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On Black and White Holes

Published online by Cambridge University Press:  07 February 2017

M. A. Markov
M. A. Markov*
Affiliation:
Laboratory of Theoretical Physics, Joint Institute for Nuclear Research, Dubna, U.S.S.R.

Abstract

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Various possible cases of spherically systems the matter of which is localized in a domain smaller than the corresponding gravitational radius is considered.

The metic of the Friedmann closed world or of a part of it with an external continuation is suggested as a model of these systems.

There can exist black holes which are described by semi-closed metrics (black holes of the second kind). The class of systems in question may be both in the state of collapse and in the state of anti-collapse (including the state of ‘white holes’).

There are some grounds to suppose that collapse of celestial bodies should stop in the domain h/mvc, where mv is the mass of the vector meson, and that the pair production effect due to collapse of a charged sphere should conserve the Laplace determinism of the process.

The role of the charges of sources of different fields (electromagnetic, meson vector, scalar long-range, scalar meson, various versions of neutrino fields) in the deformation of the external and internal metric of black and white holes is analysed.

In this consideration a number of problems arises (the absence of horizon in the case of any small charges of scalar fields, the presence of the generalized Gauss theorem for vector meson field etc.), which provide evidence that the assertion ‘Black hole has no hair’ needs further investigations. In particular, the inverse process of formation of hair (e.g. vector-meson, scalar fields) in the process of anti-collopose has not been studied yet.

For the limiting case of the Nordström-Reissner metric m = e (more correctly m → e) two essentially different possibilities of continuing to the internal metric are considered (the Papapetrou case and the case which we called ‘friedmon metric’ describing charged black holes of the second kind (friedmons)).

In the case of charged holes of the second kind (friedmons) the occurance of quantum effects (pair productions) can reduce the horizon surface and violate the Hawking theorem.

The notion of black holes may turn out to be essential in elementary particle theory: among the intermediate states in elementary particle theory there are states the characteristic feature of which is the localization of arbitrary large energies (masses) in a domain smaller than the gravitational radius.

Type
Part II: Stability and Collapse
Information
Symposium - International Astronomical Union , Volume 64: Gravitational Radiation and Gravitational Collapse , 1974 , pp. 106 - 131
Copyright
Copyright © Reidel 1974 

References

Ambartsumian, V. A.: 1962, Voprosy Kosmologii 8, 3.Google Scholar
Arnowitt, R., Deser, S., and Misner, C.: 1960, Phys. Rev. 120, 313.Google Scholar
Asanov, R.: 1972, preprint P2–6564, Dubna.Google Scholar
Asanov, R.: 1973, preprint P2–7230, Dubna.Google Scholar
Bardeen, J. M.: 1968, Bull. Am. Phys. Soc. 13, 41.Google Scholar
Bekenstein, J.: 1972, Phys. Rev. Letters 18, 452.Google Scholar
Bekenstein, J.: 1973, Phys. Rev. D7, 949.Google Scholar
Berezin, V.A. and Markov, M. A.: 1970, Teor. Mat. Fiz. 3, 161.Google Scholar
Blokhintsev, D.I.: 1960, Nuovo Cimento 16, 382.Google Scholar
Carter, B.: 1966, Phys. Letters 21, 423.Google Scholar
Chase, J.: 1972, Commun. Math. Phys. 19, 276.Google Scholar
Chernikov, N.A. and Tagirov, E. A.: 1968, Ann. Inst. Poincaré 9, 1507.Google Scholar
De la Cruz, and Israel, : 1967, Nature 216, 148, 312.Google Scholar
Dicke, R.: 1964, in Chiu, Hong-Yee and Hoffmann, W. (eds.), Gravitation and Relativity, W. A. Benjamin Inc., New-York-Amsterdam.Google Scholar
Fischer, I.: 1948, JETP 18, 636.Google Scholar
Frolov, V. P.: 1973, preprint Lebedev Inst., Moskow.Google Scholar
Hartle, J.: 1971a, Phys. Rev. D3, 2938.Google Scholar
Hartle, J.: 1971b, preprint.Google Scholar
Hawking, S. W.: 1970, Monthly Notices Roy. Astron. Soc. 152, 75.Google Scholar
Hawking, S. W.: 1971, Phys. Rev. Letters 26, 1344.Google Scholar
Hoyle, F., Fowler, W. A., Burbridge, G. R., and Burbridge, E. M.: 1965, Quasi-Stellar Sources and Gravitational Collapse, University of Chicago Press.Google Scholar
Israel, W.: 1966, Nuovo Cimento 44B, 1.CrossRefGoogle Scholar
Israel, W.: 1967, Nuovo Cimento 48B, 463.Google Scholar
Janis, A. I., Newmann, E. T., and Winicour, J.: 1968, Phys. Rev. 176, 1507.Google Scholar
Klein, O.: 1961, Werner Heisenberg und die Physik Unserer Zeit, Braunschweig.Google Scholar
Markov, M. A.: 1966, JETP 51, 878.Google Scholar
Markov, M. A.: 1970, Ann. Phys. 59, 109.CrossRefGoogle Scholar
Markov, M. A.: 1971, Cosmology and Elementary Particles (Lecture Notes), Trieste IC/71/33 Part I and II.Google Scholar
Markov, M. A.: 1972, preprint E2–6831, Dubna.Google Scholar
Markov, M. A. and Frolov, V. P.: 1970, Teor. Mat Fiz. 3, N1, 3.Google Scholar
Markov, M. A. and Frolov, V. P.: 1972, Teor. Mat. Fiz. 13, 41.Google Scholar
Markov, M. A. and Frolov, V. P.: 1973, Teor. Mat. Fiz. Google Scholar
Ne'eman, Y.: 1965, Appl. J. 141, 1303.Google Scholar
Novikov, I. D.: 1962, Vestn. Mosk. Gos. Univ. Ser. 3, N5.Google Scholar
Novikov, I. D.: 1964, Astron. J. 41, 1975.Google Scholar
Novikov, I. D.: 1966, Pisma JETP 3, 223.Google Scholar
Novikov, I. D.: 1970, JETP 59, 262 Google Scholar
Papapetrou, A.: 1945, Proc. Roy. Phys. Acad. L1, Sec.A., 191.Google Scholar
Penrose, R.: 1968, Structure of Space-Time, W. A. Benjamin inc., New-York-Amsterdam.Google Scholar
Regge, T.: 1958, Nuovo Cimento 7, 215.Google Scholar
Regge, T. and Wheeler, J. A.: 1957, Phys. Rev. 108, 1963.Google Scholar
Sakharov, : 1970, preprint N7, Inst. Prikladnoy Mat. AC.N.C.C.C.R.Google Scholar
Tamm, I.: 1934, Nature 134, 1010.Google Scholar
Teitelboim, C.: 1972, Lettere al. Nuovo Cimento 3, 326, 397.Google Scholar
Thorne, K.: 1971, preprint OAP-236.Google Scholar
Vaidya, P. C.: 1951, Phys. Rev. 83, 10.Google Scholar
Vaidya, P. C.: 1953, Nature 171, 260.Google Scholar
Wheeler, J. A.: 1971,Google Scholar
Weinberg, S.: 1967, Phys. Rev. Letters 19, 1264.Google Scholar
Zel'dovich, Ya. B.: 1962a, Zh. Exp. Teor. Fiz. 42, 641.Google Scholar
Zel'dovich, Ya. B.: 1962b, Zh. Exp. Teor. Fiz. 43, 1937.Google Scholar
Zel'dovich, Ya. B.: 1971, preprint N1, Institute of Applied Mathematics of the Acad. Nauk of the U.S.S.R. Google Scholar