1 / 28

R elativistic stellar clusters G. S. Bisnovatyi-Kogan (IKI, Moscow) ,

R elativistic stellar clusters G. S. Bisnovatyi-Kogan (IKI, Moscow) ,. ГАИШ, пятница, 21 марта 2014. Вскоре после открытия квазаров с большим красным смещением :. =1 was considered by Zeldovich and Podurets (1965). Star Clusters with Cutoff. Comments on Astrophysics 1, 134, 1969.

aquila-erickson
Download Presentation

R elativistic stellar clusters G. S. Bisnovatyi-Kogan (IKI, Moscow) ,

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

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

  5. Comments on Astrophysics 1, 134, 1969

  6. 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).

  7. 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

  8. Isothermal star cluster in Newtonian limit

  9. Variational principle

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

  11. Publications: Earlier publications

  12. Isolated cluster

  13. Newtonian cluster in box GR cluster with cutoff is thekinetic energy cutoff. In the Newtonian limit, formally reduces to Similarity between clusters in the box and clusters with cutoff

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

  15. 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

  16. Clusters with cutoff : ApJ (1998), 500, 217

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

  18. DSTU DSTU DU T U DU T U S S S S

  19. Astro-ph 1403.3985

  20. Interpretation: GW from the inflation (Linde)

  21. 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 117997, Russia 2Theoretical Astrophysics Center, Juliane Maries Vej 30, Dk-2100 Copenhagen Ø, Denmark Mon. Not. R. Astron. Soc. 347, 163–172 (2004)

More Related