表明了宇宙质量的25%是由非重子的暗物质组成的,而可见的重子物质只占宇宙质量的4%。作为星系周围晕中的一种冷的、不辐射的尘埃,暗物质的引力效应已经被了解得很透彻了,但是它的粒子物理性质还是个谜,人们从没有在实验室中观察到它们。暗物质的可能候选包括稳定的超对称粒子、弱作用重粒子(WIMP)轴子重致密晕天体(MACHO),它甚至还可能是在极小加速度下引力的修正(修正的牛顿动力学,或MOND)或膜宇宙学的一种效应。

    星系中心的物理(如活动星系核,超重黑洞)可能会给暗物质的性质提供线索。

     暗能量

    如果宇宙是平坦的,那么必须有一种东西组成71%的宇宙密度(扣除25%的暗物质和4%的重子物质)。它被称为暗能量。这种东西不能干涉大爆炸核合成和宇宙微波背景辐射,所以它不能象重子和暗物质那样在星系周围晕环中结团。因为宇宙是平坦的,所以我们知道它的总质量。通过观测我们也知道宇宙中结团物质的质量比总质量远远要小,这就为暗物质的存在提供了很强的证据。1999年发现的宇宙加速膨胀(类似宇宙早期的暴涨)为暗物质提供了更强的证据。

    除了暗物质的密度和结团性质外,我们对它一无所知。量子场论预言了一种类似暗物质但比它大120个数量级的宇宙常数温伯格和一些弦理论家由此提出人择原理。他们认为宇宙常数如此小的原因是因为人类不能在其他大宇宙常数的世界中生存。许多人觉得这种解释很牵强。暗能量其他可能的解释包括精质(quintessence)和在大尺度下引力的修正。这些模型的核心是暗能量的状态方程,不同的理论有不同的状态方程。暗能量的本质是宇宙学中最具挑战性的问题之一。

    如果我们对暗能量有更好的理解,我们可能会解开宇宙最终结局这一谜题。在现在这个宇宙时期,由暗能量引起的宇宙加速膨胀阻碍了比超团更大结构的形成。我们还不清楚这种加速膨胀会不会永久持续下去。或许它会加快,甚至它也可能会变成减速膨胀。
    December 20

    轻松架设个人服务器 - -

    轻松架设个人服务器 - -




    用自己的机子架设服务器放动网的论坛,要怎么做?总而言之,大家水平不同,问的问题也不一样,但这是关系到设置是否成功和动网论坛是否能正常使用,于是我在网上去帮大家找了这篇文章,讲得要多详细有多详细了,如果你也想架设一部属于自己的服务器,请好好看看这篇吧


    看到别人精美的个人主页,你一定会有所心动,而如今免费资源却是越来越少,往往你花大量时间去寻找免费主页空间时,最后却因它们的不稳定而给自己带来一些遗憾。此外,在信息社会中,我们经常需要转移、暂存一些文档和资料,或与别人实现文件共享,FTP服务会经常作为我们的最佳信息传输方式。但在很多时候,当我们来回穿梭于那些免费的FTP服务器时,却因为苦于没有匿名帐号或人数过多而不能正常登录。其实,我们完全可以避开这些尴尬,全力打造一个属于自己的个人服务器,从此不再搭便车,开始体会拥有的快感!下面随我一起开始个人服务器的网络架设之旅。
    WWW服务器的架设

    我们几乎每天都会浏览形形色色的网站来获取各种各样的信息,WWW服务器就是提供此类服务的,目前有很多信息提供商提供WWW服务器架设的付费服务。其实,我们完全可以自己打造WWW的个人服务器,在网上发布一些个人信息,并且体会做管理员的乐趣。WWW服务器的架设有很多种方式,下面介绍一些主流的实现方法:

    1.通过微软提供的IIS

    目前很大一部分的WWW服务器都架设在微软公司的IIS之上。它使用的环境为WinNT/2000/XP+Internet Information Service(IIS),相信很多用户现在使用的都是Win2000或WinXP系统,在Win2000 Professional和WinXP系统中,默认的情况下,它们在系统初始安装时都不会安装IIS(目前版本为IIS5.0),因此得将这些组件添加到系统中去。

    第一步:IIS的安装

    A.在控制面板中选择“添加/删除程序”,在出现的对话框中选择“添加/删除Windows组件”(如图1)。

    B.在出现的复选框中选择安装Internet信息服务(IIS)(如图2),这一组件约需19MB的空间。

    C.点击“下一步”,并将Win2000安装光盘放入光驱,安装程序即可将程序文件复制到硬盘中,点击“结束”即可完成。

    第二步:IIS中Web服务器的基本配置

    IIS中Web服务器的基本配置主要包括如下几部分:

    A.打开IIS服务器的配置窗口,选择“开始”→“程序”→“管理工具”→“Internet服务管理器”,或者“选择”→“控制面板”→“管理工具”→“Internet服务管理器”也可,打开的窗口如图3。

    B.在打开的窗口中鼠标右击“默认Web站点”,选择“属性”菜单。

    C.在出现的“默认Web站点属性”窗口中,选择“主目录”标签,用以设置Web内容在硬盘中的位置,默认目录为“C:\Inetpub\Wwwroot”,你可根据需要自己设置(如图4)。

    D.在属性窗口处选择“文档”标签,设置自己默认的首页网页名称,例如“Myfirstweb.htm”,将其添加并移动到列表的最顶端(如图5)。

    E.确认默认的Web站点是否已经启动,如果没有可以鼠标右键点击“默认Web站点”,选择“启动”,在打开的IE地址栏中键入本机的IP地址,即可看到自己指定的主页已经开始在Internet上发布了。

    这里只是介绍IIS最基本的设置选项,大家还可以按照需要去具体设置上面提到的“默认Web站点属性”,通过它来配置IIS的安全和其他一些参数。

    IIS虽然好用,但默认安装的情况下,它也有很多的安全漏洞,包括著名的Unicode漏洞和CGI漏洞,因此在IIS安装完成之后,建议继续在微软公司主页上下载安装它们提供的安全漏洞补丁SP1和SP2。此外,建议将磁盘的文件系统转换成NTFS格式,安装系统的分区可在系统安装候转换,也可在安装完系统以后用PQMagic等工具进行转换。

    2.利用微软的PWS

    PWS的全称是“Personal Web Server”,字面意思就是个人网页服务器,由微软公司提供,它主要适合于创建小型个人站点,它的配置和使用比较简单,但功能却很强大。跟IIS的区别是,PWS可以安装在Win9X/Me/NT/2000/XP系统中,因此对Win9X/Me系统来说尤其可贵。

    第一步:PWS的安装

    对Win9X/Me系统来说,在光驱里放入Win98安装光盘,进入光盘的Add-ons\Pws\目录,双击Setup.exe命令即可开始安装PWS,安装界面如图6所示。我们如果需要一些例如ASP等高级功能,还可选择自定义的安装模式,否则直接选择典型安装。组件安装完成之后,会出现如图7所示的选项来设置WWW服务目录,我们可以视实际情况来设定,建议以缺省目录来安装。最后选择“完成”并根据提示重新启动计算机后,就可在右下角任务栏看见PWS的图标(如图8)。

    这时打开一个IE窗口,在地址栏中输入“http://localhost”、“http://127.0.0.1”或者“http://你的IP地址”,就可看到PWS的默认页面,表明PWS已经成功运行了。

    对于Win2000/XP来说,PWS是作为IIS的一个组件安装的。如果你是Win9X/Me系统,没有安装PWS的光盘也不要紧,可以去http://img.cn99.com/cn99new/series/dyndns/pws.zip下载PWS的安装软件,安装步骤跟上面差不多。

    第二步:PWS的配置

    双击屏幕右下角的PWS图标,或在菜单中选择相应的程序组来启动“个人Web管理器”(如图9)。由管理器界面(图9是Win2000中IIS的PWS,因此只有3个选项)可以看出它包括5个部分,可分别管理不同的功能,利用PWS架设自己的WWW服务器一般主要有如下几个步骤。

    A.启动PWS。在PWS的主屏选项处,它又细分为“发布”和“监视”两部分。首先必须通过点击“启动”按钮来打开PWS的服务。在这里,你还可以通过“监视”中的内容查看Web站点的一些访问统计信息。

    B.设定虚拟目录。假定你的网页存放在“E:\Ww\Homepages\Homepage”下,首页文件名为“Myfirstweb.htm”。先在图10中选定虚拟目录,单击“添加”按钮,在出现的“添加目录”对话框中(如图11),指定网页所在的驱动器号和目录,这里是“E:\Ww\Homepages\Homepage”,并且为自己的这个虚拟目录设置一个别名,别名可以随便设置,是朋友访问你网站时的目录名称。安全建议:设置目录的访问权限为“读取”和“脚本”,为安全起见,不要选取“执行”权限。

    默认情况下,PWS服务器的根目录是“C:\Inetpub\Wwwroot”。我们如果不想具体来设置虚拟目录,也可将你存放的网页的所有文件拷贝到该目录中,例如:将“E:\Ww\Homepages\Homepage”中所有的文件拷贝到“C:\Inetpub\Wwwroot”中即可。

    C.设置默认文档。接下来,为你的虚拟目录设置一个能在默认情况下自动识别的网页文档。该文档的作用是,当进入本站点时,如没有指定要访问的文档,则服务器自动提供一个默认文档让其访问。在图10中,选中“启用默认文档”复选框,并在“默认文档”框中,输入自己的首页文档名“Myfirstweb.htm”。安全建议:和上面一样,出于安全的原因,不要选中“允许浏览目录”复选框,以免别人看到整个目录里的所有文件。

    D.创建访问记录。如果我们要监控访问我们页面的游客,还可以在高级中(图11)选择“保存Web站点活动日志”,系统就会自动帮我们记录访问该Web站点的数据,这些数据将记录访问者的IP地址、访问时间和访问内容。服务器将在“C:\Windows\System\Logfiles”中的文件夹中建立一个名为“Ncyymm.log”的文件(yy为年份,mm为月份)。该文件可用文本编辑器查看,也可在DOS窗口中用“Type”命令查看。

    经过这样简单的设置,打开IE并输入你自己的IP地址即可看到你发布的主页,无论是否上网都可调试自己的站点。当然也可以使用一个特殊的IP来检验安装的正确性和回送地址,即http://127.0.0.1或者http://localhost

    此外,PWS还有其他几个选项用来增强它的功能,主要包括如下两个标签。

    A.发布。这部分主要是提供定制个人主页的发布及编辑文件发布列表的功能,

    可以将文件发布出去以供别人浏览和下载。这个过程实际上也是结合了PWS的ASP功能。此外,这里还可以在定制个人发布主页时创建来宾簿和留言簿,例如,你想将“D:\Download\Tt.zip”发布出去,首先选择“发布”,点击下一步按钮,进入“发布向导”,在“发布向导”中填入相应的项目即可(如图12)。单击“添加”按钮,并点击“下一步”,PWS即提示你“已添加下列文件:Tt.zip”。继续点击“下一步”,默认是选中“将文件加入到发布的列表”,单击“下一步”,即可将要发布的“Tt.zip”文件发布出去了。打开IE窗口并访问自己的Web站点,就可看到网页上多了个发布文档的链接,其中就含有刚才配置好的发布出去的文件。

    B.Web站点。点击“Web站点”即可出现“主页向导”界面,PWS提供了主页、来宾薄和留言本3种页面的模板。按向导的提示选择好选项,就可出现动态ASP设置页面,可在这里编辑主页、查看来宾簿、打开留言簿,以得到一些反馈信息。

    3.采用Apache

    Apache是全世界使用范围最广的一款Web服务器设置软件,超过50%的网站都在使用它,它主要以高效、稳定、安全、免费(最重要的一点)而著称。目前它的最新版本为1.3.26,文件大小只有2.07MB,大家可以去它的主页:http://www.apache.org/dist/httpd/binaries/win32下载。下载时记住选择For Win32的无原码版本(Apache_1.3.26-win32-no_src.msi)。最新版的Apache for win32开始使用MSI的形式发布,从而使Windows环境下安装Apache变得非常简单,它是全英文界面,但使用起来却很方便。

    第一步:Apache的安装

    A.双击Apache的安装文件,和普通Windows程序安装一样,一路点”Next”就可以。

    B.在程序的安装过程它还要求输入你的Network Domain(网络域名:如XXX.com);Server Domain(服务器域名www.XXX.com)和网站管理员的E-mail,有就按实填写,个人用户若没有可按格式随便填一下(如图13)。

    C.到了选择安装路径,按照个人习惯选择。

    D.一路“Next”直至“Finish”,安装即可完成。

    这时,你的Apache已经启动了,你可以在IE地址栏里输入:“http://localhost”或“http://127.0.0.1”看到默认的Apache首页(如图14)。此外,在“管理工具”的“服务”项中,也可找到Apache服务的身影,以后Apache就可以作为一项服务,随着机器的启动而自动运行。

    第二步:Apache的配置

    Apache的核心配置文件是“Httpd.conf”,它在电脑中的位置为Apache的安装路径\Conf\,如果安装在C盘的根目录下,则该文件应该在“C:\Apache\Conf\”中,此外,打开Windows的“开始菜单”→“程序”→“Apache HTTP Server”→“Edit the Apache httpd.conf Configuration File”也可以,在最新的1.3.26版中,它的作用更加明显。用记事本打开它,可以看到这些配置文件都以文本方式存在,其中“#”为Apache的注释符号,我们可以在记事本菜单中的编辑选项点击“查找”逐一输入下面要配置的关键字,并进行相应配置。如图15在配置文件中查找“DocumentRoot”。

    A.配置DocumentRoot。这个语句指定你的网站路径,也就是你主页放置的目录。你可以使用默认的,一般就是Apache安装目录下的一个子目录,当然也可以自己指定一个,需要注意,这句末尾不要加“\”。此外,路径的分隔符在Apache Server里写成“\”,例如我们可以在此处将其设定为“E:\Ww\Homepages\Homepage”,打开主页时,默认打开的文档就直接去该目录下查找了。

    B.配置DirectoryIndex。这就是你站点默认显示的主页,例如你在“E:\Ww\Homepages\Homepage”中默认的主页名称为“Myfirstweb.htm”,在这里将其添加进来即可。此外,一般情况下,我们在此处还可以加入“Index.htm Index.php Index.php3 Index.cgi Index.pl Default.htm”等。注意,每种类型之间都要留一空格。

    上面两步基本就设置好了,启动IE输入你电脑的IP即可访问自己的Web站点,你也可以在该文件的ServerName处定义你的域名,在ServerAdmin处输入你的E-mail地址。以上两条就是在安装时选择配置的,以后可以在此处修改它们的属性。

    此外,如果你拒绝一部分人访问你的WWW站点,也可以到Apache的安装目录下找到Access文件,输入你禁止的IP地址即可。

    可以看出,Appache没有图形化的配置界面,这也是它非常安全稳定的主要原因,但它的配置却非常简单,只需要在文本文件中输入参数即可,这种WWW服务器的架构方式在所有方式中是最专业的。

    4.WWW服务器架设的其他方式。


    目前有很多WWW服务器架设的软件可供使用,而且它们中很多还是免费软件,大家都可以去试试,这里给出几款软件的简要介绍和下载地址。

    A.AnalogX Simple Server。它简单易用,你只要把“Index.html”拖放到Simple Server中,剩下的就由它来帮你解决了。该软件能在Win9X/NT/2000/XP底下运行,软件大小只有187kB,是一款英文软件,但它完全免费,它的下载站点之一:http://ln.skycn.net/down/sswwwi.exe(如图16)。

    B.自由网站专家XP。它是一款中文软件,无需固定IP地址、无需申请域名,只要在接入互联网的计算机上即可建立网站,使用非常简单,同样能够在Win9X/NT/2000/XP系统中使用,软件大小为2068kB,也是免费软件,下载站点之一:http://ln.skycn.net/down/fwb_xp.exe(如图17)。

    C.天雁Web服务器。这也是一款中文Web服务器的架设工具,界面精美,易于使用。支持虚拟目录,无需安装,不带垃圾,同样它的使用也非常简单。能够在Win9X/NT/2000/XP下使用,软件大小为612kB,也是免费软件,下载站点之一:http://ln.skycn.net/down/webserver.zip(如图18)。




    FTP服务器的架设
    在我们的实际网络生活中,特别是宽带网接入之后,FTP服务器作为文件的传输和共享工具得到广泛应用。FTP服务器在文件的传输上性能稳定,占用系统资源小,而且传输速度快,现在网上已经有很多的FTP服务器可供使用,而自己架设一个FTP服务器也很容易,下面介绍两种主流的FTP架构方式。

    1.利用微软公司的IIS

    微软的IIS功能非常强大,它除了提供WWW服务之外,还提供FTP的服务,利用它一样很容易就能架设一个功能卓越的FTP服务器。

    IIS的安装前面已经讲解过,下面我们一起来看看通过设置IIS来架设FTP服务器的几个步骤。

    第一步:启动IIS,并启动IIS上的FTP服务。在默认的情况下,此时你的FTP服务器已经搭建好,并且可以立即登录,但是该FTP中没有任何文件。

    第二步:鼠标右击IIS中的“默认FTP站点”项,选择“属性”菜单,即可出现如图19的对话框。

    第三步:选择“主目录”的标签,在FTP站点目录的“本地路径”处填上你要设置的共享文件路径。默认情况下,此处的文件夹位置为“C:\Inetpub\Ftproot”,你如果临时想改变共享目录,随时都可在此处修改(如图20),以后别人登录你的FTP服务器时显示的文件列表就是在这个目录中。

    第三步:在“主目录”的标签处,你还可设置FTP服务器的文件访问权限,分别有读取、写入和日志访问,安全起见,这里的写入权限一般不选,保证匿名用户不能随意对你文件进行操作。

    第四步:设置登录的用户。如果你愿意提供“匿名”的访问权限,还需在“安全标签”处选择上“允许匿名连接”(如图21)。此外,你还可从Windows系统帐号中选择FTP服务器的特殊帐号,当然也可以自己任意设置用户名和密码。

    第五步:在“消息”标签处,有“欢迎”、“退出”和“最大连接数”3个输入框,分别代表别人在登录、退出时FTP服务器上给出的提示信息,你可根据自己的需要设置。此外,最大连接数是设置同时连接本地FTP的最大主机台数(如图22)。

    第六步:在“FTP站点”的标签处设置FTP标识,包括说明、IP地址和端口,这里一般不需要改动,按照默认选择即可(如图23)。此外,在“C:\Winnt\System32\Logfiles”目录中你还可以看到连接上你FTP的IP、时间等日志信息。

    此时,利用IE或者任何一款FTP的客户端软件即可登录你架设好的FTP站点。

    2.利用Serv-U

    在FTP服务器的搭建中,Serv-U是目前使用比较多的工具之一。它设置简单,功能强大,而且非常稳定,总体上来说上它比IIS附带的FTP服务器略胜一筹。它适用于所有的Windows版本,是一款共享软件,可以让用户免费使用一个月。

    第一步:Serv-U的下载和安装。

    目前Serv-U的最高版本为4.0,文件大小为2.9MB,它的下载站点之一为“http://www.download.com.cn/show.phtml?action=detail&id=484”。

    点击下载的可执行文件即可开始安装了,安装过程很简单,所有设置保持默认值就可以,按“Next”完成每一步(如图24)。安装完毕,在Windows的桌面上就出现Serv-U的图标,双击Serv-U图标,出现Serv-U主窗口,点击主界面右边窗口的“Start server”即可启动FTP服务器 。

    第二步:Serv-U的配置。

    在Serv-U的安装完成之后即可出现配置向导,可以通过这个向导来对它进行配置,主要步骤如下。

    A.安装程序首先启动一个设置向导帮助你设置FTP服务器,点击“Next”继续。

    B.系统弹出输入IP的对话框,此项需要填入你准备为此FTP服务器绑定的IP地址。除非你的计算机有多个固定的IP地址,并且你只想其中一个被FTP服务器所使用,否则,建议不管你是否有固定的IP地址,都将此项保留为空(即让系统自动侦测),点击“Next”(如图25)。

    C.输入Domain name(域名)。此处填入你FTP服务器的域名。但域名由DNS解析而不是由这里决定,因此实际上你可以填入任意内容,比如像“我的个人FTP服务器”这种对此FTP进行说明的文字。

    D.输入FTP访问的端口号,一般保持默认的21即可。

    E.匿名用户的创建和访问目录的设定。首先向导会提示你是否要创建匿名帐号,这里选择是,如果选择不,则用户需要用户名和密码才能访问FTP服务器。接下来安装向导提示输入匿名用户的主目录(Anonymous home directory),此处按照需要来设定匿名用户访问硬盘的位置。

    F.选择匿名用户是否将其限制在主目录里,如果选择是,则用户只能访问其主目录及以下的目录树;如果选择否,则可以访问其主目录的同级或更高级的目录树。从安全角度考虑,一般建议选是。

    G.创建新用户和访问目录。按照向导的提示一步一步创建新用户并输入密码(如图26),接着指定该用户可访问的目录和用户权限即可。

    到这里,你的个人FTP就已经搭建完成了。不过这还只能实现Serv-U赋予的默认功能和权限,要真正让这个服务器能被你自己随心所欲地控制和管理,则还需要经过以下后续的操作,这主要包括如下几点。

    A.对FTP用户的管理

    欲增加一个新用户(包括增加Anonymous用户),则在Serv-U的一个域中选中Users(用户),然后单击右键,进入New User(新用户),依次根据提示为它设置好User Name(用户名)、Password(密码)、Home directory(主目录)等即可完成(如图27)。

    欲删除一个用户,则在此用户上单击右键,选Delete User(删除用户)即可。

    B.对目录权限的管理

    在Serv-U左边框架中选中用户名,再在右边框架中进入Dir Access(目录存取)窗口,然后在列表中选中相应目录后,就可在窗口的右侧更改当前用户对它的访问权限了(如图28)。

    文件的属性主要包括:

    Read(读):对文件进行读操作(复制、下载,不含查看)的权力。

    Write(写):对文件进行写操作(上传)的权力。

    Append(附加):对文件进行写操作和附加操作的权力。

    Delete(删除):对文件进行删除(上传、更名、删除、移动)操作的权力。

    Execute(执行):直接运行可执行文件的权力。

    List(列表):对文件和目录的查看权力。

    Create(建立):建立目录的权力。

    Remove(移动):对目录进行移动、删除和更名的权力。

    Inherit(继承):如勾选中此项,则以上设置的属性将对当前Path(目录)及其下的整个目录树起作用;否则就只对其当前目录有效。

    C.其他设置

    在Local server下的Setting处还可设置服务器的一些通用信息。

    在“max no.of users”处,设定同时登录该服务器的最大用户数。

    在Max.Speed处根据自己电脑的配置,设置用户最大下载速度。

    选择“Block users who connect more than XX times within YY seconds for ZZ minutes”复选框并设置相应的数值,可以防止有些恶意用户为达到攻击目的在短时间内对该服务器的频繁登录。

    选择“Delete partially uploaded files”复选框,可以自动删除上传失败后留在服务器上不完整文件。如果不要选中这项,就能让Serv-U支持断点上传功能(如图29)。

    3.架设FTP服务器的其他方式。

    A.WS_FTP Server。这是一套非常有特色的FTP Server程序。它有简单而强大的图形介面。设置起来比较容易,可以在Win9X/NT/2000/XP系统下使用,是一个共享的英文软件,文件大小为3.3MB,下载站点之一:http://www.skycn.com/soft/1296.html

    B.FileZilla Server。作为一个小巧、可*的FTP服务器软件,它配置简单,功能比较强大,适合Windows系列中的所有版本,文件大小为637kB,同时它是完全免费的软件,它的汉化版下载站点之一:http://www.skycn.com/soft/8091.html

    C.TYPSoft FTP Server汉化版。由于该软件经过汉化,因此使用起来很容易上手,是一个非常适合初学者的FTP服务器端软件,它配置简单,也能方便地管理用户,软件大小只有480kB,是一款免费软件,它的下载站点之一:http://www.skycn.com/soft/8335.html

    WWW服务器和FTP的访问途径

    WWW的访问都可使用IE或其他浏览器来实现,例如我们经常看到的Natscape和Opera等。由于它的访问很容易,这里就不再详细讨论。

    FTP的访问一般有两种方式,介绍如下:

    A.直接利用IE登录FTP。现在我们正在使用的IE也可作为登录FTP的工具了,跟浏览网页一样,只需要将地址前面的HTTP改为FTP即可,例如访问自己的FTP,可以在浏览器中输入ftp://localhost(如图30),这时是匿名访问方式,如果用IE登录FTP时需用户名和密码,则可以右键调出登录的菜单(如图31),在对话框中输入用户名和密码即可。IE登录FTP服务器之后,FTP服务器上的文件跟本机上的文件一样,可以对其进行复制和粘贴等操作。

    B.利用专用的软件登录FTP。此类软件有很多,比较著名的有FlashFXP、CuteFTP、LeapFTP等。

    个人觉得LeapFTP很不错,操作简单,占用资源也很小,它的用法分步介绍如下。

    第一步:LeapFTP的下载与安装。

    目前LeapFTP较新的版本为2.7.2,是一个共享软件,LeapFTP v2.7.2.592的汉化版可以去http://www.skycn.com/soft/711.html下载。它的安装非常简单,直接一路点击“下一步”即可完成,安装完成只有几个配置文件和它自身一个独立的程序,基本上是一个绿色软件。

    第二步:LeapFTP的使用。

    A.打开LeapFTP,它的主界面如图32。

    B.添加FTP站点。点击菜单上的“Sites”→“Site Manager”,(或直接按快捷键F4),弹出一个FTP站点的管理窗口。点击“Add site”新建一个站点,在右边的对话框中逐一输入该站点的基本信息,例如服务器名称(可以任意填写,主要是为了管理的方便)、服务器地址、端口和用户名等(如图33),要登录该FTP站,只需在左边的窗口中双击该名称即可。

    C.取得FTP服务器上的文件列表并按照需要上传或下载。登录上FTP之后,即可在LeapFTP的右上窗口中看到FTP上的文件列表,如果需要下载,将选中的文件拖入左边的本地硬盘中某个目录里(如图34)即可。同样,也可以用这种方法将硬盘中的文件上传到FTP服务器中去。

    域名的申请和动态IP的解决措施

    为了便于记忆,我们可以申请WWW服务器和FTP服务器地址的域名。

    网易提供免费域名的申请,大家可以去http://my.yeah.net/apply-new.htm上免费获得(如图35),例如申请http://202.117.51.43对应的域名http://forus.yeah.net,这样以后访问自己的WWW服务就再也不需记住那些毫无意义的数字符号了。在浏览器中直接输入自己申请的域名即可。此外,雅克精彩(http://www.k666.com/k666/yu-ming/apply.php)和My001.net网(http://www.my001.net)也都提供免费的WWW服务域名申请。

    对FTP来说,域名的申请站点相对较少,这里推荐老牌的域名转向免费服务提www.dhs.org。打开该网站之后,点击Signup的连接,输入注册内容,包括用户ID、用户姓名和用户的E-mail地址,通过该网站给你发送的E-mail地址来激活注册的帐号。然后即可按照该网站提供的密码登录了,点击“Login”,输入帐号和密码之后即可增加域名的转向服务(如图36)。注册域名之后,以后如果想访问自己的FTP只需输入注册的域名,例如输入ftp://forus.dhs.org代表本机上的FTP服务器。

    我们在架构WWW和FTP服务器时,一般都需要静态的IP地址,其实对很多拨号用户来说,IP经常变化,因此在设置服务器时,还得经常需要将变化的IP告

    Fick's law of diffusion

    Fick's law of diffusion

    Fick's laws of diffusion describe diffusion, and define the diffusion coefficient D.

    History

    Fick's laws of diffusion were derived by Adolf Fick in the year 1855.

    Fick's first law

    Fick's first law is used in steady state diffusion, i.e., when the concentration within the diffusion volume does not change with respect to time (Jin=Jout).

    J = - D \frac{\partial \phi}{\partial x}

    Where

    • J is the diffusion flux in dimensions of [(amount of substance) length-2 time-1], [mol m-2 s-1]
    • D is the diffusion coefficient or diffusivity in dimensions of [length2 time-1], [m2 s-1]
    • ɸ is the concentration in dimensions of [(amount of substance) length-3], [mol m-3]
    • x is the position [length], [m]

    Fick's second law

    Fick's second law is used in non-steady or continually changing state diffusion, i.e., when the concentration within the diffusion volume changes with respect to time.

    \frac{\partial \phi}{\partial t} = D \frac{\partial^2 \phi}{\partial x^2}

    Where

    • ɸ is the concentration in dimensions of [(amount of substance) length-3], [mol m-3]
    • t is time [s]
    • D is the diffusion coefficient in dimensions of [length2 time-1], [m2 s-1]
    • x is the position [length], [m]

    It can be derived from the First Fick's law and the mass balance:

    \frac{\partial \phi}{\partial t} =-\frac {\partial} {\partial x} J = \frac {\partial} {\partial x} (D \frac {\partial} {\partial x} \phi)

    Assuming the diffusion coefficient D to be a constant we can exchange the orders of the differentiating and multiplying on the constant:

    \frac {\partial} {\partial x} (D \frac {\partial} {\partial x} \phi) = D \frac {\partial} {\partial x}  \frac {\partial} {\partial x} \phi= D \frac{\partial^2 \phi}{\partial x^2}

    and, thus, receive the form of the Fick's equations as was stated above.

    For the case of 3-dimensional diffusion the Second Fick's Law looks like:

    \frac{\partial \phi}{\partial t} = D \nabla^2 \phi,

    where \nabla is the usual del operator.

    Finally if the diffusion coefficient is not a constant, but depends upon the coordinate and/or concentration, the Second Fick's Law looks like:

    \frac{\partial \phi}{\partial t} =  \nabla \cdot (D \nabla \phi)

    Applicability

    Equations based on Fick's law have been commonly used to model transport processes in foods, neurons, biopolymers, pharmaceuticals, porous soils, semiconductor doping process, etc. A large amount of experimental research in polymer science and food science has shown that a more general approach is required to describe transport of components in materials undergoing glass transition. In the vicinity of glass transition the flow behavior becomes "non-Fickian". See also non-diagonal coupled transport processes (Onsager relationship).

    Temperature dependence of the diffusion coefficient

    The diffusion coefficient at different temperatures is often found to be well predicted by

    D = D_0 e^{-\frac{E_{A}}{RT}}

    Where:

    • D is the diffusion coefficient
    • D0 is the maximum diffusion coefficient (at infinite temperature)
    • EA is the activation energy for diffusion in dimensions of [energy (amount of substance)-1]
    • T is the temperature in units of [absolute temperature] (kelvins or degrees Rankine)
    • R is the gas constant in dimensions of [energy temperature-1 (amount of substance)-1]


    Typically, a compound's diffusion coefficient is 10,000x greater in air than in water. Carbon dioxide in air has a diffusion coefficient of 16 mm²/s, and in water, its coefficient is 0.0016 mm²/s [1].

    Biological perspective

    The first law gives rise to the formula

    \mathrm{Rate\ of\ diffusion} = \frac{K A (P_2 - P_1)}{D}

    It states that the rate of diffusion of a gas across a membrane is

    • Constant for a given gas at a given temperature by an experimentally determined factor, K
    • Proportional to the surface area over which diffusion is taking place, A
    • Proportional to the difference in partial pressures of the gas across the membrane, P2 - P1
    • Inversely proportional to the distance over which diffusion must take place, or in other words the thickness of the membrane, D.

    Fick's first law is also important in radiation transfer equations. However, in this context it becomes inaccurate when the diffusion constant is low and the radiation becomes limited by the speed of light rather than by the resistance of the material the radiation is flowing through. In this situation, one can use a flux limiter.

    The exchange rate of a gas across a fluid membrane can be determined by using this law together with Graham's law.

    Bernoulli's principle

    Bernoulli's principle
    Bernoulli's equation redirects here; see Bernoulli differential equation for an unrelated topic in ordinary differential equations.

    Bernoulli's principle states that in fluid flow, an increase in velocity occurs simultaneously with decrease in pressure. This principle is a simplification of Bernoulli's equation which states that the sum of all forms of energy in a fluid flowing along an enclosed path (a streamline) is the same at any two points in that path. It is named after the Dutch/Swiss mathematician/scientist Daniel Bernoulli, though it was previously understood by Leonhard Euler and others. In a fluid flow with no viscosity, and therefore one in which a pressure difference is the only accelerating force, it is equivalent to Newton's laws of motion. It is important to note that the only cause of the change in fluid velocity is the difference in pressures either side of it. It is very common for the Bernoulli effect to be quoted as if it states that a change in velocity causes a change in pressure. The Bernoulli principle does not make this statement.

    Examples used to demonstrate the effect

    Lift

    One common way of understanding how an airfoil develops lift relies upon the pressure differential above and below a wing. In this model the pressures can be calculated by finding the velocities around the wing and using Bernoulli's equation. However, this explanation often uses false information, such as the incorrect assumption that the two parcels of air which separate at the leading edge of a wing must meet again at the trailing edge, and the assumption that it is the difference in air speed that causes the changes in pressure.

    Venturis

    A common model to demonstrate the Bernoulli effect is a convergent, divergent nozzle also called a venturi. This is simply a large diameter tube feeding into a smaller diameter tube and then further feeding into another larger tube. Venturis are easier to understand when considering a gas rather than a liquid, but the functions for either are much the same. In order for any gas flow to occur it is essential that the exit pressure is lower than the entry pressure for this system. This pressure difference causes the fluid to accelerate from the intake larger tube into the smaller tube. The stored spring energy available to the fluid because of the pressure difference results in the fluid not only expanding as it goes from higher to lower pressure, but effectively overshooting in its expansion as a result of the mass of the gas particles and compressibility of the gas, springing apart beyond the point where all the forces would be balanced. Before the fluid can spring back, there is more fluid behind it, also at this lower pressure. This first sample of fluid then has no pressure difference either side of it to cause it to spring back. This part of the fluid then remains at a lower pressure until it merges with the slower fluid in the exit tube. The pressure in the exit tube will be higher than that in the smaller middle tube, and so the fluid moving from the smaller to larger tube is slowed down by this pressure difference.

    Venturi effect and carburetors

    Bernoulli's principle can be used to analyze the venturi effect that is used in carburetors and elsewhere. In a carburetor, air is passed through a Venturi tube to increase its speed and by the mechanisms explained above, decrease its pressure. The low pressure air is routed over a tube leading to a fuel bowl. The low pressure sucks the fuel into the airflow so that the combined fuel and air can be sent to the engine. The pressure reduction is proportional to the rate of air flow squared, so that more fuel is sucked in as the air flow increases, and the fuel:air mixture remains roughly the same proportion over a wide range of speeds. The pressure reduction effect can be observed by blowing over the top end of a straw with the bottom of the straw in a container of water; the water level will rise in the straw as the flow over the top of the straw increases in speed.

    Bernoulli equations

    There are typically two different formulations of the equations; one applies to incompressible flow and the other applies to compressible flow.

    Incompressible flow

    The original form, for incompressible flow in a uniform gravitational field (such as on Earth), is:

    {v^2 \over 2}+gh+{p \over \rho}=\mathrm{constant}
    v = fluid velocity along the streamline
    g = acceleration due to gravity on Earth
    h = height from an arbitrary point in the direction of gravity
    p = pressure along the streamline
    ρ = fluid density

    These assumptions must be met for the equation to apply:

    • Inviscid flow − viscosity (internal friction) = 0
    • Steady flow
    • Incompressible flow − ρ = constant along a streamline. Density may vary from streamline to streamline, however.
    • Generally, the equation applies along a streamline. For constant-density potential flow, it applies throughout the entire flow field.

    The decrease in pressure simultaneous with an increase in velocity, as predicted by the equation, is often called Bernoulli's principle.

    The equation is named for Daniel Bernoulli although it was first presented in the above form by Leonhard Euler.

    Compressible flow

    A second, more general form of Bernoulli's equation may be written for compressible fluids, in which case, following a streamline:

    {v^2 \over 2}+ \phi + w =\mathrm{constant}
    \phi \, = gravitational potential energy per unit mass, \phi = gh \, in the case of a uniform gravitational field
    w \, = fluid enthalpy per unit mass, which is also often written as h \, (which conflicts with the use of h \, in this article for "height"). Note that w = \epsilon + \frac{p}{\rho} where \epsilon \, is the fluid thermodynamic energy per unit mass, also known as the specific internal energy or "sie".

    The constant on the right hand side is often called the Bernoulli constant and denoted b. For steady inviscid adiabatic flow with no additional sources or sinks of energy, b is constant along any given streamline. More generally, when b may vary along streamlines, it still proves a useful parameter, related to the "head" of the fluid (see below).

    When shock waves are present, in a reference frame moving with a shock, many of the parameters in the Bernoulli equation suffer abrupt changes in passing through the shock. The Bernoulli parameter itself, however, remains unaffected. An exception to this rule is radiative shocks, which violate the assumptions leading to the Bernoulli equation, namely the lack of additional sinks or sources of energy.

    Derivation

    Incompressible fluids

    The Bernoulli equation for incompressible fluids can be derived by integrating the Euler equations, or applying the law of conservation of energy in two sections along a streamline, ignoring viscosity, compressibility, and thermal effects.

    The simplest derivation is to first ignore gravity and consider constrictions and expansions in pipes that are otherwise straight, as seen in Venturi effect. Let the x axis be directed down the axis of the pipe.

    The equation of motion for a parcel of fluid on the axis of the pipe is

    \rho \frac{dv}{dt}= -\frac{dp}{dx}

    In steady flow, v = v(x) so

    \frac{dv}{dt}= \frac{dv}{dx}\frac{dx}{dt} = \frac{dv}{dx}v=\frac{d}{dx} \frac{v^2}{2}

    With ρ constant, the equation of motion can be written as

    \frac{d}{dx} \left(  \rho \frac{v^2}{2} + p \right) =0

    or

    \frac{v^2}{2} + \frac{p}{\rho}= C

    where C is a constant, sometimes referred to as the Bernoulli constant. We deduce that where the speed is large, pressure is low. In the above derivation, no external work-energy principle is invoked. Rather, the work-energy principle is inherently derived by a simple manipulation of the momentum equation. The derivation that follows includes gravity and applies to a curved trajectory, but a work-energy principle must be assumed.

    A streamtube of fluid moving to the right. Indicated are pressure, height, velocity, distance (s), and cross-sectional area.
    A streamtube of fluid moving to the right. Indicated are pressure, height, velocity, distance (s), and cross-sectional area.

    Applying conservation of energy we find that:

    the work done by the forces in the fluid + decrease in potential energy = increase in kinetic energy.

    The work done by the forces is

    F_{1} s_{1}-F_{2} s_{2}=p_{1} A_{1} v_ {1}\Delta t-p_{2} A_{2} v_{2}\Delta t. \;

    The decrease of potential energy is

    m g h_{1}-m g h_{2}=\rho g A _{1} v_{1}\Delta t h_{1}-\rho g A_{2} v_{2} \Delta t h_{2} \;

    The increase in kinetic energy is

    \frac{1}{2} m v_{2}^{2}-\frac{1}{2} m v_{1}^{2}=\frac{1}{2}\rho A_{2} v_{2}\Delta t v_{2} ^{2}-\frac{1}{2}\rho A_{1} v_{1}\Delta t v_{1}^{2}.

    Putting these together,

    p_{1} A_{1} v_{1}\Delta t-p_{2} A_{2} v_{2}\Delta t+\rho g A_{1} v_{1}\Delta t h_{1}-\rho g A_{2} v_{2}\Delta t h_{2}=\frac{1}{2}\rho A_{2} v_{2}\Delta t v_{2}^{2}-\frac{1}{2}\rho A_{1} v_{1}\Delta t v_{1}^{2}

    or

    \frac{\rho A_{1} v_{1}\Delta t v_{1}^{ 2}}{2}+\rho g A_{1} v_{1}\Delta t h_{1}+p_{1} A_{1 } v_{1}\Delta t=\frac{\rho A_{2} v_{2}\Delta t v_{ 2}^{2}}{2}+\rho g A_{2} v_{2}\Delta t h_{2}+p_{2} A_{2} v_{2}\Delta t.

    After dividing by Δt, ρ and A1v1 (= rate of fluid flow = A2v2 as the fluid is incompressible):

    \frac{v_{1}^{2}}{2}+g h_{1}+\frac{p_{1}}{\rho}=\frac{v_{2}^{2}}{2}+g h_{2}+\frac{p_{2}}{\rho}

    or, as stated in the first paragraph:

    \frac{v^{2}}{2}+g h+\frac{p}{\rho}=C

    Further division by g implies

    \frac{v^{2}}{2 g}+h+\frac{p}{\rho g}=C

    A free falling mass from a height h (in vacuum), will reach a velocity

    v=\sqrt{{2 g}{h}}, or h=\frac{v^{2}}{2 g}.

    The term \frac{v^2}{2 g} is called the velocity head.

    The hydrostatic pressure or static head is defined as

    p=\rho  g  h \,, or h=\frac{p}{\rho  g}.

    The term \frac{p}{\rho  g} is also called the pressure head.

    A way to see how this relates to conservation of energy directly is to multiply by density and by unit volume (which is allowed since both are constant) yielding:

    v^2 \rho + P = constant \, and
    mV^2 + P \cdot volume = constant \,

    Compressible fluids

    The derivation for compressible fluids is similar. Again, the derivation depends upon (1) conservation of mass, and (2) conservation of energy. Conservation of mass implies that in the above figure, in the interval of time Δt, the amount of mass passing through the boundary defined by the area A1 is equal to the amount of mass passing outwards through the boundary defined by the area A2:

    0 = \Delta M_1 - \Delta M_2 = \rho_1 A_1 v_1 \, \Delta t - \rho_2 A_2 v_2 \, \Delta t.

    Conservation of energy is applied in a similar manner: It is assumed that the change in energy of the volume of the streamtube bounded by A1 and A2 is due entirely to energy entering or leaving through one or the other of these two boundaries. Clearly, in a more complicated situation such as a fluid flow coupled with radiation, such conditions are not met. Nevertheless, assuming this to be the case and assuming the flow is steady so that the net change in the energy is zero,

    0 = \Delta E_1 - \Delta E_2 \,

    where ΔE1 and ΔE2 are the energy entering through A1 and leaving through A2, respectively.

    The energy entering through A1 is the sum of the kinetic energy entering, the energy entering in the form of potential gravitational energy of the fluid, the fluid thermodynamic energy entering, and the energy entering in the form of mechanical p\,dV work:

    \Delta E_1 = \left[  \frac{1}{2} \rho_1 v_1^2 + \phi_1 \rho_1 + \epsilon_1 \rho_1  + p_1 \right] A_1 v_1 \, \Delta t

    A similar expression for ΔE2 may easily be constructed. So now setting 0 = ΔE1 - ΔE2:

    0 = \left[  \frac{1}{2} \rho_1 v_1^2+ \phi_1 \rho_1 + \epsilon_1 \rho_1  + p_1 \right] A_1 v_1 \, \Delta t  - \left[ \frac{1}{2} \rho_2 v_2^2 + \phi_2\rho_2 + \epsilon_2 \rho_2  + p_2 \right] A_2 v_2 \, \Delta t

    which can be rewritten as:

    0 = \left[ \frac{1}{2} v_1^2 + \phi_1 + \epsilon_1  + \frac{p_1}{\rho_1} \right] \rho_1 A_1 v_1 \, \Delta t  - \left[  \frac{1}{2} v_2^2  + \phi_2 + \epsilon_2  + \frac{p_2}{\rho_2} \right] \rho_2 A_2 v_2 \, \Delta t

    Now, using the previously-obtained result from conservation of mass, this may be simplified to obtain

    \frac{1}{2}v^2 + \phi + \epsilon + \frac{p}{\rho} = {\rm constant} \equiv b

    which is the Bernoulli equation for compressible flow.

    External links


    This entry is from Wikipedia, the leading user-contributed encyclopedia. It may not have been reviewed by professional editors (see full disclaimer)

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    Britney Spears
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    Britney Spears, Singer

    • Born: 2 December 1981
    • Birthplace: Kentwood, Louisiana
    • Best Known As: Pop superstar singer of ...Baby One More Time

    Name at birth: Britney Jean Spears

    Britney Spears was only 17 when she reached #1 on the U.S. pop music charts with her 1999 debut album ...Baby One More Time. Her catchy tunes and hubba-hubba physique made Spears one of America's biggest pop stars, and she became a near-constant presence on MTV, radio broadcasts and magazine covers around the world. Spears had an early head start on teen stardom: she was in the cast of the Disney Channel's The Mickey Mouse Club during its 1993 and 1994 seasons. (Future pop stars Christina Aguilera, and Justin Timberlake and J.C. Chasez of the band 'N Sync got their starts on the same show. Spears and Timberlake were romantically linked on and off from 2000-2003.) Spears's second album, Oops!...I Did It Again was released in May of 2000 and went gold in its first week. In 2003 she released her third album, In the Zone. She also starred in the 2002 teen road-trip film Crossroads. In that film the younger version of her character, Lucy, was played by her sister, Jamie Lynn Spears, the star of the cable TV comedy Zoey 101.

    Spears married Kevin Federline, a professional dancer, in 2004. The ceremony was held on 18 September, but papers formalizing the wedding weren't filed until October 7th. It was the first marriage for Federline, who previously fathered two children with Moesha star Shar Jackson... Spears and Federline had their first child, a son named Sean Preston Federline, on 14 September 2005. She announced on the David Letterman show on 9 May 2006 that she was pregnant with a second child; her second son was born 12 September 2006. Spears filed for divorce from Federline on 7 November 2006, citing irreconcilable differences... Spears married childhood friend Jason Alexander in an impromptu ceremony in the Little White Wedding Chapel on the Las Vegas Strip in the early morning of 3 January 2004. The couple agreed to an annulment later the same day. Alexander is no relation to Seinfeld star Jason Alexander... Spears was considered for the role of Daisy Duke in the 2005 movie The Dukes of Hazzard, but the role instead went to fellow pop star Jessica Simpson... Spears' middle name is often incorrectly reported to be "Jeau" rather than "Jean."

    Steven Spielberg

    Steven Spielberg
    Source
    Steven Spielberg, Filmmaker / Movie Producer

    • Born: 18 December 1946
    • Birthplace: Cincinnati, Ohio
    • Best Known As: The director of E.T.

    Steven Spielberg got his first contract as a TV director when he was 20 years old. His first TV movie, Duel (1971), was successful enough to earn a theatrical release. Spielberg has since become the most successful movie mogul alive, with directorial credits that include Jaws (1975), Close Encounters of the Third Kind (1977), Raiders of the Lost Ark (1981, co-produced by George Lucas), E.T.: The Extra-Terrestrial (1982) and the dinosaurs-on-the-loose classic Jurassic Park (1993). His huge box office successes have allowed him to make more serious films also, including The Color Purple (1985), Schindler's List (1993) and Saving Private Ryan (1998). In 1994, with fellow Hollywood moguls Jeffrey Katzenberg and David Geffen, he founded the studio Dreamworks SKG.

    Spielberg is married to actress Kate Capshaw; he was formerly married to actress Amy Irving... He took over Stanley Kubrick's long-planned film A.I. (2001) after Kubrick's 1999 death... Spielberg once directed Hollywood legend Joan Crawford in a 1969 episode of the TV series Night Gallery.

    孔子的英文名字

    孔子的英文名字
    孔子收到美国「世界汉学国际研讨会」的请柬,邀他在开幕典礼后作专题演讲。
    孔子十分高兴,准备先去印一盒名片。
    文具店老板见圣人来了,异常恭敬,问清楚名片要中英文对照,就对孔子说:
    「英文的一面,不知该怎么称呼?」
    「不是有现成的Confucius吗?」
    孔子反问。「那是外国人对您老的尊称,把『孔夫子』拉丁化的说法。
    老板笑笑说, 「您老不好意思自称『孔夫子』吧?」
    「那倒是的。」
    孔子想到自己平常鼓吹谦虚之道,不禁沉吟起来。
    「那,该怎么印呢?」
    「杜甫昨天也来过,」
    老板说。「哦,他的名字怎么印的?」孔子问。
    「杜先生本来要印Tu Fu,」老板说,
    「我一听表示不好,太像『豆腐』了。」
    杜先生说,「那就倒过来,叫Fu Tu好了。」
    我说,「那更不行,简直像『胡涂』!」
    「那怎么办?」孔子问。
    「后来我就对诗圣说:
    『您老不是字子美吗?子美,子美。。。。。。有了!』
    杜甫说:『怎么有了?』
    我说:『杜子美,就叫Jimmy Tu吧!』」
    孔子笑起来,叫一声「妙!」
    「其实韩愈也来过,」老板又说。
    「真的呀?」孔子更好奇了。
    「他就印Han Yu吧?」
    「本来他要这样的,」
    老板说。「我一听又说不行,太像Hang you了。
    韩老说,那『倒过来呢?』
    我说,「You hang?那也不行。
    不是『吊死你』就是『你去上吊吧』,
    太不雅了!」
    「那后来呢?」孔子问。
    「后来呀,」老板得意洋洋,
    「还是我想到韩老的故乡,对他说:
    『您老不是韩昌黎吗?』他说『是呀』,
    我说就印Charlie Han好了!」
    「太好了,太好了!」孔子笑罢,又皱起眉头说,「他们都解决了,可是我到底怎么
    印呢?」
    老板想了一下,叫道,「有了!」
    「怎么样?」孔子问。
    「您老不是字仲尼吗?」老板笑道。
    「对呀,」孔子满脸期待。
    老板大声道「而且还曾周游列国,那就印 Johnny Walker 好了!」
    December 16

    Millau Viaduct

    Millau Viaduct
    Millau Viaduct
    Millau Viaduct
    Official name Le Viaduc de Millau
    Carries 4 lanes of the A75 autoroute
    Crosses valley of the River Tarn
    Locale Millau, France
    Design Cable-Stayed
    Longest span 342 metres (1,122 ft)
    Total length 2,460 metres (8,071 ft)
    Width 32 metres (105 ft)
    Clearance below 270 metres (886 ft) at maximum
    Opening date December 14, 2004

    The 'Millau Viaduct' (French: le Viaduc de Millau) is a cable-stayed road bridge that spans the valley of the River Tarn near Millau in southern France. Designed by French bridge engineer Michel Virlogeux in collaboration with British architect Norman Foster, it is the tallest vehicular bridge in the world, with one pier's summit at 343 metres (1,125 ft)—slightly higher than the Eiffel Tower and only 38 m (125 ft) shorter than the Empire State Building. It was formally opened on 14 December 2004 and opened to traffic on 16 December 2004.

    Location

    Millau Viaduct's coordinates are 44.077165° N 3.022887° E. Before the bridge was constructed, traffic had to descend into the Tarn River valley and pass along the route nationale N9 near the town of Millau, causing heavy congestion at the beginning and end of the July and August vacation season. The bridge now traverses the Tarn valley above its lowest point, linking the causse du Larzac to the causse rouge, and is inside the perimeter of the Grands Causses regional natural park.

    The bridge forms the last link of the A75 (la Méridienne) autoroute, providing a continuous high-speed route south from Paris through Clermont-Ferrand to Béziers. The purpose of the A75 is to increase the speed and reduce the cost of vehicle traffic travelling along this route. Many tourists heading to southern France and Spain follow this route because it is direct and without tolls for the 340 km between Clermont-Ferrand to Béziers, except for the bridge itself.

    The Eiffage group operates the viaduct as a toll bridge, with the toll currently set at 4.90 for light automobiles (€6.50 during the peak months of July and August). The bridge was constructed by the Eiffage group, which also built the Eiffel Tower, under a government contract which allows the company to collect tolls for up to 75 years.

    Description

    Panoramic view of Millau Viaduct from south-east side
    Enlarge
    Panoramic view of Millau Viaduct from south-east side

    The Millau Viaduct consists of an eight-span steel roadway supported by seven concrete piers. The roadway weighs 36,000 tonnes and is 2,460 m long, measuring 32 m wide by 4.2 m deep. The six central spans each measure 342 m with the two outer spans measuring 204 m. The roadway has a slope of 3% descending from south to north, and curves in plan section on a 20 km radius to give drivers better visibility. It carries two lanes of traffic in each direction.

    The piers range in height from 77–246 m, and taper in their longitudinal section from 24.5 m at the base to 11 m at the deck. Each pier is composed of 16 framework sections, each section weighing 2,230 tonnes. These sections were assembled on site from pieces of 60 tonnes, 4 m wide and 17 m long, made in factories in Lauterbourg and Fos-sur-Mer by Eiffage. The piers each support 97 m tall pylons. The piers were assembled first, together with some temporary supports, before the decks were slid out across the piers by satellite-guided hydraulic rams that moved the deck 600 mm every 4 minutes.

    The viaduct is the tallest vehicular bridge in the world, nearly twice as tall as the previous tallest vehicular bridge in Europe, the Europabrücke in Austria. (The proposed Strait of Messina Bridge in Italy, if constructed, would be taller.)

    The Millau Viaduct is the second highest vehicular bridge measured from the roadway elevation. Its deck, at approximately 270 m above the Tarn, is slightly higher than the New River Gorge Bridge in West Virginia in the United States, which is 267 m above the New River. The Royal Gorge Bridge in Colorado, United States has a deck considerably higher than either, at 321 m above the Arkansas River.

    Construction

    The viaduct under construction, seen from the south in early 2004
    Enlarge
    The viaduct under construction, seen from the south in early 2004

    Construction began on 10 October 2001 and was intended to take three years, but weather conditions put work on the bridge behind schedule. A revised schedule aimed for the bridge to be opened in January 2005. The viaduct was officially inaugurated by President Chirac on 14 December 2004 to open for traffic on 16 December, several weeks ahead of the revised schedule. The construction of the bridge is depicted in a documentary of the Discovery Channel 'Megastructures' series.

    Preliminary studies

    In initial studies, four options were examined:

    1. bypass Millau to the east, requiring two large bridges over the Tarn and the Dourbie;
    2. bypass Millau to the west (12 km longer), requiring four bridges;
    3. follow the path of Route Nationale 9, providing good access to Millau but at the cost of technical difficulties and intrusion on the town; and
    4. traverse the middle of the valley.

    The fourth option was selected by the government on 28 June 1989. It consisted of two possibilities: the high solution, and the low solution, requiring the construction of a 200 m bridge to cross the Tarn, then a viaduct of 2300 m extended by a tunnel on the Larzac side. After long construction studies, the low solution was abandoned because it would have intersected the water table, had negative effects on the town, cost more, and the driving distance would have been longer.

    After the choice of the high viaduct's path, five teams of architects and researchers simultaneously worked on a technical solution. The original concept for the bridge was devised by French designer Michel Virlogeux. The architects of the bridge are the British firm Foster and Partners. They worked together with the Dutch engineering firm ARCADIS, responsible for the technical design of the bridge.

    Implementation

    The nearly completed bridge in September 2004
    Enlarge
    The nearly completed bridge in September 2004

    The bridge deck was constructed on land at the ends of the viaduct and rolled lengthwise from one tower to the next, with eight temporary added towers also in place. The movement was accomplished by a computer-controlled system of pairs of wedges under the deck; the upper and lower wedges of each pair pointed in opposite directions. These were hydraulically operated, and moved repeatedly in the following sequence:

    • Lower wedge slides under the upper wedge, raising it to the roadway above and then forcing the upper wedge still higher to lift the roadway.
    • Both wedges move together, advancing the roadway a short distance.
    • Lower wedge retracts from under the upper wedge, lowering the roadway and then allowing the upper wedge to drop away from the roadway.
    • Upper wedge moves backward, placing it into position farther (back) along the roadway, ready to repeat the cycle and advance the roadway again.

    The builders

    PERI Formwork technology for the construction of the highest bridge pier
    Enlarge
    PERI Formwork technology for the construction of the highest bridge pier

    Four consortia were in competition for the building contract:

    • One led by Dragados (Spanish), with Skanska (Swedish) and Bec (French);
    • Société du viaduc de Millau, made up of ASF, Egis, GTM, Bouygues Travaux Publics, SGE, CDC Projets, Tofinso (all French) and Autostrade (Italian); and
    • One led by Générale Routière, with Via GTI (French), and Cintra, Necso, Acciona, and Ferrovial Agroman (all Spanish).
    • The successful bidders, lead by the Eiffage group, product of the Fougerolles-SEA fusion, the third largest French group in public works, and the sixth largest in Europe.

    The work leader is the Compagnie Eiffage du Viaduc de Millau, owner of the government contract. The construction consortium is made up of the Eiffage TP company for the concrete part, the Eiffel company for the steel roadway (Gustave Eiffel built the Garabit viaduct in 1884, a train bridge in the neighboring Cantal département), and the Enerpac company for the roadway's hydraulic supports. The engineering group Setec has authority in the project, with SNCF engineering having partial control.

    The formwork technology for the bridge piers came from PERI.

    Costs and resources

    The bridge's construction cost up to €394 million, with a toll plaza 6 km north of the viaduct costing an additional €20 million. The builders, Eiffage, financed the construction in return for a concession to collect the tolls for 75 years, until 2080. However, if the concession is very profitable, the French government can assume control of the bridge in 2044.

    The project required about 127,000  of concrete, 19,000 metric tons of steel for the reinforced concrete, and 5,000 metric tons of pre-stressed concrete for the cables and shrouds. The builder claims that the bridge's lifetime will be at least 120 years.

    Statistics

    • 2,460 metre: total length of the roadway
    • 7: number of piers
    • 77 m: height of Pier 7, the shortest
    • 343 m: height of Pier 2, the tallest (245 m at the roadway's level)
    • 87 m: height of a pylon
    • 154: number of shrouds
    • 270 m: average height of the roadway
    • 4.20 m: thickness of the roadway
    • 32.05 m: width of the roadway
    • 85,000 : total volume of concrete used
    • 290,000 tonnes: total weight of the bridge
    • 10,000–25,000 vehicles: estimated daily traffic
    • 4.90–6.50: typical automobile toll, as of 2005
    • 20 km: horizontal radius of curvature of the road deck

    Project timeline

    • 28 June 1989: governmental approval of the middle route
    • 19 October 1991: selection of the high solution, with the viaduct at 2500 m
    • 10 January 1995: declaration of utilité publique (public usefulness), as needed to apply eminent domain or compulsory purchase.
    • 9 July 1996: choice of the cable-stayed bridge type
    • 1998: decision to contract out both construction costs and future tolls to a private enterprise
    • 16 October 2001: work begins
    • 14 December 2001: laying of the first stone
    • January 2002: laying pier foundations
    • March 2002: start of work on the pier support C8
    • June 2002: support C8 completed, start of work on piers
    • July 2002: start of work on the foundations of temporary, height adjustable roadway supports
    • August 2002: start of work on pier support C0
    • September 2002: assembly of roadway begins
    • November 2002: first piers complete
    • 25 February26 February 2003: laying of first pieces of roadway
    • November 2003: completion of the last piers (Piers P2 at 221 m and P3 at 245 m are the highest piers in the world.)
    • 28 May 2004: the pieces of roadway are several centimetres apart, their juncture to be accomplished within two weeks
    • 2nd half of 2004: installation of the pylons and shrouds, removal of the temporary roadway supports
    • 14 December 2004: official inauguration
    • 16 December 2004: opening of the viaduct, ahead of schedule
    • 10 January 2005: initial planned opening date

    Gallery

    Panoramic view of the Millau Viaduct, as seen from the south. The red temporary supports are still visible in this 29 June 2004 photograph.

    Single segment of the construction on the small exhibition under viaduct

    Large numbers of people stop to observe the viaduct from the viewing area on the northern side

    See also

    External links

    Wikimedia Commons has media related to:
    Viaduc de Millau


    Supertall structures (at least 300 meters in height - Other proposed structures)
    Antennas: Alma-Ata Tower, Azeri TV Tower, Emley Moor, Europaturm, Gerbrandy Tower, Kiev TV Tower, Mumbai Television Tower, Saint Petersburg TV Tower, Sumida Tower (proposed), TV Tower Yerevan, WITI TV Tower, Zendstation Smilde
    Bridges: Millau Viaduct, Strait of Messina Bridge (proposed)
    Dams: Rogun Dam (construction), Nurek Dam, Jinping 1 Hydropower Station (construction)
    Solar towers: Solar Tower Buronga (proposed), Ciudad Real Torre Solar (proposed)
    Electricity pylons: Yangtze River Crossing
    Oil platforms: Petronius Platform, Troll Platform, Hibernia Oil Platform


    Ludwig van Beethoven

    Ludwig van Beethoven
    View Poster
    Ludwig van Beethoven, Composer

    • Born: December 1770
    • Birthplace: Bonn, Germany
    • Died: 26 March 1827 (cirrhosis of the liver, plus dropsy)
    • Best Known As: The composer of Beethoven's Fifth

    Mozart aside, Ludwig van Beethoven is the most famous classical composer of the western world. He is remembered for his powerful and stormy compositions, and for continuing to compose and conduct even after he began to go deaf at age 28. The ominous four-note beginning to his Fifth Symphony -- bom bom bom bommmmm -- is one of the most famous moments in all of music.

    Beethoven never married. After his death his friends found letters to a lover he called "Immortal Beloved," whose identity has never been discovered... Beethoven's precise date of birth is unknown; he was baptized on 17 December 1770, and it is presumed he was born on 16 December.

    Jane Austen

    Jane Austen
    Source
    Jane Austen, Writer

    • Born: 16 December 1775
    • Birthplace: Steventon, Hampshire, England
    • Died: 18 July 1817
    • Best Known As: The author of Pride and Prejudice

    Jane Austen's novels were witty, warm and ironic portraits of the privileged classes of 18th- and 19th-century England. Her best-known works are Emma (1815), Pride and Prejudice (1813) and Sense and Sensibility (1811), though due to the status of women authors at the time, most of her novels were published anonymously. Austen was one of eight children of an English clergyman, and given the accomplishments of her novels she lived a remarkably quiet and domestic life in the rural south of England. She never married and was only 41 when she died. The Pride and Prejudice heroine Elizabeth Bennet and her dashing suitor Mr. Darcy are one of the more famous couples in English fiction.

    Austen has long been a favorite of Hollywood; recent movie adaptations include Pride and Prejudice (2005, with Keira Knightley), Emma (1996, with Gwyneth Paltrow) and Sense and Sensibility (1995, with Emma Thompson and Kate Winslet). The 1995 Alicia Silverstone movie Clueless is considered a whimsical remake of Emma... The exact cause of Austen's early death has never been clear. In the last year of her life she suffered from fatigue, back pain, nausea and fevers as she gradually faded away. Addison's disease, Hodgkin's disease and tuberculosis have all been suggested as possible causes by modern-day scholars.

    Philip K. Dick

    Philip K. Dick
    Source
    Philip K. Dick, Writer

    • Born: 16 December 1928
    • Birthplace: Chicago, Illinois
    • Died: 2 March 1982 (heart failure)
    • Best Known As: Mind-bending sci-fi author

    Philip Kindred Dick was a prolific science fiction author who ditched bug-eyed monsters and spacemen to explore the nature of reality and paranoia on a cosmic scale. In spite of winning a Hugo Award for his 1962 novel The Man in the High Castle, Dick was largely unknown until 1982, when his novel Do Androids Dream of Electric Sheep? was made into the film Blade Runner (directed by RIdley Scott and starring Harrison Ford and Daryl Hannah). After his death Dick's work found a new audience, and the "mainstream" novels of his early career (ignored at the time) were finally published. Among his best-known novels are Martian Time-Slip (1964), Ubik (1969) and Valis (1981).

    Dick was married five times... His friend, K.W. Jeter, has written two sequels to Blade Runner... Dick's story We Can Remember It For You Wholesale was the basis for the 1990 Arnold Schwarzenegger film Total Recall... The 2002 film Minority Report (directed by Steven Spielberg and starring Tom Cruise) is based on a Philip K. Dick story of the same name... Richard Linklater's 2006 film A Scanner Darkly (starring Keanu Reeves) was based on Dick's 1977 novel of the same name.

     

    Bibliography of Philip K. Dick

    Published works

    Novels by year of composition

    Dates are for completion of first (and usually only) draft. Publication dates follow. + indicates subsequent significant expansion, * subsequent revision or minor expansion

    1950
    Gather Yourselves Together (1994)
    1952
    Voices From the Street (forthcoming 2006)
    1953
    Vulcan's Hammer (1960+)
    Dr. Futurity (1960+)
    The Cosmic Puppets (1957*)
    1954
    Solar Lottery (1955*)
    Mary and the Giant (1987*)
    The World Jones Made (1956)
    1955
    Eye in the Sky (1957)
    The Man Who Japed (1956)
    1956
    A Time for George Stavros (ms. lost)
    Pilgrim on the Hill (ms. lost)
    The Broken Bubble (1988)
    1957
    Puttering About in a Small Land (1985)
    1958
    Nicholas and the Higs (ms. lost)
    Time Out of Joint (1959)
    In Milton Lumky Territory (1985)
    1959
    Confessions of a Crap Artist (1975)
    1960
    The Man Whose Teeth Were All Exactly Alike (1982)
    Humpty Dumpty in Oakland (1986)
    1961
    The Man in the High Castle (1962)
    1962
    We Can Build You (1972)
    Martian Time-Slip (1964)
    1963
    Dr. Bloodmoney, or How We Got Along After the Bomb (1965)
    The Game-Players of Titan (1963) (ISBN 0-679-74065-1)
    The Simulacra (1964)
    The Crack in Space (1966+)
    Now Wait for Last Year (1966)
    1964
    Clans of the Alphane Moon (1964)
    The Three Stigmata of Palmer Eldritch (1965)
    The Zap Gun (1967)
    The Penultimate Truth (1964)
    Deus Irae with Roger Zelazny (1976*+)
    The Unteleported Man (1966 / 1983+ / 1984*+ as Lies, Inc.)
    1965
    The Ganymede Takeover with Ray Nelson (1967*)
    Counter-Clock World (1967)
    1966
    Do Androids Dream of Electric Sheep? (1968)
    Nick and the Glimmung (for children) (1988)
    Ubik (1969)
    1968
    Galactic Pot-Healer (1969)
    A Maze of Death (1970)
    1969
    Our Friends from Frolix 8 (1970)
    1970
    Flow My Tears, The Policeman Said (1974*)
    1973
    A Scanner Darkly (1977*)
    1976
    Radio Free Albemuth (1985)
    1978
    VALIS (1981)
    1980
    The Divine Invasion (1981)
    1981
    The Transmigration of Timothy Archer (1982)

    Short stories

    The short stories of Philip K. Dick have recently been republished in five omnibus volumes, as follows:

    1. The Short Happy Life of the Brown Oxford and Other Stories, ISBN 0-8065-1153-2
    2. We Can Remember It for You Wholesale and Other Stories, ISBN 0-8065-1209-1
    3. Second Variety and Other Stories, ISBN 0-8065-1226-1
    4. The Minority Report and Other Stories, ISBN 0-8065-1276-8
    5. The Eye of the Sibyl and Other Stories, ISBN 0-8065-1328-4
    1952
    Beyond Lies the Wub
    The Gun
    The Little Movement
    The Skull
    The Variable Man
    1953
    The Builder
    Colony
    The Commuter
    The Cookie Lady
    The Cosmic Poachers
    The Defenders
    Expendable
    The Eyes Have It
    The Great C
    The Hanging Stranger
    The Impossible Planet
    Impostor
    The Indefatigable Frog
    The Infinities
    The King of the Elves – optioned by Disney Animation in June 2006
    Martians Come in Clouds
    Mr. Spaceship
    Out in the Garden
    Paycheck
    Piper in the Woods
    Planet for Transients
    The Preserving Machine
    Project: Earth
    Roog
    Second Variety
    Some Kinds of Life
    The Trouble with Bubbles
    The World She Wanted
    1954
    A World of Talent
    The Last of the Masters
    Adjustment Team
    Beyond the Door
    Breakfast at Twilight
    The Crawlers
    The Crystal Crypt
    Exhibit Piece
    The Father-thing
    The Golden Man
    James P. Crow
    Jon's World
    The Little Black Box
    Meddler
    Of Withered Apples
    A Present for Pat
    Prize Ship
    Progeny
    Prominent Author
    Sales Pitch
    Shell Game
    The Short Happy Life of the Brown Oxford
    Small Town
    Souvenir
    Strange Eden
    Survey Team
    Time Pawn
    Tony and the Beetles
    The Turning Wheel
    Upon the Dull Earth
    1955
    Autofac
    Captive Market
    The Chromium Fence
    Foster, You're Dead!
    The Hood Maker
    Human Is
    The Mold of Yancy
    Nanny
    Psi-man Heal My Child!
    Service Call
    A Surface Raid
    Vulcan's Hammer
    War Veteran
    1956
    A Glass of Darkness
    Minority Report
    Pay for the Printer
    To Serve the Master
    1957
    Misadjustment
    The Unreconstructed M
    1958
    Null-o
    1959
    Explorers We
    Fair Game
    Recall Mechanism
    War Game
    1963
    All We Marsmen
    The Days of Perky Pat
    If There Were No Benny Cemoli
    Stand-by
    What'll We Do With Ragland Park?
    1964
    Cantata 140
    A Game of Unchance
    Novelty Act
    Oh, to be a Blobel!
    Orpheus with Clay Feet
    Precious Artifact
    The Unteleported Man
    The War with the Fnools
    Waterspider
    What the Dead Men Say
    1965
    Project Plowshare
    Retreat Syndrome
    1966
    Holy Quarrel
    We Can Remember It For You Wholesale
    Your Appointment Will Be Yesterday
    1967
    Faith of our Fathers
    Return Match
    1968
    Not By Its Cover
    The Story To End All Stories
    1969
    A. Lincoln, Simulacrum
    The Electric Ant
    1972
    Cadbury, the Beaver Who Lacked
    1974
    The Different Stages of Love
    The Pre-persons
    A Little Something For Us Tempunauts
    1979
    The Exit Door Leads In
    1980
    I Hope I Shall Arrive Soon - originally titled Frozen Journey
    Rautavaara's Case
    Chains of Air, Web of Aether
    1981
    The Alien Mind
    1984
    Strange Memories Of Death
    1987
    The Day Mr. Computer Fell Out of Its Tree
    The Eye of The Sibyl
    Fawn, Look Back
    Stability
    1988
    Goodbye, Vincent
    1989
    11-17-80
    1992
    The Name of the Game is Death

     

    Film adaptations

    # Film Date Director Source
    work
    Date Type TV
    Series
    Date
    1 Blade Runner 1982 Ridley Scott Do Androids Dream of Electric Sheep? 1968 Novel - -
    2 Total Recall 1990 Paul Verhoeven We Can Remember It For You Wholesale 1966 Short Story Total Recall 2070 1999
    3 Confessions d'un Barjo 1992 Jérôme Boivin Confessions of a Crap Artist 1975 Novel - -
    4 Screamers 1995 Christian Duguay Second Variety 1953 Short Story - -
    5 Minority Report 2002 Steven Spielberg Minority Report 1956 Short Story - -
    6 Impostor 2002 Gary Fleder Impostor 1953 Short Story Episode of Out of This World adapted by Terry Nation 1962
    7 Paycheck 2003 John Woo Paycheck 1953 Short Story - -
    8 A Scanner Darkly 2006 Richard Linklater A Scanner Darkly 1977 Novel - -
    9 Next 2007 Lee Tamahori The Golden Man 1954 Short Story - -

    December 15

    Time:Stardust Surprise

    When the Stardust mission was launched toward Comet Wild 2 back in 1999, planetary scientists weren't sure it would really work: the spacecrafts almost absurdly ambitious mission was to fly by the comet, let particles of comet dust embed themselves in collectors made of aerogel, and then extract the particles after the probe returned to Earth. At the time, nobody knew quite how they'd get the particles out of the collectors.

    The were, however, pretty sure that if they could do it, what they'd find was pristine, material from interstellar space. It's generally agreed that the Sun and planets condensed out of a collapsing cloud of interstellar dust and gas. The comets are mostly ice, formed from gases pushed to the edge of the newborn solar system by the Sun's radiation (gases that only made it partway out formed into the gas-giant planets Jupiter, Saturn, Uranus and Neptune). But the comets are also liberally sprinkled with dust--and that, everyone assumed, had never been near the Sun at all. And since it hadn't been heated, this dust, were pretty sure, would be an untainted sample of the stuff between the stars, more ancient by far than our 4.6-billion-year-old solar system.

    Oops. Turns out that scientists did manage to extract dust particles from the Stardust collectors, and have just published no fewer than 7 papers in Science on what they found.  It' s not what they expected.  To their general astonishment, it turns out that a significant fraction of the comet dust had in fact been heated and altered by the Sun after all. The early Solar System was evidently a more turbulent place than anyone thought, with dust churning in and out of the center: when the comets finally froze out, they carried a record of the churn. That's bad news for the conventional theory, but good news for Frank Shu, the Berkeley scientist who a decade or so ago suggested that intense magnetic fields in the early Solar System could have churned things up more than anyone suspected. There were hints of this last spring, after a preliminary analysis, but today's publication is considered definitive).

    But all is not lost:  there's evidently plenty of actual stardust as well--so even if comets are more complicated creatures than most scientists knew, they'll still offer a window into the time before the Sun was born. Just not as big a window as everyone hoped. 

    Potter Books Upheld In GA

    Potter Books Upheld In GA

    The Georgia Board of Education voted on Dec. 14 to uphold a local school board's decision to leave Harry Potter books on library shelves, despite a mother's objections that they promoted witchcraft, the Associated Press reported.

    The board members voted without discussion to back the Gwinnett County school board's decision to deny Laura Mallory's request to remove the best-selling books.

    Mallory, who has three children in elementary school, has worked for more than a year to ban the books from Gwinnett schools, claiming the popular fiction series is an attempt to indoctrinate children in witchcraft.

    Gwinnett school officials have argued that the books are good tools to encourage children to read and to spark creativity and imagination. Banning all books with references to witchcraft would mean classics such as Macbeth and Cinderella would have to go, they said.

    J.K. Rowling's Harry Potter books have been challenged 115 times since 2000, making them the most challenged texts of the 21st century, according to the American Library Association.

    Del Toro Swings To Tarzan?

    Del Toro Swings To Tarzan?

    Warner Brothers is in negotiations with director Guillermo del Toro to helm a new take on Edgar Rice Burroughs' classic Tarzan character for the big screen, Variety reported. Jerry Weintraub will produce the movie, and John Collee (Master and Commander: Far Side of the World, Happy Feet) is negotiating to write the screenplay. Weintraub will produce through his Jerry Weintraub Prods. banner.

    Del Toro (Pan's Labyrinth, Hellboy) grew up reading Spanish-language translations of Burroghs' books and feels that the classic themes are still compelling, the trade paper reported. Del Toro also sees that there is new ground to cover in the Tarzan mythology by turning back to the original Burroughs prose.

    In the years since Burroughs first introduced the loincloth-clad character in book form in 1914, Tarzan has headlined live-action and animated films, as well as radio and TV shows.

    Pan's Labyrinth opens Dec. 29. Del Toro is in preproduction on Hellboy 2.

    JVC camera is peepers delight with a 34x zoom

    JVC camera is peepers delight with a 34x zoom

    Related Entries:  Camcorders

    jvc gr d750

    This new camcorder from JVC has a pretty insane 34x optical zoom, which should let you see pretty clearly what's happening in your neighbors window across the street. However, have you ever tried keeping a camera steady when it's zoomed in even to 10x? At 34x unless you're some kind of steel-alloy robot your picture would be shaking so badly you wouldn't be able to tell if you're peeping on that cute girl in the house across the way or a flesh-colored armchair. A tripod is a necessity with something like this to say the least.

    Beyond the nutty zoom capabilities of this camera, it's got a 2.7-inch LCD screen and takes MiniDV tapes. It can shoot stills, but at a paltry .34-megapixels it's not really worth even calling it a feature. I mean, my two-year-old cellphone can take nicer pictures than that. Come on, JVC. In any case this camera drops in Japan in January for a bit under $450. — Adam Frucci

    Akihabara News, via Gizmodo