LogoLogo
  • Bio
  • Fyzika
  • V médiích
  • Fotografie
  • Výstavy
  • Kontakt

    Mass estimate of the XTE J1650-500 black hole from the extended orbital resonance model for high-frequency QPOs

    Zdeněk Stuchlík · Prosinec 01, 2008 · Fyzika · 0 comments
    0

    Publication date: Dec 2008

    Abstract:
    Context: XTE J1650-500 is a Galactic black-hole binary system for which
    at least one high-frequency QPO at 250 Hz has been reported. Moreover
    there are indications that the system harbours a near-extreme Kerr black
    hole with a spin aast ≃ 0.998 and mass M_BH ≲ 7.3
    Msun. Recently it was discovered that the orbital 3-velocity
    of test-particle (geodesical) discs orbiting Kerr black holes with a
    spin aast > 0.9953, analyzed in the locally non-rotating
    frames, reveals a hump near the marginally stable orbit. It was
    suggested that the hump could excite the epicyclic motion of particles
    near the ISCO with frequencies typical for high-frequency QPOs. The
    characteristic frequency of the hump-induced oscillations was defined as
    the maximal positive rate of change of the LNRF-related orbital velocity
    with the proper radial distance. If the characteristic “humpy
    frequency” and the radial epicyclic frequency are commensurable,
    strong resonant phenomena are expected. Aims: We apply the idea
    of hump-induced oscillations in accretion discs around near-extreme Kerr
    black holes to estimate the black-hole mass in the XTE J1650-500 binary
    system. Methods: For the Kerr black hole with spin
    aast ≃ 0.9982 the characteristic “humpy
    frequency” and the radial epicyclic frequency are in the ratio 1:3
    at the orbit where the positive rate of change of the LNRF-related
    orbital velocity with the proper radial distance is maximal. Identifying
    the radial epicyclic frequency with the observed 250 Hz QPO, we arrive
    at the mass of the black hole. In this method the ratio of frequencies
    determines the spin (and vice versa), and the values of the frequencies
    determine the black-hole mass. Results: The mass of the Kerr
    black hole in XTE J1650-500 binary system is estimated to be around 5.1
    Msun.

    Authors:
    Slaný, P.; Stuchlík, Z.;

    http://adsabs.harvard.edu/abs/2008A%26A…492..319S

      Facebook   Pinterest   Twitter   Google+

    Leave a Comment! Zrušit odpověď na komentář

    You must be logged in to post a comment.
    Archivy
    Copyright © 2016 Zdeněk Stuchlík