Dr Stephan Rosswog
Professor of Astrophysics

Jacobs University Bremen
Campus Ring 1
D-28759 Bremen
Germany

Tel: +49 421 200-3226
Fax: +49 421 200-3229
email: s.rosswog@jacobs-university.de
URL: http://www.faculty.iu-bremen.de/srosswog




Movies



Merging Neutron Stars

  • Two neutron stars in corotation; equation of state: extended Shen et al.; shown is temperature;
    initial frame: ca. 100 km x 100 km;
    (visualisation: R. West)
    avi-format for linux
    avi-format for windows
  • Same as above, but cut through the orbital plane;
    initial frame: ca. 100 km x 100 km;
    (visualisation: R. West)
    avi-format for linux
    avi-format for windows
  • corotating binary system; density in the orbital plane; only highest densities (>10**13.5 g/ccm) shown;
    fixed frame: 50 km x 50 km;

    mpeg: use "mpeg_play -dither color";
    (if you are using Netscape: set in "preferences" the mpeg video command to:

    "mpeg_play -dither color %s")
  • corotating binary system; column density in the orbital plane

    mpeg: use "mpeg_play -dither color";
    (if you are using Netscape: set in "preferences" the mpeg video command to:

    "mpeg_play -dither color %s")




    • Relativistic Jet

  • temperature evolution in a 2D relativistic jet; simulation performed with relativistic PPM-code (PLUTO; written by A. Mignone)

    • (click on figure for movie)




    Neutron star black hole encounter

    Coalescences of Black Hole Neutron Star binaries are thought to be prime candidates for the long-searched central engines of short Gamma-ray Bursts. They are expected to be among the first sources of gravitational waves detected by ground-based detectors. Moreover, their very neutron-rich ejecta may produce some of the heaviest nuclei in the universe.

    Input physics
  • gravity: Paczynski-Wiita potential for Black Hole, Newtonian self-gravity plus back reaction forces
  • equation of state: temperature and composition dependent relativistic mean field equation of state (Shen et al. 1998)
  • opacity-dependent multi-flavour neutrino cooling included
  • Hydrodynamics: smoothed particle hydrodynamics (SPH)





    • Black Hole 14, neutron star 1.4 solar masses (q=0.1)
  • tidal locking, 3 000 000 SPH-particles


    • small (21 Mb), AVI-format large (100 Mb), AVI-format very large (130 Mb), AVI-format




    Black Hole 18, neutron star 1.4 solar masses (q=0.07778)
  • tidal locking, 500 000 SPH-particles

    • large (100 Mb), AVI-format