KOTRLOVÁ, Andrea, Zdeněk STUCHLÍK, Eva ŠRÁMKOVÁ and Gabriel TÖRÖK. Confronting the models of 3:2 quasiperiodic oscillations with the rapid spin of the microquasar GRS 1915+105. Astronomy & Astrophysics. FR - Francouzská republika, 2011, vol. 531, A59, 7 pp. ISSN 0004-6361. Available from: https://dx.doi.org/10.1051/0004-6361/201015549.
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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
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Confidentiality degree is not subject to a state or trade secret
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).
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 7/4/2021 07:53.
Abstract
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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