# Olbers' paradox

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Olbers' paradox in action

In astrophysics and physical cosmology, Olbers' paradox, named after the German astronomer Heinrich Wilhelm Olbers (1758–1840) and also called the "dark night sky paradox", is the argument that the darkness of the night sky conflicts with the assumption of an infinite and eternal static universe. The darkness of the night sky is one of the pieces of evidence for a dynamic universe, such as the Big Bang model. If the universe is static, homogeneous at a large scale, and populated by an infinite number of stars, any sight line from Earth must end at the (very bright) surface of a star, so the night sky should be completely bright. This contradicts the observed darkness of the night.[1]

## History

Edward Robert Harrison's Darkness at Night: A Riddle of the Universe (1987) gives an account of the dark night sky paradox, seen as a problem in the history of science. According to Harrison, the first to conceive of anything like the paradox was Thomas Digges, who was also the first to expound the Copernican system in English and also postulated an infinite universe with infinitely many stars.[2] Kepler also posed the problem in 1610, and the paradox took its mature form in the 18th century work of Halley and Cheseaux.[3] The paradox is commonly attributed to the German amateur astronomer Heinrich Wilhelm Olbers, who described it in 1823, but Harrison shows convincingly that Olbers was far from the first to pose the problem, nor was his thinking about it particularly valuable. Harrison argues that the first to set out a satisfactory resolution of the paradox was Lord Kelvin, in a little known 1901 paper,[4] and that Edgar Allan Poe's essay Eureka (1848) curiously anticipated some qualitative aspects of Kelvin's argument:[1]

Were the succession of stars endless, then the background of the sky would present us a uniform luminosity, like that displayed by the Galaxy – since there could be absolutely no point, in all that background, at which would not exist a star. The only mode, therefore, in which, under such a state of affairs, we could comprehend the voids which our telescopes find in innumerable directions, would be by supposing the distance of the invisible background so immense that no ray from it has yet been able to reach us at all.[5]

## The paradox

What if every line of sight ended in a star? (Infinite universe assumption#2)

The paradox is that a static, infinitely old universe with an infinite number of stars distributed in an infinitely large space would be bright rather than dark.[1]

To show this, we divide the universe into a series of concentric shells, 1 light year thick. A certain number of stars will be in the shell 1,000,000,000 to 1,000,000,001 light years away. If the universe is homogeneous at a large scale, then there would be four times as many stars in a second shell, which is between 2,000,000,000 and 2,000,000,001 light years away. However, the second shell is twice as far away, so each star in it would appear one quarter as bright as the stars in the first shell. Thus the total light received from the second shell is the same as the total light received from the first shell.

Thus each shell of a given thickness will produce the same net amount of light regardless of how far away it is. That is, the light of each shell adds to the total amount. Thus the more shells, the more light; and with infinitely many shells, there would be a bright night sky.

While dark clouds could obstruct the light, these clouds would heat up, until they were as hot as the stars, and then radiate the same amount of light.

Kepler saw this as an argument for a finite observable universe, or at least for a finite number of stars. In general relativity theory, it is still possible for the paradox to hold in a finite universe:[6] though the sky would not be infinitely bright, every point in the sky would still be like the surface of a star.

## The mainstream explanation

The poet Edgar Allan Poe suggested that the finite size of the observable universe resolves the apparent paradox.[7] More specifically, because the universe is finitely old and the speed of light is finite, only finitely many stars can be observed within a given volume of space visible from Earth (although the whole universe can be infinite in space).[8] The density of stars within this finite volume is sufficiently low that any line of sight from Earth is unlikely to reach a star.

However, the Big Bang theory introduces a new paradox: it states that the sky was much brighter in the past, especially at the end of the recombination era, when it first became transparent. All points of the local sky at that era were comparable in brightness to the surface of the Sun, due to the high temperature of the universe in that era; and most light rays will terminate not in a star but in the relic of the Big Bang.

This paradox is explained by the fact that the Big Bang theory also involves the expansion of space, which can cause the energy of emitted light to be reduced via redshift. More specifically, the extreme levels of radiation from the Big Bang have been redshifted to microwave wavelengths (1100 times the length of its original wavelength) as a result of the cosmic expansion, and thus forms the cosmic microwave background radiation. This explains the relatively low light densities present in most of our sky despite the assumed bright nature of the Big Bang. The redshift also affects light from distant stars and quasars, but the diminution is minor, since the most distant galaxies and quasars have redshifts of only around 5 to 8.6.

## Alternative explanations

### Steady state

The redshift hypothesised in the Big Bang model would by itself explain the darkness of the night sky even if the Universe were infinitely old. The steady state cosmological model assumed that the Universe is infinitely old and uniform in time as well as space. There is no Big Bang in this model, but there are stars and quasars at arbitrarily great distances. The expansion of the Universe causes the light from these distant stars and quasars to redshift (by the Doppler effect and thermalisation[9]), so that the total light flux from the sky remains finite. Thus the observed radiation density (the sky brightness of extragalactic background light) can be independent of finiteness of the Universe. Mathematically, the total electromagnetic energy density (radiation energy density) in thermodynamic equilibrium from Planck's law is

${\displaystyle {U \over V}={\frac {8\pi ^{5}(kT)^{4}}{15(hc)^{3}}},}$

e.g. for temperature 2.7 K it is 40 fJ/m3 ... 4.5×10−31 kg/m3 and for visible temperature 6000 K we get 1 J/m3 ... 1.1×10−17 kg/m3. But the total radiation emitted by a star (or other cosmic object) is at most equal to the total nuclear binding energy of isotopes in the star. For the density of the observable universe of about 4.6×10−28 kg/m3 and given the known abundance of the chemical elements, the corresponding maximal radiation energy density of 9.2×10−31 kg/m3, i.e. temperature 3.2 K (matching the value observed for the optical radiation temperature by Arthur Eddington[10][11]). This is close to the summed energy density of the cosmic microwave background and the cosmic neutrino background. The Big Bang hypothesis predicts that the CBR should have the same energy density as the binding energy density of the primordial helium, which is much greater than the binding energy density of the non-primordial elements; so it gives almost the same result. However, the steady-state model does not predict the angular distribution of the microwave background temperature accurately.[12]

### Finite age of stars

Stars have a finite age and a finite power, thereby implying that each star has a finite impact on a sky's light field density. Edgar Allan Poe suggested that this idea could provide a resolution to Olbers' paradox; a related theory was also proposed by Jean-Philippe de Chéseaux. However, stars are continually being born as well as dying. As long as the density of stars throughout the universe remains constant, regardless of whether the universe itself has a finite or infinite age, there would be infinitely many other stars in the same angular direction, with an infinite total impact. So the finite age of the stars does not explain the paradox.[13]

### Brightness

Suppose that the universe were not expanding, and always had the same stellar density; then the temperature of the universe would continually increase as the stars put out more radiation. Eventually, it would reach 3000 K (corresponding to a typical photon energy of 0.3 eV and so a frequency of 7.5×1013 Hz), and the photons would begin to be absorbed by the hydrogen plasma filling most of the universe, rendering outer space opaque. This maximal radiation density corresponds to about 1.2×1017 eV/m3 = 2.1×10−19 kg/m3, which is much greater than the observed value of 4.7×10−31 kg/m3.[3] So the sky is about fifty billion times darker than it would be if the universe was neither expanding nor too young to have reached equilibrium yet.

### Fractal star distribution

A different resolution, which does not rely on the Big Bang theory, was first proposed by Carl Charlier in 1908 and later rediscovered by Benoît Mandelbrot in 1974. They both postulated that if the stars in the universe were distributed in a hierarchical fractal cosmology (e.g., similar to Cantor dust)—the average density of any region diminishes as the region considered increases—it would not be necessary to rely on the Big Bang theory to explain Olbers' paradox. This model would not rule out a Big Bang, but would allow for a dark sky even if the Big Bang had not occurred.

Mathematically, the light received from stars as a function of star distance in a hypothetical fractal cosmos is:

${\displaystyle {\text{light}}=\int _{r_{0}}^{\infty }L(r)N(r)\,dr}$

where:

r0 = the distance of the nearest star. r0 > 0;

r = the variable measuring distance from the Earth;

L(r) = average luminosity per star at distance r;

N(r) = number of stars at distance r.

The function of luminosity from a given distance L(r)N(r) determines whether the light received is finite or infinite. For any luminosity from a given distance L(r)N(r) proportional to ra, ${\displaystyle {\text{light}}}$ is infinite for a ≥ −1 but finite for a < −1. So if L(r) is proportional to r−2, then for ${\displaystyle {\text{light}}}$ to be finite, N(r) must be proportional to rb, where b < 1. For b = 1, the numbers of stars at a given radius is proportional to that radius. When integrated over the radius, this implies that for b = 1, the total number of stars is proportional to r2. This would correspond to a fractal dimension of 2. Thus the fractal dimension of the universe would need to be less than 2 for this explanation to work.

This explanation is not widely accepted among cosmologists since the evidence suggests that the fractal dimension of the universe is at least 2.[14][15][16] Moreover, the majority of cosmologists accept the cosmological principle,[citation needed] which assumes that matter at the scale of billions of light years is distributed isotropically. Contrarily, fractal cosmology requires anisotropic matter distribution at the largest scales; interestingly, cosmic microwave background radiation has cosine anisotropy.[17]

## References

1. ^ a b c Overbye, Dennis (August 3, 2015). "The Flip Side of Optimism About Life on Other Planets". New York Times. Retrieved October 29, 2015.
2. ^ Hellyer, Marcus, ed. (2008). The Scientific Revolution: The Essential Readings. Blackwell Essential Readings in History. 7. John Wiley & Sons. p. 63. ISBN 9780470754771. The Puritan Thomas Digges (1546–1595?) was the earliest Englishman to offer a defense of the Copernican theory. ... Accompanying Digges's account is a diagram of the universe portraying the heliocentric system surrounded by the orb of fixed stars, described by Digges as infinitely extended in all dimensions.
3. ^ a b Unsöld, Albrecht; Baschek, Bodo (2001). The New Cosmos: An Introduction to Astronomy and Astrophysics. Physics and astronomy online. Springer. p. 485. ISBN 9783540678779. The simple observation that the night sky is dark allows far-reaching conclusions to be drawn about the large-scale structure of the universe. This was already realized by J. Kepler (1610), E. Halley (1720), J.-P. Loy de Chesaux (1744), and H. W. M. Olbers (1826).
4. ^ For a key extract from this paper, see Harrison (1987), pp. 227–28.
5. ^ Poe, Edgar Allan (1848). "Eureka: A Prose Poem".
6. ^ D'Inverno, Ray. Introducing Einstein's Relativity, Oxford, 1992.
7. ^ "Poe: Eureka". Xroads.virginia.edu. Retrieved 2013-05-09.
8. ^ http://www.cfa.harvard.edu/seuforum/faq.htm - Brief Answers to Cosmic Questions
9. ^ http://physicsessays.org/doi/abs/10.4006/1.3028952?journalCode=phes - Gilles Corriveau: The 3 K Background Emission, the Formation of Galaxies, and the Large‐Scale Structure of the Universe
10. ^ Wright, Edward L. (23 Oct 2006). "Eddington's Temperature of Space". Retrieved 10 July 2013.
11. ^ Eddington, A.S. (1926). Eddington's 3.18°K "Temperature of Interstellar Space". The Internal Constitution of the Stars. Cambridge University Press. pp. 371–372. Retrieved 10 July 2013.
12. ^ Wright, E. L., E. L. "Errors in the Steady State and Quasi-SS Models". UCLA, Physics and Astronomy Department. Retrieved 2015-05-28.
13. ^ Kidger, Mark (2008), "The Mortality of the Stars", Cosmological Enigmas: Pulsars, Quasars, and Other Deep-Space Questions, JHU Press, pp. 144–145, ISBN 9780801893353.
14. ^ Joyce, M.; Labini, F.S.; Gabrielli, A.; Montouri, M.; et al. (2005). "Basic Properties of Galaxy Clustering in the light of recent results from the Sloan Digital Sky Survey". Astronomy and Astrophysics. 443 (11): 11–16. arXiv:astro-ph/0501583. Bibcode:2005A&A...443...11J. doi:10.1051/0004-6361:20053658.
15. ^ Labini, F.S.; Vasilyev, N.L.; Pietronero, L.; Baryshev, Y. (2009). "Absence of self-averaging and of homogeneity in the large scale galaxy distribution". Europhys.Lett. 86 (4): 49001. arXiv:0805.1132. Bibcode:2009EL.....8649001S. doi:10.1209/0295-5075/86/49001.
16. ^ Hogg, David W.; Eisenstein, Daniel J.; Blanton, Michael R.; Bahcall, Neta A.; et al. (2005). "Cosmic homogeneity demonstrated with luminous red galaxies". The Astrophysical Journal. 624: 54–58. arXiv:astro-ph/0411197. Bibcode:2005ApJ...624...54H. doi:10.1086/429084.
17. ^ Smoot G. F., Gorenstein M. V., and Muller R. A. (5 October 1977). "Detection of Anisotropy in the Cosmic Blackbody Radiation" (PDF). Lawrence Berkeley Laboratory and Space Sciences Laboratory, University of California, Berkeley. Retrieved 15 September 2013.

## Further reading

• Edward Robert Harrison (1987) Darkness at Night: A Riddle of the Universe, Harvard University Press. Very readable.
• -------- (2000) Cosmology, 2nd ed. Cambridge Univ. Press. Chpt. 24.
• Taylor Mattie, Fundamentals of Heat Transfer. MAHS
• Wesson, Paul (1991). "Olbers' paradox and the spectral intensity of the extragalactic background light". The Astrophysical Journal. 367: 399–406. Bibcode:1991ApJ...367..399W. doi:10.1086/169638.