Planck's Law As a Consequence of the Zeropoint Radiation Field
Total Page:16
File Type:pdf, Size:1020Kb
REVISTA MEXICANA DE FISICA´ 48 SUPLEMENTO 1, 1 - 8 SEPTIEMBRE 2002 Planck’s law as a consequence of the zeropoint radiation field L. de la Pena˜ and A.M. Cetto Instituto de F´ısica, Universidad Nacional Autonoma´ de Mexico´ Apdo. Post. 20-364, 01000 Mexico,´ D.F., Mexico Recibido el 19 de marzo de 2001; aceptado el 3 de julio de 2001 In this paper we show that a strong link exists between Planck’s blackbody radiation formula and the zeropoint field. Specifically, the hypothesis that the equilibrium field (including the zeropoint term) follows a canonical distribution, in combination with the requirements that its specific heat remain finite as the temperature T ! 0 and that it behave classically as T ! 1, implies that the energy of the zeropoint field has a fixed value and leads to Planck’s law for the equilibrium distribution at arbitrary T ; this in turn implies quantization of the energy of the field oscillators. There is no need to introduce any quantum property or ad hoc assumption for the purpose of the present derivation. Keywords: Zeropoint field; Planck’s law; blackbody radiation; energy quantization. En este trabajo se exhibe la existencia de una estrecha relacion´ entre la formula´ de Planck para la radiacion´ de cuerpo negro y el campo de punto cero. Espec´ıficamente, la hipotesis´ de que el campo de equilibrio (incluido el termino´ de punto cero) sigue una distribucion´ canonica,´ junto con las demandas de que su calor espec´ıfico se mantenga finito conforme T ! 0 y de que se comporte clsicamente para T ! 1, implica que la energ´ıa del campo de punto cero tiene un valor fijo y conduce a la ley de Planck para la distribucion´ de equilibrio a temperatura arbitraria; esto a su vez implica la cuantizacion´ de la energ´ıa de los osciladores del campo. No hay necesidad de introducir propiedades cuanticas´ o supuestos ad hoc para el proposito´ de la presente derivacion.´ Descriptores: Campo de punto cero; ley de Planck; radiacion´ de cuerpo negro; cuantizacion´ de la energ´ıa. PACS: 02.50.Ey; 03.65.Ta; 05.40.+j To our colleague Leopoldo Garc´ıa Col´ın, with whom we have the fortune to share a long and warm friendship —and a common interest in the fundamentals of physics. 1. Introduction The proposal of Planck and Nernst, appealing as it sounds, remained idle for decades in an obscure corner of As has been repeatedly recalled on occasion of its centen- physics until it was finally revived by Boyer [9], after some nial, the first problem to find an answer in terms of quantum previous attempts, notably those by Park and Epstein [10] and physics was the determination of the spectrum of blackbody Surdin et al. [11] In a first attempt to put to the proof the fea- radiation. Planck noted right from the start [1; 2] —and Eins- sibility of the idea, Boyer showed that a classical treatment of tein elaborated on it briefly afterwards [3]— that the correct the radiation field including a random zeropoint component formula for the spectral distribution of the blackbody radia- of average energy ~!=2 per normal mode, along with some tion field in thermal equilibrium was obtained by introducing assumptions on the role of the container walls in restoring a discrete element; this led to a picture that is now a funda- and maintaining equilibrium, leads to Planck’s distribution mental part of quantum theory. law. This work aroused interest in the subject and triggered What has not been so clearly established, however, is the a whole series of efforts (see e.g. Refs. 12–22), several of link between the Planck distribution (with the ensuing ener- which contain significant positive results; however, what is gy quantization) and the zeropoint field. Planck discovered still wanting is a definitive derivation of the blackbody spec- the latter only in 1911, while formulating his so-called se- trum as a direct result of the presence of the zeropoint field cond theory [4], in which the total mean energy of the matter free of ad hoc assumptions. oscillators contains a zeropoint term ~!=2. The possibility of a direct relationship between quantization as revealed by Planck’s law, and the zeropoint energy of matter oscillators, In the present paper, which is a revision and updating of was envisaged for the first time, still in a classical context, an earlier work [23], we turn back to this problem, carefully by Einstein and Stern in 1913 [5]. However, it was Nernst [7] avoiding the use of any ad hoc assumption but maintaining who a few years later suggested to read Planck’s complete at the same time the simplicity of the reasoning. A couple of blackbody radiation formula as saying that also the electro- elementary and customary statistical and thermodynamic ar- magnetic field possesses such zeropoint fluctuations, and to guments are here used to demonstrate that the quantization consider these fluctuations as the source of quantization. A of the radiation field as implied by Planck’s law, and this law nice discussion of some of these and related points can be itself, follow indeed from the hypothesis of the existence of seen in Milonni’s book [8], where also the case is made for a real fluctuating zeropoint field with energy ~!=2. There is the need to recognize the reality of the zeropoint radiation no need to introduce any explicit quantum property or ad hoc field. assumption for the purpose of the present derivation. 2 ENGLISHL. DE LA PENA˜ AND A.M. CETTO 2. Inconsistency between the zeropoint field For f = Er, r = 0; 1; 2;:::, one obtains in particular and equipartition of energy 0 Er = EEr ¡ Er+1: (8) Let us consider the equilibrium radiation field inside a cavi- ty at temperature T . The field is made of independent modes This result is a generalization of the well-known Einstein for- characterized by a given frequency !, so that we may fo- mula for the thermal energy fluctuations, obtained for r = 1, cus on one frequency in particular. Irrespective of whether dE 2 the system is classical or quantum, the energy is distributed = E ¡ E2: (9) among the modes of a given frequency within the energy in- d¯ terval between E and E + dE following a canonical distribu- Another useful formula derived from Eq. (5) is tion, r r r 1 d Z 1 E = (¡) r ; (10) W (E) dE = g(E)e¡¯E dE; (1) Z d¯ Z of which Eq. (6) is a particular case and Eq. (8) is an imme- where ¯ = 1=kT and g(E) represents the intrinsic probabi- diate consequence. We recall that Eqs. (5)–(10) hold for any lity for the states with energy around E. This is our central function g(E), including of course the classical value g = 1. assumption. In classical physics one has From Einstein’s formula, rewritten as @E 2 g(E) = 1; (2) kT 2 = E2 ¡ E ´ σ2 ; (11) @T E while in quantum physics g(E) takes the form of a discrete a simple relation between the energy fluctuations σ2 and the distribution. The main task of the present investigation is to E specific heat of the field c = @E=@T follows, namely, derive the function g(E) from the assumption of the existence V of the zeropoint radiation field [see Eq. (48)]. 2 2 kT cV = σE : (12) Given their relevance for the present discussion, we recall a couple of (classical) results that are obtained for g(E) = 1. This result holds in principle for any temperature, includ- Firstly, the average energy of every field oscillator is given by ing T = 0 [21; 24]. Hence, since according to the third law Z of thermodynamics c approaches zero as T ! 0, also the 1 1 V E = EW (E) dE = ; (3) energy variance of the field must go to zero as T ! 0. More ¯ 2 0 specifically, it must go to zero as rapidly as T cV (below we see that this means exponentially rapid). and the higher-order moments are given by 2 In classical physics, with E2 = 2E according to Eq. (4), r Er = r!E : (4) this demand on the energy fluctuations implies that E ! 0 as T ! 0, which is automatically satisfied by the equipartition As we see, g(E)=1 leads to equipartition of energy E =kT formula E = kT and leads to the Rayleigh-Jeans distribution among the radiation oscillators and thus it is in contradiction when the result is inserted into the Planck formula for the with experiment, as is well known after a century of quan- equilibrium spectral energy density, ½(!) = (!2=¼2c3)E. tum physics. Thus, results such as Eq. (4) obviously require Things are different in the presence of the zeropoint field, revision. however. Let us denote by E0 the average value of the energy For the general case with arbitray g(E), the partition of this field. Equation (12) tells us that even if E0 > 0, the function is given by variance of the zeropoint energy must vanish, which means Z that ¡¯E Z = g(E)e dE; (5) 2 E2 = E at T = 0; (13) so that its derivative with respect to ¯ is contrary to the (classical) equation [Eq. 4]. This result will play an important role in what follows. In fact, the present 0 Z = ¡Z E: (6) derivation of Planck’s law differs from all previous attempts (except for that of Ref. 23) by this crucial point. Going back Further, for an arbitrary function f(E) one has to Eq. (1), it means that the function g(E) must indeed be a Z 1 non trivial function of the energy.