| Subject: Does consciousness matter?
Date: Sat, 14 Jun 2003 02:47:30 +0300 From: Dimi Chakalov <dchakalov@surfeu.at> To: linde@physics.stanford.edu, alinde@stanford.edu CC: alstar@itp.ac.ru, guth@ctp.mit.edu, pdavies@els.mq.edu.au, stefan@gr.uchicago.edu, rmwa@midway.uchicago.edu, mukhanov@theorie.physik.uni-muenchen.de, suneeta@theorie.physik.uni-muenchen.de, unruh@physics.ubc.ca, don@phys.ualberta.ca, shinji@resceu.s.u-tokyo.ac.jp, brandenb@physics.ubc.ca, kallosh@stanford.edu RE: Inflation, Quantum Cosmology and the Anthropic Principle,
by Andrei Linde, 8 November 2002, hep-th/0211048.
To appear in: Science and Ultimate Reality: From Quantum to Cosmos, honoring
John Wheeler's 90th birthday. J.D. Barrow, P.C.W. Davies, & C.L. Harper
eds. Cambridge University Press (2003).
Andrei dorogoi, I hope my email of Tue, 09 Oct 2001 02:55:54 +0200 (printed below) has been received. In your article "Inflation, Quantum Cosmology and the Anthropic Principle", hep-th/0211048, Sec. 10, "Does consciousness matter?", you posed a tantalizing question: "Is it possible to introduce a 'space of elements of consciousness,' and investigate a possibility that consciousness may exist by itself, even in the absence of matter, just like gravitational waves, excitations of space, may exist in the absence of protons and electrons?" Why invent the wheel? The solution has been proposed by W. Pauli and C. Jung more than fifty years ago. Would you like some references? The story goes back to Leibnitz, http://plato.stanford.edu/entries/leibniz-mind/#2 Perhaps you didn't have the chance to read anything but Marx/Lenin/Stalin while living in USSR, but now I believe you are free to explore the library of Stanford University. But since you're a physicist, let me switch to your field of professional expertise: inflationary cosmology. As you stated at your web page at http://hbar.stanford.edu/linde , "I am one of the authors of the inflationary cosmology and of the theory of the cosmological phase transitions." You also wrote at your web page that "inflation remains the only robust mechanism that produces density perturbations with a flat spectrum and simultaneously solves all major cosmological problems." And in the above-mentioned article, hep-th/0211048, you wrote: "The only known way to explain why our universe is so large, flat, homogeneous and isotropic requires inflation." Do you know what is the topology of the universe? It seems to me that you have a problem with the "cosmic equator", http://members.aon.at/chakalov/Tegmark.html#note If you know the solution, please don't hesitate to publish it. Perhaps it would be a good idea if you consult Dr. Alexey Starobinsky who is also one of the authors of the inflationary cosmology. I'm afraid the hypothesis of inflation does not solve the major cosmological problems. They are very old and widely known, even in the USSR. See http://members.aon.at/chakalov/Shinji.html Besides, I can't see how some *physical clock*, as defined in GR, could possibly survive if you run it back to the inflation stage (if any). Please see http://members.aon.at/chakalov/Wald.html Once it enters the non-causal inflationary stage, the poor clock will inevitably crash, I'm afraid. Please correct me if I'm wrong. With math, if possible. I extend this request to all recipients of this email. I believe your insights will also address the problem of "how to approximately reconstruct a classical spacetime from nonlocal diffeomorphism-invariant observables", http://members.aon.at/chakalov/Suneeta.html#3 Regards, Dimi ==
Note: If you have an inflationary bubble, what can you do with it for 10-35 seconds? Quite a lot, according to Andrei Linde [Ref. 1]. All you have to do is to start from the Planckian density and Planck size, 10-33 cm [Ibid.], and then all inhomogeneities would be exponentially stretched during that 10-35 seconds, after which the universe would be almost exactly homogeneous on large scale, which is what you observe. Lucky you, because other bubbles would decide to jump back to the initial Plankian state, in line with the idea of "stationary equilibrium" [Ibid.]. Exactly how lucky are you? Infinitely lucky. There are infinitely many bubbles reserved for each of the possible inflation playscripts, but one and only one has led to the unique observable universe, sources say. Anyway, I don't know what was the reaction of the audience at the Nobel Symposium "Cosmology and String Theory" in August 2003, but I know that Andrei Linde did receive my email of Saturday, 14 June 2003 (cf. above), because he very politely asked me not to send him email, ever. Then he went on with his talk in August 2003, as if he didn't know that the chance of being 'infinitely lucky' is infinitely small. It is not 'one in a G' (a google, G, is defined to be ten to the power one hundred, G = 10100). It is not one in a G100 either. It is "exactly" 'one out of infinity'. So, I asked him to use math (cf. above). Well, I guess now you know why A. Linde asked me not to send him email, ever. Other people were less polite, or simply did not respond. That's the sole difference. All these people have studied Quantum Mechanics, only they don't care. Their pay check is secured, and they live in total socialism, just like Andrei Linde back in the USSR. Is it fun though?
D. Chakalov [Ref. 1] Andrei Linde, Prospects of Inflation, hep-th/0402051, 6 February 2004 Comments: 23 pages, extended version of the talk at the Nobel Symposium "Cosmology and String Theory," August 2003 "This was done with the invention
of the chaotic inflation scenario [9]. This scenario resolved all problems
of old and new inflation. According to this scenario, inflation may occur
even in the theories with simplest potentials such as [XXX]. Inflation
may begin even if there was no thermal equilibrium in the early universe,
and it may start even at the Planckian density, in which case the problem
of initial conditions for inflation can be easily resolved [4]. "In realistic versions of inflationary
theory the duration of inflation could be as short as
10-35 seconds.
"The main difference between inflationary theory and the old cosmology becomes clear when one calculates the size of a typical inflationary domain at the end of inflation. Investigation of this question shows that even if the initial size of inflationary universe was as small as the Planck size l_p 10-33 cm, after 10-35 seconds of inflation the universe acquires a huge size of l (1010)12 cm! This number is model-dependent, but in all realistic models the size of the universe after inflation appears to be many orders of magnitude greater than the size of the part of the universe which we can see now, l 1028 cm. This immediately solves most of the problems of the old cosmological theory [9, 4]. "Our universe is almost exactly homogeneous
on large scale because all inhomogeneities were exponentially stretched during
inflation. "The resulting picture resembles
eternal inflation in the old inflation scenario. However,
now we have an incredibly large
number of false vacuum states, plus some states which
may allow slow-roll inflation. Once
inflation begins, different parts of the universe start
wondering from one of these vacuum
states to another, so that the universe becomes divided into indefinitely
many regions with all possible laws of low-energy physics corresponding
to different 4d vacua of string theory [4].
"Moreover, as it was argued in [20], the probability (per unit time and unit volume) to jump back to the eternally inflating regime is always finite, even after the field enters the regime where, naively, one would not expect eternal inflation. Each bubble of a new phase which appears during the decay of the eternally inflating dS space is an open universe of an infinite volume. Therefore during the slow-roll inflation there always will be some inflationary domains jumping back to the original dS space, so some kind of stationary equilibrium will always exist between various parts of the inflationary universe. "Thus, the existence of many different dS vacua in string theory leads to the regime of eternal inflation. This regime may help us to solve the problem of initial conditions for the slow-roll inflation even in the models where the slow-roll inflation by itself is not eternal and would occur only on a small energy scale."
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