Dirac large numbers hypothesis

Paul Dirac

The Dirac large numbers hypothesis (LNH) is an observation made by Paul Dirac in 1937 relating ratios of size scales in the Universe to that of force scales. The ratios constitute very large, dimensionless numbers: some 40 orders of magnitude in the present cosmological epoch. According to Dirac's hypothesis, the apparent similarity of these ratios might not be a mere coincidence but instead could imply a cosmology with these unusual features:

The strength of gravity, as represented by the gravitational constant, is inversely proportional to the age of the universe: $G \propto 1/t\,$
The mass of the universe is proportional to the square of the universe's age: $M \propto t^2$ .

Neither of these two features has gained wide acceptance in mainstream physics.

Background

LNH was Dirac's personal response to a set of large number 'coincidences' that had intrigued other theorists of his time. The 'coincidences' began with Hermann Weyl (1919),^[1]^[2] who speculated that the observed radius of the universe, R_U, might also be the hypothetical radius of a particle whose rest energy is equal to the gravitational self-energy of the electron:

\frac {R_U}{r_e}\approx \frac{r_H}{r_e} \approx 10^{42} ,

r_e = \frac {e^2}{4 \pi \epsilon_0 m_e c^2},

r_H = \frac {e^2}{4 \pi \epsilon_0 m_H c^2},

m_H c^2 = \frac {Gm_e^2}{r_e}

where r_e is the classical electron radius, m_e is the mass of the electron, m_H denotes the mass of the hypothetical particle, and r_H is its electrostatic radius.

The coincidence was further developed by Arthur Eddington (1931)^[3] who related the above ratios to N, the estimated number of charged particles in the universe:

\frac {e^2}{4 \pi \epsilon_0 Gm_e^2} \approx \sqrt {N} \approx 10^{42}.

In addition to the examples of Weyl and Eddington, Dirac was influenced also by the primeval-atom hypothesis of Georges Lemaître, who lectured on the topic in Cambridge in 1933. The notion of a varying-G cosmology first appears in the work of Edward Arthur Milne a few years before Dirac formulated LNH. Milne was inspired not by large number coincidences but by a dislike of Einstein's general theory of relativity.^[4]^[5] For Milne, space was not a structured object but simply a system of reference in which Einstein's conclusions could be accommodated by relations such as this:

G = \left(\frac{c^3}{M_U}\right)t,

where M_U is the mass of the universe and t is the age of the universe in seconds. According to this relation, G increases over time.

Dirac's interpretation of the large number coincidences

The Weyl and Eddington ratios above can be rephrased in a variety of ways, as for instance in the context of time:

\frac {ct}{r_e} \approx 10^{40},

where t is the age of the universe, $c$ is the speed of light and r_e is the classical electron radius. Hence, in units where c=1 and r_e = 1, the age of the universe is about 10⁴⁰ units of time. This is the same order of magnitude as the ratio of the electrical to the gravitational forces between a proton and an electron:

\frac{e^2}{4 \pi \epsilon_0 G m_p m_e} \approx 10^{40}.

Hence, interpreting the charge $e$ of the electron, the mass $m_p$ / $m_{e}$ of the proton/electron, and the permittivity factor $4 \pi \epsilon_0$ in atomic units (equal to 1), the value of the gravitational constant is approximately 10⁻⁴⁰. Dirac interpreted this to mean that $G$ varies with time as $G \approx 1/t\,$ . Although George Gamov noted that such a temporal variation does not necessarily follow from Dirac's assumptions,^[6] a corresponding change of G has not been found.^[7] According to general relativity, however, G is constant, otherwise the law of conserved energy is violated. Dirac met this difficulty by introducing into the Einstein field equations a gauge function β that describes the structure of spacetime in terms of a ratio of gravitational and electromagnetic units. He also provided alternative scenarios for the continuous creation of matter, one of the other significant issues in LNH:

'additive' creation (new matter is created uniformly throughout space) and
'multiplicative' creation (new matter is created where there are already concentrations of mass).

Later developments and interpretations

Dirac's theory has inspired and continues to inspire a significant body of scientific literature in a variety of disciplines. In the context of geophysics, for instance, Edward Teller seemed to raise a serious objection to LNH in 1948^[8] when he argued that variations in the strength of gravity are not consistent with paleontological data. However, George Gamow demonstrated in 1962^[9] how a simple revision of the parameters (in this case, the age of the Solar System) can invalidate Teller's conclusions. The debate is further complicated by the choice of LNH cosmologies: In 1978, G. Blake^[10] argued that paleontological data is consistent with the 'multiplicative' scenario but not the 'additive' scenario. Arguments both for and against LNH are also made from astrophysical considerations. For example, D. Falik^[11] argued that LNH is inconsistent with experimental results for microwave background radiation whereas Canuto and Hsieh^[12]^[13] argued that it is consistent. One argument that has created significant controversy was put forward by Robert Dicke in 1961. Known as the anthropic coincidence or fine-tuned universe, it simply states that the large numbers in LNH are a necessary coincidence for intelligent beings since they parametrize fusion of hydrogen in stars and hence carbon-based life would not arise otherwise.

Various authors have introduced new sets of numbers into the original 'coincidence' considered by Dirac and his contemporaries, thus broadening or even departing from Dirac's own conclusions. Jordan (1947)^[14] noted that the mass ratio for a typical star and an electron approximates to 10⁶⁰, an interesting variation on the 10⁴⁰ and 10⁸⁰ that are typically associated with Dirac and Eddington respectively.

Several authors have recently identified and pondered the significance of yet another large number, approximately 120 orders of magnitude. This is for example the ratio of the theoretical and observational estimates of the energy density of the vacuum, which Nottale (1993)^[15] and Matthews (1997)^[16] associated in an LNH context with a scaling law for the cosmological constant. Carl Friedrich von Weizsäcker identified 10¹²⁰ with the ratio of the universe's volume to the volume of a typical nucleon bounded by its Compton wavelength, and he identified this ratio with the sum of elementary events or bits of information in the universe.^[17]

References

↑ H. Weyl (1917). "Zur Gravitationstheorie". Annalen der Physik. 359 (18): 117. Bibcode:1917AnP...359..117W. doi:10.1002/andp.19173591804.
↑ H. Weyl (1919). "Eine neue Erweiterung der Relativitätstheorie". Annalen der Physik. 364 (10): 101. Bibcode:1919AnP...364..101W. doi:10.1002/andp.19193641002.
↑ A. Eddington (1931). "Preliminary Note on the Masses of the Electron, the Proton, and the Universe". Proceedings of the Cambridge Philosophical Society. 27: 15. Bibcode:1931PCPS...27...15E. doi:10.1017/S0305004100009269.
↑ E. A. Milne (1935). Relativity, Gravity and World Structure. Oxford University Press.
↑ H. Kragh (1996). Cosmology and Controversy: The historical development of two theories of the universe. Princeton University Press. pp. 61–62. ISBN 978-0-691-02623-7.
↑ H. Kragh (1990). Dirac: A Scientific Biography. Cambridge University Press. p. 177. ISBN 978-0-521-38089-8.
↑ J. P.Uzan (2003). "The fundamental constants and their variation, Observational status and theoretical motivations". Reviews of Modern Physics. 75 (2): 403. arXiv:hep-ph/0205340. Bibcode:2003RvMP...75..403U. doi:10.1103/RevModPhys.75.403.
↑ E. Teller (1948). "On the change of physical constants". Physical Review. 73 (7): 801–802. Bibcode:1948PhRv...73..801T. doi:10.1103/PhysRev.73.801.
↑ G. Gamow (1962). Gravity. Doubleday. pp. 138–141. LCCN 62008840.
↑ G. Blake (1978). "The Large Numbers Hypothesis and the rotation of the Earth". Monthly Notices of the Royal Astronomical Society. 185: 399. Bibcode:1978MNRAS.185..399B. doi:10.1093/mnras/185.2.399.
↑ D. Falik (1979). "Primordial Nucleosynthesis and Dirac's Large Numbers Hypothesis". The Astrophysical Journal. 231: L1. Bibcode:1979ApJ...231L...1F. doi:10.1086/182993.
↑ V. Canuto, S. Hsieh (1978). "The 3 K blackbody radiation, Dirac's Large Numbers Hypothesis, and scale-covariant cosmology". The Astrophysical Journal. 224: 302. Bibcode:1978ApJ...224..302C. doi:10.1086/156378.
↑ V. Canuto, S. Hsieh (1980). "Primordial nucleosynthesis and Dirac's large numbers hypothesis". The Astrophysical Journal. 239: L91. Bibcode:1980ApJ...239L..91C. doi:10.1086/183299.
↑ P. Jordan (1947). Die Herkunft der Sterne. Wissenschaftliche Verlagsgesellschaft. Bibcode:1947dhds.book.....J. doi:10.1002/asna.19472751012.
↑ L. Nottale. "Mach's Principle, Dirac's Large Numbers and the Cosmological Constant Problem" (PDF).
↑ R. Matthews (1998). "Dirac's coincidences sixty years on" (PDF). Astronomy & Geophysics. 39 (6): 19–20. doi:10.1093/astrog/39.6.6.19.
↑ H. Lyre (2003). "C. F. Weizsäcker's Reconstruction of Physics: Yesterday, Today and Tomorrow". arXiv:quant-ph/0309183 [quant-ph].

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