J 2011

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

KOTRLOVÁ, Andrea, Zdeněk STUCHLÍK, Eva ŠRÁMKOVÁ and Gabriel TÖRÖK

Basic information

Original name

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

Authors

KOTRLOVÁ, Andrea, Zdeněk STUCHLÍK, Eva ŠRÁMKOVÁ and Gabriel TÖRÖK

Edition

Astronomy & Astrophysics, FR - Francouzská republika, 2011, 0004-6361

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Confidentiality degree

není předmětem státního či obchodního tajemství

Organization unit

Faculty of Philosophy and Science in Opava

DOI

http://dx.doi.org/10.1051/0004-6361/201015549

UT WoS

000293017700015

Keywords in English

X-rays: binaries, black hole physics, accretion, accretion disks

Tags

, GA202-090772, LC06014, MSM4781305903

Tags

International impact, Reviewed

Links

GA202/09/0772, research and development project. LC06014, research and development project. MSM4781305903, plan (intention).
Změněno: 7/4/2021 07:53, Mgr. Pavlína Jalůvková

Abstract

V originále

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
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