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Relativistic stellar clusters G.S.Bisnovatyi-Kogan (IKI, Moscow), ГАИШ, пятница, 21 марта 2014.

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Presentation on theme: "Relativistic stellar clusters G.S.Bisnovatyi-Kogan (IKI, Moscow), ГАИШ, пятница, 21 марта 2014."— Presentation transcript:

1 Relativistic stellar clusters G.S.Bisnovatyi-Kogan (IKI, Moscow), ГАИШ, пятница, 21 марта 2014

2 Вскоре после открытия квазаров с большим красным смещением:

3 =1 was considered by Zeldovich and Podurets (1965)

4 Star Clusters with Cutoff

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8 Comments on Astrophysics 1, 134, 1969

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10 GR5: Tbilisi, 9-13 September 1968 Proceedings: 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).

11 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 , 1969 =2/a r(g)/r=const~a

12 Isothermal star cluster in Newtonian limit

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14 Variational principle

15 Relative binding energy E(b)/M is better for stability analysis than M

16 Publications: Earlier publications

17 Isolated cluster

18 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

19 E(b)/N W(0)=const, each extremum gives birth to new dynamically unstable mode. At W(0)> 15.8 all models are stable.

20 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

21 Clusters with cutoff : ApJ (1998), 500, 217

22 Large central density (central redshift) regime loss of dynamic stability at T=0.06

23 DU T U S DS TU DU T U S DS TU

24 Astro-ph

25 Interpretation: GW from the inflation (Linde)

26 A simplified model of the formation of structures in dark matter and a background of very long gravitational waves G. S. Bisnovatyi-Kogan1,2 1Space Research Institute, Moscow, Russia, Profsoyuznaya 84/32, Moscow , 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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