Optical and X-ray timing analysis of the 2018–2020 outburst and rebrightening of the black hole transient MAXI J1820+070

Fiori, M.; Zampieri, L.; Burtovoi, A.; Naletto, G.; Ochner, P.; Munari, U.; Manzini, F.; Vagnozzi, A.; Barsukova, E.A.; Burlak, M.A.; Goranskij, V.P.; Ikonnikova, N.P.; Katysheva, N.A.; Sheyanov, E.G.; Shugarov, S.Y.; Zharova, A.V.; Zubareva, A.M.; Motta, S.E.

Авторы: Fiori M., Zampieri L., Burtovoi A., Naletto G., Ochner P., Munari U., Manzini F., Vagnozzi A., Barsukova E.A., Burlak M.A., Goranskij V.P., Ikonnikova N.P., Katysheva N.A., Sheyanov E.G., Shugarov S.Yu, Zharova A.V., Zubareva A.M., Motta S.E.
Журнал: Astronomy and Astrophysics
Том: 697
Год издания: 2025
Издательство: Springer Verlag
Местоположение издательства: Germany
Первая страница: A222
DOI: 10.1051/0004-6361/202553899
Аннотация: We report the results of a comprehensive analysis of the multi-wavelength (in optical and X-rays) and multi-timescale (from monthsto tenths of a second) variability of the 2018–2020 outburst of the black hole transient MAXI J1820+070. A detailed analysis ofthe optical photometry revealed a periodicity that evolves over time during the first outburst episode and stabilises at a frequency of1.4517(1) 1/d (∼0.5% longer than the orbital period). This super-orbital modulation is also seen in the X-rays for a few days shortlyafter the transition to the high-soft state. We also observed optical quasi-periodic oscillations (QPOs) that correspond to some of theQPOs observed in X-rays at three different epochs when the source was in the low-hard state. In two epochs, optical QPOs with acentroid consistent with half the frequency of the most prominent X-ray QPO can be seen. If the lowest modulation frequency isthe one observed in the optical, the characteristic precession frequency of MAXI J1820+070 is lower than that inferred from the‘fundamental’ QPO in the X-rays. Assuming that QPOs can be generated by Lense-Thirring precession, we calculated the spin ofthe black hole in the case where the fundamental precession frequency is tracked by the optical emission. We find a relatively slowlyspinning black hole with a spin parameter of <0.15. The super-orbital optical and X-ray modulations observed after the disappearanceof the QPOs may be triggered by the self-irradiation of the outer disc by a standard inner disc truncated at a few gravitational radii.
Добавил в систему: Шугаров Сергей Юрьевич

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Optical and X-ray timing analysis of the 2018–2020 outburst and rebrightening of the black hole transient MAXI J1820+070статья

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