relativistic stellar clusters g.s.bisnovatyi-kogan (iki, moscow), ГАИШ, пятница, 21...
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Relativistic stellar clustersG.S.Bisnovatyi-Kogan (IKI, Moscow),
ГАИШ, пятница, 21 марта 2014
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Вскоре после открытия квазаров с большим красным смещением:
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=1 was considered by Zeldovich and Podurets (1965)
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Star Clusters with Cutoff
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Comments on Astrophysics 1, 134, 1969
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GR5: Tbilisi, 9-13 September 1968Proceedings: None.Abstracts: GR5, abstracts of the 5th international conference on gravitation and the theory of relativity, ed. V.A. Fock et al. Tbilisi University Press (1968).
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MODELS OF CLUSTERS OF POINT MASSES WITH LARGE CENTRAL REDSHIFTS
G. S. Bisnovatyi-Kogan and Ya. B. Zel'dovich
Astrofizika, Vot. 5, No. 2, pp. 223-234, 1969
=2/a
0.006
r(g)/r=const~a
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Isothermal star cluster in Newtonian limit
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Variational principle
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Relative binding energy E(b)/M is better for
stability analysis than M
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Publications:
Earlier publications
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Isolated cluster
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is the kinetic energy cutoff.
In the Newtonian limit, formally reduces to
Similarity between clusters in the box and clusters with cutoff
Newtonian cluster in box GR cluster with cutoff
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E(b)/N
W(0)=const, each extremum gives birth to new dynamically
unstable mode . At W(0)> 15.8 all models are stable.
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Dynamic stability against perturbations with constant adiabatic invariants.
Equivalent to constant entropy for stability of gaseous star
Thermodynamic stability include processes leading to thermal equilibrium, smoothing temperature over the newtonian
cluster or star
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Clusters with cutoff : ApJ (1998), 500, 217
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Large central density (central redshift) regime loss of dynamic stability at T=0.06
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DU T U
S S
DS TUDU T U
S S
DS TU
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Astro-ph 1403.3985
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Interpretation: GW from the inflation (Linde)
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A simplified model of the formation of structures in dark matterand a background of very long gravitational waves
G. S. Bisnovatyi-Kogan1,2
1Space Research Institute, Moscow, Russia, Profsoyuznaya 84/32, Moscow 117997, Russia
2Theoretical Astrophysics Center, Juliane Maries Vej 30, Dk-2100 Copenhagen Ø, Denmark
Mon. Not. R. Astron. Soc. 347, 163–172 (2004)
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