Feynman Physics Lectures V1 Ch41 1962-04-20 The Brownian Movement

Feynman Physics - 41 The Brownian Movement 41—1 Equipartition of energy The Brownian movement was discovered in 1827 by Robert Brown a botanist

Info iconThis preview shows pages 1–10. Sign up to view the full content.

View Full Document Right Arrow Icon
Background image of page 1

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Background image of page 2
Background image of page 3

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Background image of page 4
Background image of page 5

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Background image of page 6
Background image of page 7

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Background image of page 8
Background image of page 9

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Background image of page 10
This is the end of the preview. Sign up to access the rest of the document.

Unformatted text preview: 41 The Brownian Movement 41—1 Equipartition of energy The Brownian movement was discovered in 1827 by Robert Brown, a botanist. While he was studying microscopic life, he noticed little particles of plant pollens jiggling around in the liquid he was looking at in the microscope, and he was wise enough to realize that these were not living, but were just little pieces of dirt moving around in the water. In fact he helped to demonstrate that this had nothing to do with life by getting from the ground an old piece of quartz in which there was some water trapped. It must have been trapped for millions and millions of years, but inside he could see the same motion. What one sees is that very tiny particles are jiggling all the time. This was later proved to be one of the efi'ects of molecular motion, and we can understand it qualitatively by thinking of a great push ball on a playing field, seen from a great distance, with a lot of people underneath, all pushing the ball in various directions. We cannot see the people because we imagine that we are too far away, but we can see the ball, and we notice that it moves around rather irregularly. We also know, from the theorems that we have discussed in previous chapters, that the mean kinetic energy of a small particle suspended in a liquid or a gas will be ng even though it is very heavy compared with a molecule. If it is very heavy, that means that the speeds are relatively slow, but it turns out, actually, that the speed is not really so slow. In fact, we cannot see the speed of such a particle very easily because although the mean kinetic energy is ng, which represents a speed of a millimeter or so per second for an object a micron or two in diameter, this is very hard to see even in a microscope, because the particle continuously reverses its direction and does not get anywhere. How far it does get we will discuss at the end of the present chapter. This problem was first solved by Einstein at the beginning of the present century. Incidentally, when we say that the mean kinetic energy of this particle is ng, we claim to have derived this result from the kinetic theory, that is, from Newton’s laws. We shall find that we can derive all kinds of things—marvelous things—‘from the kinetic theory, and it is most interesting that we can apparently get so much from so little. Of course we do not mean that Newton’s laws are “little” —they are enough to do it, really~what we mean is that we did not do very much. How do we get so much out? The answer is that we have been perpetually making a certain important assumption, which is that if a given system is in thermal equilibrium at some temperature, it will also be in thermal equilibrium with anything else at the same temperature. For instance, if we wanted to see how a particle would move if it was really colliding with water, we could imagine that there was a gas present, composed of another kind of particle, little fine pellets that (we suppose) do not interact with water, but only hit the particle with “hard” collisions. Suppose the particle has a prong sticking out of it; all our pellets have to do is hit the prong. We know all about this imaginary gas of pellets at tempera- ture T——it is an ideal gas. Water is complicated, but an ideal gas is simple. Now, our particle has to be in equilibrium with the gas of pellets. Therefore, the mean motion of the particle must be what we get for gaseous collisions, because if it were not moving at the right speed relative to the water but, say, was moving faster, that would mean that the pellets would pick up energy from it and get hotter than the water. But we had started them at the same temperature, and we assume that if a thing is once in equilibrium, it stays in equilibrium—parts of it do not get hotter and other parts colder, spontaneously. 41—1 41—1 Equipartition of energy 41—2 Thermal equilibrium of radiation 41—3 Equipartition and the quantum oscillator 41—4 The random walk (a) (b) Fig. 4l—l. (a) A sensitive light-beam galvanometer. Light from a source L is reflected from a small mirror onto a scale. (b) A schematic record of the reading of the scale as a function of the time. R R (a) (b) Fig. 41—2. A high-Q resonant circuit. (0) Actual circuit, at temperature T. (b) Artificial circuit, with an ideal (noise- less) resistance and a "noise generator" G. This proposition is true and can be proved from the laws of mechanics, but the proof is very complicated and can be established only by using advanced mechanics. It is much easier to prove in quantum mechanics than it is in classical mechanics. It was proved first by Boltzmann, but for now we simply take it to be true, and then we can argue that our particle has to have ng of energy if it is hit with artificial pellets, so it also must have ng when it is being hit with water at the same temperature and we take away the pellets; so it is ng. It is a strange line of argument, but perfectly valid. In addition to the motion of colloidal particles for which the Brownian move- ment was first discovered, there are a number of other phenomena, both in the laboratory and in other situations, where one can see Brownian movement. If we are trying to build the most delicate possible equipment, say a very small mirror on a thin quartz fiber for a very sensitive ballistic galvanometer (Fig. 41—1), the mirror does not stay put, but jiggles all the time——all the time—so that when we shine a light on it and look at the position of the spot, we do not have a perfect instrument because the mirror is always jiggling. Why? Because the average kinetic energy of rotation of this mirror has to be, on the average, lkT. What is the mean-square angle over which the mirror will wobble? Suppose we find the natural vibration period of the mirror by tapping on one side and seeing how long it takes to oscillate back and forth, and we also know the moment of inertia, I. We know the formula for the kinetic energy of rotation—it is given by Eq. (19.8): T = %Iw2. That is the kinetic energy, and the potential energy that goes with it will be proportional to the square of the angle—it is V = %a02. But, if we know the period to and calculate from that the natural frequency (do = 27r/to, then the potential energy is V 2 gauge? Now we know that the average kinetic energy is ékT, but since it is a harmonic oscillator the average potential energy is also §kT. Thus was = em or (92) = kT/Iwg. (41.1) In this way we can calculate the oscillations of a galvanometer mirror, and thereby find what the limitations of our instrument will be. If we want to have smaller oscillations, we have to cool the mirror. An interesting question is, where to cool it. This depends upon where it is getting its “kicks” from. If it is through the fiber, we cool it at the top—if the mirror is surrounded by a gas and is getting hit mostly by collisions in the gas, it is better to cool the gas. As a matter of fact, if we know where the damping of the oscillations comes from, it turns out that that is always the source of the fluctuations also, a point which we will come back to. The same thing works, amazingly enough, in electrical circuits. Suppose that we are building a very sensitive, accurate amplifier for a definite frequency and have a resonant circuit (Fig. 41—2) in the input so as to make it very sensitive to this certain frequency, like a radio receiver, but a really good one. Suppose we wish to go down to the very lowest limit of things, so we take the voltage, say off the inductance, and send it into the rest of the amplifier. Of course, in any circuit like this, there is a certain amount of loss. It is not a perfect resonant circuit, but it is a very good one and there is a little resistance, say (we put the resistor in so we can see it, but it is supposed to be small). Now we would like to find out: How much does the voltage across the inductance fluctuate? Answer: We know that %L12 is the “kinetic energy”——the energy associated with a coil in a resonant circuit (Chapter 25). Therefore the mean value of %L12 is equal to §kT—that tells us what the rms current is and we can find out what the rms voltage is from the rms current. For if we want the voltage across the inductance the formula is 171, = iwLI: and the mean absolute square voltage on the inductance is (Vi) = L2w3 I2), and putting in %L(I2) = %kT, we obtain (V%) = LwfikT. (41.2) So now we can design circuits and tell when we are going to get what is called Johnson noise, the noise associated with thermal fluetuations! 41—2 Where do the fluctuations come from this time? They come again from the resistor—they come from the fact that the electrons in the resistor are jiggling around because they are in thermal equilibrium with the matter in the resistor, and they make fluctuations in the density of electrons. They thus make tiny electric fields which drive the resonant circuit. Electrical engineers represent the answer in another way. Physically, the resistor is effectively the source of noise. However, we may replace the real circuit having an honest, true physical resistor which is making noise, by an artificial circuit which contains a little generator that is going to represent the noise, and now the resistor is otherwise ideal—no noise comes from it. All the noise is in the artificial generator. And so if we knew the characteristics of the noise generated by a resistor, if we had the formula for that, then we could calculate what the circuit is going to do in response to that noise. So, we need a formula for the noise fluctuations. Now the noise that is generated by the resistor is at all frequencies, since the resistor by itself is not resonant. Of course the resonant circuit only “listens” to the part that is near the right frequency, but the resistor has many different frequencies in it. We may describe how strong the generator is, as follows: The mean power that the resistor would absorb if it were connected directly across the noise generator would be (E2)/R, if E were the voltage from the generator. But we would like to know in more detail how much power there is at every fre- quency. There is very little power in any one frequency; it is a distribution. Let P(w) dw be the power that the generator would deliver in the frequency range dw into the very same resistor. Then we can prove (we shall prove it for another case, but the mathematics is exactly the same) that the power comes out P(w) dw = (2/7r)kT dw, (41.3) and is independent of the resistance when put this way. 41-2 Thermal equilibrium of radiation Now we go on to consider a still more advanced and interesting proposition that is as follows. Suppose we have a charged oscillator like those we were talking about when we were discussing light, let us say an electron oscillating up and down in an atom. If it oscillates up and down, it radiates light. Now suppose that this oscillator is in a very thin gas of other. atoms, and that from time to time the atoms collide with it. Then in equilibrium, after a long time, this oscillator will pick up energy such that its kinetic energy of oscillation is %kT, and since it is a harmonic oscillator, its entire energy of motion will become kT. That is, of course, a wrong description so far, because the oscillator carries electric charge, and if it has an energy kT it is shaking up and down and radiating light. Therefore it is impossible to have equilibrium of real matter alone without the charges in it emitting light, and as light is emitted, energy flows away, the oscillator loses its kT as time goes on, and thus the whole gas which is colliding with the oscillator gradually cools off. And that is, of course, the way a hot stove cools on a cold night by radiating the light into the sky, because the atoms are jiggling their charge and they contin- ually radiate, and slowly, because of this radiation, the jiggling motion slows down. On the other hand, if we enclose the whole thing in a box so that the light does not go away to infinity, then we can eventually get thermal equilibrium. We may either put the gas in a box where we can say that there are other radiators in the box walls sending light back or, to take a nicer example, we may suppose the box has mirror walls. It is easier to think about that case. Thus we assume that all the radiation that goes out from the oscillator keeps running around in the box. Then, of course, it is true that the oscillator starts to radiate, but pretty soon it can maintain its kT of kinetic energy in spite of the fact that it is radiating, because it is being illuminated, we may say, by its own light reflected from the walls of the box. That is, after a while there is a great deal of light rushing around in the box, and although the oscillator is radiating some, the light comes back and returns some of the energy that was radiated. 41—3 We shall now determine how much light there must be in such a box at tempera- ture T in order that the shining of the light on this oscillator will generate just enough energy to account for the light it radiated. Let the gas atoms be very few and far between, so that we have an ideal oscillator with no resistance except radiation resistance. Then we consider that at thermal equilibrium the oscillator is doing two things at the same time. First, it has a mean energy kT, and we calculate how much radiation it emits. Second, this radiation should be exactly the amount that would result because of the fact that the light shining on the oscillator is scattered. Since there is nowhere else the energy can go, this effective radiation is really just scattered light from the light that is in there. Thus we first calculate the energy that is radiated by the oscillator per second, if the oscillator has a certain energy. (We borrow from Chapter 32 on radiation resistance a number of equations without going back over their derivation.) The energy radiated per radian divided by the energy of the oscillator is called 1 / Q (Eq. 32.8): 1 / Q = (dW/dt)/woW. Using the quantity ‘Y, the damping constant, this can also be written as 1/ Q = W/wo, where (.00 is the natural frequency of the oscillator—if gamma is very small, Q is very large. The energy radiated per second is then dW _ woW _ w0W7 _ 117 ‘ ? — wo _ 7W. (41.4) The energy radiated per second is thus simply gamma times the energy of the oscillator. Now the oscillator should have an average energy kT, so we see that gamma kT is the average amount of energy radiated per second: (dW/dt) = M. (41.5) Now we only have to know what gamma is. Gamma is easily found from Eq. (32.12). It is — “’0 — 2 ’0‘“ (41.6) where r0 = eZ/mc2 is the classical electron radius, and we have set >\ = 27rc/wo. Our final result for the average rate of radiation of light near the frequency we is therefore dW _ 2 rotong 7? _ 5 c ' (41.7) Next we ask how much light must be shining on the oscillator. It must be enough that the energy absorbed from the light (and thereupon scattered) is just exactly this much. In other words, the emitted light is accounted for as scattered light from the light that is shining on the oscillator in the cavity. So we must now calculate how much light is scattered from the oscillator if there is a certam amount —unknown—of radiation incident on it. Let 1(w) dw be the amount of light energy there is at the frequency to, within a certain range do.) (because there is no light at exactly a certain frequency; it is spread all over the spectrum). So [(w) is a certain spectral distribution which we are now going to find—it is the color of a furnace at temperature T that we see when we open the door and look in the hole. Now how much light is absorbed? We worked out the amount of radiation absorbed from a given incident light beam, and we calculated it in terms of a cross section. It is just as though we said that all of the light that falls on a certain cross section is absorbed. So the total amount that is re-radiated (scattered) is the incident intensity 1(w) dw multiplied by the cross section a. The formula for the cross section which we derived (Eq. 31.19) did not have the damping included. It is not hard to go through the derivation again and put in the resistance term which we neglected. If we do that, and calculate the cross section the same way, we get 81rr3 w4 414 Now, as a function of frequency, a, is of significant size only for a) very near to the natural frequency (.00. (Remember that the Q for a radiating oscillator is about 108.) The oscillator scatters very strongly when w is equal to wo, and very weakly for other values of (.0. Therefore we can replace w by too and w2 — cog by 2w0(w — coo), and we get 21rr3w3 =aw~mfi¥wm‘ Now the whole curve is localized near 0) = am. (We do not really have to make any approximations, but it is much easier to do the integrals if we simplify the equation a bit.) Now we multiply the intensity in a given frequency range by the cross section of scattering, to get the amount of energy scattered in the range dw. The total energy scattered is then the integral of this for all w. Thus 0'3 (41.9) dag/8 = /0 1(w)a,(w)dw (41 . 10) 2717'?)ng (to) do.) =flMw—MVIMM' Now we set dWs/dt = 37kT. Why three? Because when we made our analysis of the cross section in Chapter 32, we assumed that the polarization was such that the light could drive the oscillator. If we had used an oscillator which could move only in one direction, and the light, say, was polarized in the wrong way, it would not give any scattering. So we must either average the cross section of an oscillator which can go only in one direction, over all directions of incidence and polarization of the light or, more easily, we can imagine an oscillator which will follow the field no matter which way the field is pointing. Such an oscillator, which can oscillate equally in three directions, would have 3kT average energy because there are 3 degrees of freedom in that oscillator. So we should use 37kT because of the 3 degrees of freedom. Now we have to do the integral. Let us suppose that the unknown spectral distribution I(w) of the light is a smooth curve and does not vary very much across the very narrow frequency region where a, is peaked (Fig. 41—3). Then the only significant contribution comes when w is very close to coo, within an amount gamma, which is very small. So therefore, although 1(a)) may be an unknown and complicated function, the only place where it is important is near to = too, and there we may replace the smooth curve by a flat one—a “constant”——at the same height. In other words, we simply take [(00) outside the integral sign and call it [(wo). We may also take the rest of the constants out in front of the integral, and what we have left is w dw 0 (w — 600V ‘1‘ 72/4 Now, the integral should go from 0 to 00, but 0 is so far from wo that the curve is all finished by that time, so we go instead to minus oo—it makes no difference and it is much easier to do the integral. The integral is an inverse tangent function of the form fdx/(x2 + a2). If we look it up in a book we see that it is equal to 1r/a. So what it comes to for our case is 27/7. Therefore we get, with some re- arranging, : 37kT. (41.11) 2 2 %7r0w01(w0) 972kT _ 41r2r3w3 [(090) = (41.12) Then we substitute the formula (41.6) for gamma (do not worry about writing coo; since it is true of any coo, we may just call it w) and the formula for 1(a)) then comes out (0sz . 7r2c2 1(a)) = (41.13) And that gives us the distribution of light in a hot furnace. It is called the black- 41—5 Fig. 41—3. The factors in the integrand (41.10). The peak is the resonance curve l/(w — mg)2 + 72/4. To a good ap- proximation the factor I(w) can be replaced by l(wo). Ital) Fig. 41—4. The blackbody intensity distribution at two temperatures, accord- ing to classical physics (solid curves). The dashed curves show the actual distribution. body radiation. Black, because the hole in the furnace that we look at is black when the temperature is zero. Inside a closed box at temperature T, (41.13) is the distribution of energy of the radiation, according to classical theory. First, let us notice a remarkable feature of that expression. The charge of the oscillator, the mass of the oscillator, all properties specific to the oscillator, cancel out, because once we have reached equilib- rium with one oscillator, we must be at equilibrium with any other oscillator of a different mass, or we will be in trouble. So this is an important kind of check on the proposition that equilibrium does not depend on what we are in equilibrium with, but only on the temperature. Now let us draw a picture of the 1(w) curve (Fig. 41—4). It tells us how much light we have at different frequencies. The amount of intensity that there is in our box, per unit frequency range, goes, as we see, as the square of the frequency, which means that if we have a box at any temperature at all, and if we look at the x-rays that are coming out, there will be a lot of them! Of course we know this is false. When we open the furnace and take a look at it, we do not burn our eyes out from x-rays at all. It is completely false. Further- more, the total energy in the box, the total of all this intensity summed over all frequencies, would be the area under this infinite curve. Therefore, something is fundamentally, powerfully, and absolutely wrong. Thus was the classical theory absolutely incapable of correctly describing the distribution of light from a blackbody, just as it was incapable of correctly de- scribing the specific heats of gases. Physicists went back and forth over this deriva- tion from many different points of view, and there is no escape. This is the pre- diction of classical physics. Equation (41.13) is called Rayleigh’s law, and it is the prediction of classical physics, and is obviously absurd. 41—3 Equipartition and the quantum oscillator The difficulty above was another part of the continual problem of classical physics, which started with the difficulty of the specific heat of gases, and now has been focused on the distribution of light in a blackbody. Now, of course, at the time that theoreticians studied this thing, there were also many measurements of the actual curve. And it turned out that the correct curve looked like the dashed curves in Fig. 41—4. That is, the x-rays were not there. If we lower the temperature, the whole curve goes down in proportion to T, according to the classical theory, but the observed curve also cuts off sooner at a lower temperature. Thus the low- frequency end of the curve is right, but the high-frequency end is wrong. Why? When Sir James Jeans was worrying about the specific heats of gases, he noted that motions which have high frequency are “frozen out” as the temperature goes too low. That is, if the temperature is too low, if the frequency is too high, the oscillators do not have kT of energy on the average. Now recall how our derivation of (41.13) worked: It all depends on the energy of an oscillator at thermal equilib- rium. What the kT of (41.5) was, and what the same kT in (41.13) is, is the mean energy of a harmonic oscillator of frequency to at temperature T. Classically, this is kT, but experimentally, nol—not when the temperature is too low or the oscillator frequency is too high. And so the reason that the curve falls off is the same reason that the specific heats of gases fail. It is easier to study the blackbody curve than it is the specific heats of gases, which are so complicated, therefore our attention is focused on determining the true blackbody curve, because this curve is a curve which correctly tells us, at every frequency/what the average energy of harmonic oscillators actually is as a function of temperature. Planck studied this curve. He first determined the answer empirically, by fitting the observed curve with a nice function that fitted very well. Thus he had an empirical formula for the average energy of a harmonic oscillator as a function of frequency. In other words, he had the right formula instead of kT, and then by fiddling around he found a simple derivation for it which involved a very peculiar assumption. That assumption was that the harmonic oscillator can take up energies only fit.) at a time. The idea that they can have any energy at all is false. Of course, that was the beginning of the end of classical mechanics. 41—6 The very first correctly determined quantum-mechanical formula will now be derived. Suppose that the permitted energy levels of a harmonic oscillator were equally spaced at hwo apart, so that the oscillator could take on only these different energies (Fig. 41—5). Planck made a somewhat more complicated argument than the one that is being given here, because that was the very beginning of quantum mechanics and he had to prove some things. But we are going to take it as a fact (which he demonstrated in this case) that the probability of occupying a level of energy E is P(E) = axe—EH”. If we go along with that, we will obtain the right result. Suppose now that we have a lot of oscillators, and each is a vibrator of fre- quency we. Some of these vibrators will be in the bottom quantum state, some will be in the next one, and so forth. What we would like to know is the average energy of all these oscillators. To find out, let us calculate the total energy of all the oscilla- tors and divide by the number of oscillators. That will be the average energy per oscillator in thermal equilibrium, and will also be the energy that is in equilibrium with the blackbody radiation and that should go in Eq. (41.13) in place of kT. Thus we let N 0 be the number of oscillators that are in the ground state (the lowest energy state); N1 the number of oscillators in the state E1; N 2 the number that are in state E2; and so on. According to the hypothesis (which we have not proved) that in quantum mechanics the law that replaced the probability e_P‘E'/kT or e_K'E"kT in classical mechanics is that the probability goes down as e‘”’”, where AE is the excess energy, we shall assume that the number N1 that are in the first state will be the number N 0 that are in the ground state, times e‘M/kT. Simi- larly, N 2, the number of oscillators in the second state, is N 2 = Noe—2W”. To simplify the algebra, let us call e“'l"’”‘T = x. Then we simply have N1 = N 0x, N2 = Noxz, . . . ,Nn = Nox”. The total energy of all the oscillators must first be worked out. If an oscillator is in the ground state, there is no energy. If it is in the first state, the energy is hwo, and there are N1 of them. So N lhw, or thox is how much energy we get from those. Those that are in the second state have Zhwo, and there are N 2 of them, so N 2 - 2hw = Zthox2 is how much energy we get, and so on. Then we add it all together to get Em = Nohw(0 + x + 2x2 + 3x3 + . . .). And now, how many oscillators are there? Of course, N 0 is the number that are in the ground state, N1 in the first state, and so on, and we add them together: N101 = No(1 + x + x2 + x3 + . . .). Thus the average energy is _ Etot =1_Vohw(0+x+2x2+3x3+...). Ntot N0(l +x+x2+...) Now the two sums which appear here we shall leave for the reader to play with and have some fun with. When we are all finished summing and substituting for x in the sum, we should get—if we make no mistakes in the sum— hw efiu/kT _ 1 (E) (41.14) (E) = (41.15) This, then, was the first quantum-mechanical formula ever known, or ever discussed, and it was the beautiful culmination of decades of puzzlement. Maxwell knew that there was something wrong, and the problem was, what was right? Here is the quantitative answer of what is right instead of kT. This expression should, of course, approach kT as w —> 0 or as T —> 00. See if you can prove that it does— learn how to do the mathematics. This is the famous cutoff factor that Jeans was looking for, and if we use it instead of kT in (41.13), we obtain for the distribution of light in a black box hw3 dco 7“_2c2(e7im/ICT _ We see that for a large to, even though we have (.03 in the numerator, there is an e raised to a tremendous power in the denominator, so the curve comes down again and does not “blow up”—we do not get ultraviolet light and x-rays where we do not expect them! 1(a)) do) = (41.16) 41—7 —‘— E4 - 41w P. - onp(-4fm/kT) 95- AexM-SM/k'l'l E2 - 211w Pz - Acxu-ZMIKT) N —l— E, - 11w P, - Aupt-‘fiw/kT) No Eu- 0 Po- A Fig. 41—5. The energy levels of a harmonic oscillator are equally spaced: 5,, = nhw. 36 Fig. 41—6. A random walk of 36 steps of length I. How far is $36 from B? Ans: about 6! on the average. One might complain that in our derivation of (41.16) we used the quantum theory for the energy levels of the harmonic oscillator, but the classical theory in determining the cross section 08. But the quantum theory of light interacting with a harmonic oscillator gives exactly the same result as that given by the classical theory. That, in fact, is why we were justified in spending so much time on our analysis of the index of refraction and the scattering of light, using a model of atoms like little oscillators—~the quantum formulas are substantially the same. Now let us return to the Johnson noise in a resistor. We have already re- marked that the theory of this noise power is really the same theory as that of the classical blackbody distribution. In fact, rather amusingly, we have already said that if the resistance in a circuit were not a real resistance, but were an antenna (an antenna acts like a resistance because it radiates energy), a radiation resistance, it would be easy for us to calculate what the power would be. It would be just the power that runs into the antenna from the light that is all around, and we would get the same distribution, changed by only one or two factors. We can suppose that the resistor is a generator with an unknown power spectrum P(w). The spec- trum is determined by the fact that this same generator, connected to a resonant circuit of any frequency, as in Fig. 41—2(b), generates in the inductance a voltage of the magnitude given in Eq. (41.2). One is thus led to the same integral as in (41.10), and the same method works to give Eq. (41.3). For low temperatures the kT in (41.3) must of course be replaced by (41.15). The two theories (blackbody radiation and Johnson noise) are also closely related physically, for we may of course connect a resonant circuit to an antenna, so the resistance R is a pure radiation resistance. Since (41.2) does not depend on the physical origin of the resistance, we know the generator G for a real resistance and for radiation resist- ance is the same. What is the origin of the generated power P(w) if the resistance R is only an ideal antenna in equilibrium with its environment at temperature T? It is the radiation [(02) in the space at temperature Twhich impinges on the antenna and, as “received signals,” makes an effective generator. Therefore one can deduce a direct relation of P(w) and 1(a)), leading then from (41.13) to (41.3). All the things we have been talking about—the so-called Johnson noise and Planck’s distribution, and the correct theory of the Brownian movement which we are about to describe—are developments of the first decade or so of this century. Now with those points and that history in mind, we return to the Brownian move- ment. 41—4 The random walk Let us consider how the position of a jiggling particle should change with time, for very long times compared with the time between “kicks.” Consider a little Brownian movement particle which is jiggling about because it is bombarded on all sides by irregularly jiggling water molecules. Query: After a given length of time, how far away is it likely to be from where it began? This problem was solved by Einstein and Smoluchowski. If we imagine that we divide the time into little intervals, let us say a hundredth of a second or so, then after the first hundredth of a second it moves here, and in the next hundredth it moves some more, in the next hundredth of a second it moves somewhere else, and so on. In terms of the rate of bombardment, a hundredth of a second is a very long time. The reader may easily verify that the number of collisions a single molecule of water receives in a second is about 10 14, so in a hundredth of a second it has 1012 collisions, which is a lot! Therefore, after a hundredth of a second it is not going to remember what happened before. In other words, the collisions are all random, so that one “step” is not related to the previous “step.” It is like the famous drunken sailor problem: the sailor comes out of the bar and takes a sequence of steps, but each step is chosen at an arbitrary angle, at random (Fig. 41—6). The question is: After a long time, where is the sailor? Of course we do not know! It is impossible to say. What do we mean—he is just somewhere more or less random. Well then, on the average, where is he? 0n the average, how far away from the bar has he gone? We have already answered this question, because once we were discussing the 41—8 superposition of light from a whole lot of different sources at different phases, and that meant adding a lot of arrows at different angles (Chapter 32). There we discovered that the mean square of the distance from one end to the other of the chain of random steps, which was the intensity of the light, is the sum of the intensities of the separate pieces. And so, by the same kind of mathematics, we can prove immediately that if RN is the vector distance from the origin after N steps, the mean square of the distance from the origin is proportional to the number N of steps. That is, (Riv) = NL2, where L is the length of each step. Since the num- ber of steps is proportional to the time in our present problem, the mean square distance is proportional to the time: (R2) = at. (41.17) This does not mean that the mean distance is proportional to the time. If the mean distance were proportional to the time it would mean that the drifting is at a nice uniform velocity. The sailor is making some relatively sensible headway, but only such that his mean square distance is proportional to time. That is the character- istic of a random walk. We may show very easily that in each successive step the square of the distance increases, on the average, by L2. For if we write RN = RN_1 + L, we find that Rir is RN -RN = R13 = R134 + 2RN_1 - L + L2, and averaging over many trials, we have (Rgzv) = (R12V_1> + L2, since (RN_1 -L) = 0. Thus. by induction, R12v = NL2. (41.18) Now we would like to calculate the coefficient a in Eq. (41.17), and to do so we must add a feature. We are going to suppose that if we were to put a force on this particle (having nothing to do with the Brownian movement—we are taking a side issue for the moment), then it would react in the following way against the force. First, there would be inertia. Let m be the coeffic1ent of inertia, the eflective mass of the object (not necessarily the same as the real mass of the real particle, because the water has to move around the particle if we pull on it). Thus if we talk about motion in one direction, there is a term like m (d2x/dt2) on one side. And next, we want also to assume that if we kept a steady pull on the object, there would be a drag on it from the fluid, proportional to its velocity. Besides the inertia of the fluid, there is a resistance to flow due to the viscosity and the complexity of the fluid. It is absolutely essential that there be some irreversible losses, something like resistance, in order that there be fluctuations. There is no way to produce the kT unless there are also losses. The source of the fluctuations is very closely related to these losses. What the mechanism of this drag is, we will discuss soon—we shall talk about forces that are proportional to the velocity and where they come from. But let us suppose for now that there is such a resistance. Then the formula for the motion under an external force. when we are pulling on it in a normal manner, is dzx dx The quantity n can be determined directly from experiment. For example, we can watch the drop fall under gravity. Then we know that the force is mg, and p is mg divided by the speed of fall the drop ultimately acquires. Or we could put the drop in a centrifuge and see how fast it sediments. Or if it is charged, we can put an electric field on it. So a is a measurable thing, not an artificial thing, and it is knowu for many types of colloidal particles, etc. Now let us use the same formula in the case where the force is not external, but is equal to the irregular forces of the Brownian movement. We shall then try to determine the mean square distance that the object goes. Instead of taking the distances in three dimensions, let us take just one dimension, and find the mean of x2, just to prepare ourselves. (Obviously the mean of x2 is the same as the mean of y2 is the same as the mean of 22, and therefore the mean square of the distance 41—9 is just 3 times what we are going to calculate.) The x-component of the irregular forces is, of course, just as irregular as any other component. What is the rate of change of x2? It is d(x2)/dt = 2x(dx/d1), so what we have to find is the average of the position times the velocity. We shall show that this is a constant, and that therefore the mean square radius will increase proportionally to the time, and at what rate. Now if we multiply Eq. (41.19) by x, mx(d2x/dt2) + ux(dx/ dz) = sz. We want the time average of x(dx/dt), so let us take the average of the whole equation, and study the three terms. Now what about x times the force? If the particle happens to have gone a certain distance x, then, since the irregular force is completely irregular and does not know where the particle started from, the next impulse can be in any direction relative to x. If x is positive, there is no reason why the average force should also be in that direction. It is just as likely to be one way as the other. The bombardment forces are not driving it in a definite direction. So the average value of x times F is zero. On the other hand, for the term mx(d2x/dt2) we will have to be a little fancy, and write this as d2x _ m d[x(dx/dt)] _ m (dx)2 "MHz—2 _ dt d7 Thus we put in these two terms and take the average of both. So let us see how much x times the velocity should be. Now x times the velocity has a mean that does not change with time, because when it gets to some position it has no re- membrance of where it was before, so things are no longer changing with time. So this quantity, on the average, is zero. We have left the quantity mvz, and that is the only thing we know: m02/2 has a mean value fikT. Therefore we find that d2 d <mxafix + ,u<xd—:C = (xF,) implies _ 2 £1 2 = (mv>+2dt(x> 0, 01‘ 2 ‘12:) = 2 (41.20) Therefore the object has a mean square distance (R2), at the end of a certain amount of t, equal to (R2) = 6kTi. (41.21) And so we can actually determine how far the particles go! We first must determine how they react to a steady force, how fast they drift under a known force (to find it), and then we can determine how far they go in their random motions. This equation was of considerable importance historically, because it was one of the first ways by which the constant k was determined. After all, we can measure it, the time, how far the particles go, and we can take an average. The reason that the determination of k was important is that in the law PV = RT for a mole, we know that R, which can also be measured, is equal to the number of atoms in a mole times k. A mole was originally defined as so and so many grams of oxygen— 16 (now carbon is used), so the number of atoms in a mole was not known, orig- inally. It is, of course, a very interesting and important problem. How big are atoms? How many are there? So one of the earliest determinations of the number of atoms was by the the determination of how far a dirty little particle would move if we watched it patiently under a microscope for a certain length of time. And thus Boltzmann’s constant k and the Avogadro number N 0 were determined be- cause R had already been measured. 41-10 ...
View Full Document

This note was uploaded on 06/18/2009 for the course PHYSICS Physics taught by Professor Limkong during the Spring '09 term at Uni. Nottingham - Malaysia.

Page1 / 10

Feynman Physics - 41 The Brownian Movement 41—1 Equipartition of energy The Brownian movement was discovered in 1827 by Robert Brown a botanist

This preview shows document pages 1 - 10. Sign up to view the full document.

View Full Document Right Arrow Icon
Ask a homework question - tutors are online