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Confronting the models of 3:2 quasiperiodic oscillations with the rapid spin of the microquasar GRS 1915+105

Result description

Spectral fitting of the spin a = cJ/GM(2) in the microquasar GRS 1915+105 estimate values higher than a = 0.98. However, there are certain doubts about this (nearly) extremal number. Confirming a high value of a > 0.9 would have significant concequencesfor the theory of high-frequency quasiperiodic oscillations (HF QPOs). Here we discuss its possible implications assuming several commonly used orbital models of 3: 2 HF QPOs. We show that the estimate of a > 0.9 is almost inconsistent with two hot-spot(relativistic precession and tidal disruption) models and the warped disc resonance model. In contrast, we demonstrate that the epicyclic resonance and discoseismic models assuming the c-and g-modes are favoured. We extend our discussion to another two microquasars that display the 3: 2 HF QPOs. The frequencies of these QPOs scale roughly inversely to the microquasar masses, and the differences in the individual spins, such as a = 0.9 compared to a = 0.7, represent a generic problem for

Keywords

X-rays: binariesblack hole physicsaccretionaccretion disks

The result's identifiers

Alternative languages

  • Result language

    angličtina

  • Original language name

    Confronting the models of 3:2 quasiperiodic oscillations with the rapid spin of the microquasar GRS 1915+105

  • Original language description

    Spectral fitting of the spin a = cJ/GM(2) in the microquasar GRS 1915+105 estimate values higher than a = 0.98. However, there are certain doubts about this (nearly) extremal number. Confirming a high value of a > 0.9 would have significant concequencesfor the theory of high-frequency quasiperiodic oscillations (HF QPOs). Here we discuss its possible implications assuming several commonly used orbital models of 3: 2 HF QPOs. We show that the estimate of a > 0.9 is almost inconsistent with two hot-spot(relativistic precession and tidal disruption) models and the warped disc resonance model. In contrast, we demonstrate that the epicyclic resonance and discoseismic models assuming the c-and g-modes are favoured. We extend our discussion to another two microquasars that display the 3: 2 HF QPOs. The frequencies of these QPOs scale roughly inversely to the microquasar masses, and the differences in the individual spins, such as a = 0.9 compared to a = 0.7, represent a generic problem for

  • Czech name

  • Czech description

Classification

  • Type

    Jx - Unclassified - Peer-reviewed scientific article (Jimp, Jsc and Jost)

  • CEP classification

    BE - Theoretical physics

  • OECD FORD branch

Result continuities

  • Project

    Result was created during the realization of more than one project. More information in the Projects tab.

  • Continuities

    P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
    Z - Vyzkumny zamer (s odkazem do CEZ)
    S - Specificky vyzkum na vysokych skolach

Others

  • Publication year

    2011

  • Confidentiality

    S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Data specific for result type

  • Name of the periodical

    ASTRONOMY & ASTROPHYSICS

  • ISSN

    0004-6361

  • e-ISSN

  • Volume of the periodical

    531

  • Issue of the periodical within the volume

  • Country of publishing house

    FR - FRANCE

  • Number of pages

    7

  • Pages from-to

    15549

  • UT code for WoS article

  • EID of the result in the Scopus database

Basic information

Result type

Jx - Unclassified - Peer-reviewed scientific article (Jimp, Jsc and Jost)

Jx

CEP

BE - Theoretical physics

Year of implementation

2011