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Why can't cosmology be more open?

Big bang. Many believe it is the last word in cosmic sciences. Self-confessed agnostic Jayant Vishnu Narlikar reviews the weaknesses of the model to suggest that scientists might just be fooling themselves with the "Emperor's New Clothes". He challenges many holy cows of cosmology here.

Jayant Vishnu Narlikar

doi:10.1038/nindia.2007.54 Published online 16 January 2008

Jayant V Narlikar

© IUCAA

"Cosmologists are always wrong but never in doubt," said Lev Landau, the distinguished physicist and Nobel laureate. Ideally, a cosmologist strives to know how far the universe extends, when it was born (if ever there was an instant when it was created) and what will happen to it in future. This desire to know is not new: many thinkers across cultures and millennia have conjectured and claimed to know the answers. Old literature contains a wealth of speculation replete with the imaginativeness of writers.

More than two millennia back, Pythagoreans believed that the Earth went round a central fire, with the Sun lying well outside its orbit. When sceptics asked," Why can't we see the fire?", theorists had to postulate that there was a 'counter-Earth' going around the central fire in an inner orbit that blocked our view of the fire. The sceptics asked again: why don't we see this 'counter-Earth'? The theorists replied that since Greece was facing away from it. In due course this explanation too was also shot down by people sailing around and looking from other directions.

I have painstakingly elaborated this ancient episode because it holds a moral for scientists. When you are on the wrong track, you may have to invoke additional assumptions, like the counter-Earth, to prop up your original theory against an observed fact. If there is no other independent support for these assumptions, the entire structure becomes suspect. The scientific approach then requires a critical re-examination of the basic paradigm.

Begin at the beginning

The first ambitious programme to scientifically model the universe began early last century. By mid-1920s astronomers had begun to appreciate the fact that our Milky Way Galaxy has more than a hundred billion stars and that the universe observed through the best available telescopes has many such galaxies. The challenge was how to describe the vast universe extending up to and beyond distances of millions of light years. A daring attempt to mathematically model this large system was made by Albert Einstein through his 1917 paper1. He believed that the universe is static with its major components at rest. In order to arrive at this, he had to modify his equations of general relativity to include a cosmic force of repulsion. However, Alexander Friedmann2 during 1922-24 and Abbe Lemaitre3 in 1927 independently arrived at models of the expanding universe using Einstein's equations.

Now, is the universe static or expanding?

A major observational advance resolved this question when Edwin Hubble4, used the then largest telescope (2.5 metre) from Mount Wilson in California, to find that almost all galaxies observed seemed to be receding from the Milky Way in a systematic fashion. In short, the universe was not static; it seemed to expand exactly as suggested by the models of Friedmann and Lemaitre.

These models have since provided the basic framework for cosmology as studied today. The expansion results in all galaxies moving away from one another with speeds increasing in proportion to the distances between them.

Then what's the bang all about?

Given the success of the expanding universe picture, scientists followed it further to suggest that the universe had a beginning in a gigantic explosion. This explosion was concentrated within a very small volume, literally a point, and the expansion was the aftermath of this primordial event. That event is popularly known as the big bang. The laws of science so far understood were then applied to this system. This exercise has met mixed success.

Cosmologists are speculating about the state of the universe that's unobservable and to which no tested physics can be applied

As first argued by nuclear astrophysicist George Gamow5 in the 1940s, the closer we probe the universe to the big bang, the hotter and denser we find it. This led Gamow to propose that during the period around 1-200 seconds after the big bang, the universe was hot enough to serve as a nuclear fusion reactor. Gamow hoped to show that most chemical elements we see today were synthesized in that period as neutrons and protons came together.

This, however, did not happen. Constraints of nuclear physics and the rapidly changing conditions of the expanding universe allow only some light nuclei like deuterium, helium and lithium to form6. That too is possible only if the neutrons and protons satisfy certain physical conditions.

Even so, the abundance of light nuclei in the universe is consistent with these theoretical estimates. Moreover, as Gamow's younger colleagues Ralph Alpher and Robert Herman7 predicted, the hot radiation then present would leave behind a relic background, albeit very cool today owing to the continued expansion of the universe. This 1948 prediction was borne out in 1965 by the discovery of the microwave background by Arno Penzias and Robert Wilson8. This background has been extensively studied and it shows (as predicted) a black body spectrum with a temperature of 2.73 Kelvin. In hindsight, however, one can say that this background had been observed as early as 1941 by McKellar9 through stellar spectroscopy.

Thus by the late 1960s most cosmologists were convinced that the big bang model is basically a correct description of the universe. Most work in cosmology in the last three decades has centred on establishing this belief as fact. To this end cosmologists have concentrated their efforts in many 'problem areas', building on Gamow's pioneering work. These problem areas include an understanding of the large scale structure observed in the universe, the early physical processes that left their imprints on the microwave background, the origin of subatomic particles, knowing why the universe today is dominated by matter over antimatter, knowing why it is so homogeneous and isotropic and above all trying to assess the physical conditions in the very early stages when many physicists believe the basic forces of nature acted in a unified framework10.

From facts to speculation

This ambitious agenda presented a challenge to the best intellects available today. Theoretically, a unified framework for physics lies in the realm of speculation. For, the particle energies (1000 GeV) produced by the best man-made accelerators today fall well short of the high energies (1016 GeV) needed to test such theories. Direct astronomical observations of the distant universe go back to epochs when the linear size of the (expanding) universe was about a tenth of the present size.

Have more mundane and familiar options to arrive at results been really exhausted?

Theory tells us that even if we had far more efficient telescopes, we would hit against an optically opaque wall erected by the radiation background at past epochs when the universe was smaller than a thousandth of its present size. The current theories about the very early universe take us back to epochs when the universe was 10-28 of its present linear size! In short, cosmologists are speculating about the state of the universe that is not only astronomically unobservable, but to which no tested physics can be applied. One may still indulge in a study of the very early universe, as an intellectual feat. Provided one is conscious that it is highly speculative.

Unfortunately, by describing the present model of the universe as a 'precision' or 'concordance' model11 an impression is created that the model with its various parameters is the last word in the subject. Let us take one example. The concordance model describes the break up of matter-energy content of the universe as 4% ordinary (baryonic) matter that is familiar to us, 23% non-baryonic dark matter and 73% dark energy. All astronomy to date has grown on observations of the baryonic part: there is no direct evidence for the remaining 96%. Certainly there is good astronomical evidence for dark matter; but if it were taken to be all baryonic, then the big bang model has two problems.

It cannot explain the observed deuterium in the universe and the microwave background would show far stronger inhomogeneities than actually observed. So to sustain the model one is forced to postulate non-baryonic dark matter for which there is no independent evidence either in astronomy or in the physics labs. Is this not a modern example of the Pythagorean counter-Earth?

Likewise, for dark energy there is no independent evidence. It was invoked as a solution for understanding why distant supernovae look dimmer than expected. Have other, more mundane and familiar options, to arrive at the results been really exhausted? Or, are theoreticians indulging in an exercise reminiscent of Hans Andersen's satire 'The Emperor's new clothes'?

In the Vatican Conference held in the late 1960s, Fred Hoyle12, the most imaginative astrophysicist of the twentieth century, wondered if the human brain was capable of understanding all the intricacies of physics and even if it was, whether that stage had been reached in the decade ending in 1970. He made this cautionary comment, because the big bang cosmologists at the conference were making very definitive claims about what the universe is like.

In retrospect, Hoyle's caution seems justified, since the so called last word on cosmology of the 1960s was innocent of non-baryonic dark matter, dark energy, inflation, and all the rest of paraphernalia that go to make up the present 'last word' on cosmology.

The author is an eminent astrophysicist and Emeritus Professor at the Inter-University Centre for Astronomy and Astrophysics, Pune, India.


References

  1. Einstein, A., Koniglich Preussische Akademie der WissenschaftenKoniglich Preussische Akademie der Wissenschaften, 1917
  2. Friedmann, A., Zeitschrift für Physik 10,377, 1922  | Article |
  3. Lemaitre, Abbe G., Annales de la Société Scientifique de Bruxelles, A47, 49, 1927
  4. Hubble, E.P., Proc. National Academy of Science (USA), 15, 16, 1929
  5. Alpher, R.A., Bethe, H. & Gamow, G., Physical Review, 73, 803, 1948 | Article | ISI |
  6. Wagoner, R.V., Fowler, W.A. & Hoyle, F., Astrophysical Journal, 148, 3, 1967 | Article |
  7. Alpher, R.A. & Herman, R.C., Nature, 162, 774, 1948 | Article |
  8. Penzias, A.A. & Wilson, R.W., Astrophysical Journal, 142, 419, 1965  | Article |
  9. McKellar, A., Dominion Astrophysics Observatory Journal, Victoria, British Columbia, VII, 251, 1941
  10. Narlikar, J.V., An Introduction to Cosmology, Cambridge University Press, 2002
  11. Spergel, D.N. et al, Astrophysical Journal Supp., 148, 175, 2003 | Article |
  12. Hoyle, F., Study Week on nNuclei of Galaxies,, 757 1970