KOTRLOVÁ, Andrea, Eva ŠRÁMKOVÁ, Gabriel TÖRÖK, Kateřina GOLUCHOVÁ, Jiří HORÁK, Odele STRAUB, Debora LANČOVÁ, Zdeněk STUCHLÍK a Marek ABRAMOWICZ. Models of high-frequency quasi-periodic oscillations and black hole spin estimates in Galactic microquasars. Astronomy & Astrophysics. FR - Francouzská republika, roč. 643, October, s. "A31-1"-"A31-9", 9 s. ISSN 0004-6361. doi:10.1051/0004-6361/201937097. 2020.
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Základní údaje
Originální název Models of high-frequency quasi-periodic oscillations and black hole spin estimates in Galactic microquasars
Autoři KOTRLOVÁ, Andrea (203 Česká republika, domácí), Eva ŠRÁMKOVÁ (203 Česká republika, domácí), Gabriel TÖRÖK (203 Česká republika, domácí), Kateřina GOLUCHOVÁ (203 Česká republika, domácí), Jiří HORÁK (203 Česká republika), Odele STRAUB (756 Švýcarsko, domácí), Debora LANČOVÁ (203 Česká republika, domácí), Zdeněk STUCHLÍK (203 Česká republika, domácí) a Marek ABRAMOWICZ (616 Polsko, domácí).
Vydání Astronomy & Astrophysics, FR - Francouzská republika, 2020, 0004-6361.
Další údaje
Originální jazyk angličtina
Typ výsledku Článek v odborném periodiku
Obor 10308 Astronomy
Stát vydavatele Francie
Utajení není předmětem státního či obchodního tajemství
WWW URL
Kód RIV RIV/47813059:19630/20:A0000010
Organizační jednotka Fyzikální ústav v Opavě
Doi http://dx.doi.org/10.1051/0004-6361/201937097
UT WoS 000588072000002
Klíčová slova anglicky X-rays: binaries; black hole physics; accretion; accretion disks
Štítky , FÚ2020, GA17-16287S, LTI17018, RIV21, SGS12-2019, SGS13-2019
Příznaky Mezinárodní význam, Recenzováno
Návaznosti GA17-16287S, projekt VaV. LTI17018, projekt VaV.
Změnil Změnil: doc. RNDr. Jiří Kovář, Ph.D., učo 49132. Změněno: 31. 3. 2022 17:35.
Anotace
We explore the influence of nongeodesic pressure forces present in an accretion disc on the frequencies of its axisymmetric and nonaxisymmetric epicyclic oscillation modes. We discuss its implications for models of high-frequency quasi-periodic oscillations (QPOs), which have been observed in the X-ray flux of accreting black holes (BHs) in the three Galactic microquasars, GRS 1915+105, GRO J1655-40, and XTE J1550-564. We focus on previously considered QPO models that deal with low-azimuthal-number epicyclic modes, |m| <= 2, and outline the consequences for the estimations of BH spin, a is an element of [0, 1]. For four out of six examined models, we find only small, rather insignificant changes compared to the geodesic case. For the other two models, on the other hand, there is a significant increase of the estimated upper limit on the spin. Regarding the falsifiability of the QPO models, we find that one particular model from the examined set is incompatible with the data. If the spectral spin estimates for the microquasars that point to a> 0.65 were fully confirmed, two more QPO models would be ruled out. Moreover, if two very different values of the spin, such as a approximate to 0.65 in GRO J1655-40 and a approximate to 1 in GRS 1915+105, were confirmed, all the models except one would remain unsupported by our results. Finally, we discuss the implications for a model that was recently proposed in the context of neutron star (NS) QPOs as a disc-oscillation-based modification of the relativistic precession model. This model provides overall better fits of the NS data and predicts more realistic values of the NS mass compared to the relativistic precession model. We conclude that it also implies a significantly higher upper limit on the microquasar's BH spin (a similar to 0.75 vs. a similar to 0.55).
VytisknoutZobrazeno: 28. 3. 2024 11:12