2013
Confronting the Models of 3:2 QPOs with the Evidence of Near Extreme Kerr Black Hole
KOTRLOVÁ, Andrea, Zdeněk STUCHLÍK, Eva ŠRÁMKOVÁ a Gabriel TÖRÖKZákladní údaje
Originální název
Confronting the Models of 3:2 QPOs with the Evidence of Near Extreme Kerr Black Hole
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Vydání
Cambridge, UK, Proceedings of the International Astronomical Union, Symposium No. 290: Feeding compact objects: Accretion on all scales, od s. 239-240, 2 s. 2013
Nakladatel
Cambridge University Press
Další údaje
Jazyk
angličtina
Typ výsledku
Stať ve sborníku
Obor
10308 Astronomy
Utajení
není předmětem státního či obchodního tajemství
Odkazy
Organizační jednotka
Filozoficko-přírodovědecká fakulta v Opavě
ISBN
978-1-107-03379-5
ISSN
Klíčová slova anglicky
accretion; accretion disks; X-rays: binaries; black hole physics
Příznaky
Mezinárodní význam
Návaznosti
GPP209/12/P740, projekt VaV.
Změněno: 7. 12. 2020 14:39, Mgr. Pavlína Jalůvková
Anotace
V originále
The black hole mass and spin estimates assuming various specific models of the 3 : 2 high frequency quasi-periodic oscillations (HF QPOs) have been carried out in T¨or¨ok et al. (2005, 2011). Here we briefly summarize some current points. Spectral fitting of the spin a=cJ/GM2 in the microquasar GRS 1915+105 reveals that this system can contain a near extreme rotating black hole (e.g., McClintock et al., 2011). Confirming the high value of the spin would have significant consequences for the theory of the HF QPOs. The estimate of a > 0.9 is almost inconsistent with the relativistic precession (RP), tidal disruption (TD), and the warped disc (WD) model. The epicyclic resonance (Ep) and discoseismic models assuming the c- and g- modes are instead favoured. However, consideration of all three microquasars that display the 3 : 2 HF QPOs leads to a serious puzzle because the differences in the individual spins, such as a = 0.9 compared to a = 0.7, represent a generic problem almost for any u