Refining the OJ 287 2022 impact flare arrival epoch
Refining the OJ 287 2022 impact flare arrival epoch
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DOI：
10.1093/mnras/stad922
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发表时间：
2023-03
影响因子：
4.8
通讯作者：
M. Valtonen;S. Zoła;A. Gopakumar;A. Lähteenmäki;M. Tornikoski;L. Dey;Alok C. Gupta;T. Pursimo;E. Knudstrup;J. Gómez;R. Hudec;Martin Jelínek;J. Štrobl;A. Berdyugin;S. Ciprini;D. Reichart;V. Kouprianov;K. Matsumoto;M. Dróżdż;M. Mugrauer;A. Sadun;M. Zejmo;A. Sillanpää;H. Lehto;K. Nilsson;R. Imazawa;M. Uemura
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文献类型：
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作者：
M. Valtonen;S. Zoła;A. Gopakumar;A. Lähteenmäki;M. Tornikoski;L. Dey;Alok C. Gupta;T. Pursimo;E. Knudstrup;J. Gómez;R. Hudec;Martin Jelínek;J. Štrobl;A. Berdyugin;S. Ciprini;D. Reichart;V. Kouprianov;K. Matsumoto;M. Dróżdż;M. Mugrauer;A. Sadun;M. Zejmo;A. Sillanpää;H. Lehto;K. Nilsson;R. Imazawa;M. Uemura
明亮的耀变体OJ 287经常会出现高亮度的韧致辐射耀斑，这被解释为是次级超大质量黑洞（SMBH）撞击双星系统中更大质量的初级SMBH的吸积盘的结果。吸积盘不是刚性的，而是由于次级潮汐的影响而以可计算的方式弯曲。下面我们将这种现象称为可变椎间盘水平。我们开始表明，这些耀斑发生的时间预测的一个简单的分析公式，根据广义相对论启发修改开普勒方程，解释自1888年以来的影响耀斑。2022年的撞击耀斑，即第26号耀斑，是相当特殊的，因为它打破了每12年周期发生两次撞击耀斑的典型模式。这是当前周期的第三次韧致辐射耀斑，此前已经观察到2015年和2019年OJ 287的撞击耀斑。结果表明，在我们的模型中，26号耀斑的到达时期对原始SMBH吸积盘相对于其平均水平的水平是敏感的。我们将这些潮汐引起的吸积盘水平变化纳入其中，以推断热耀斑应该发生在2022年7月至8月期间，当时不可能从地球上观察到它。此后，我们通过使用2004/05和2021/22年活动的光谱和偏振数据，探索某些耀斑前活动的可能观测证据。我们指出了2022年1月至2月期间观察到的两个小耀斑的理论和观测意义。
The bright blazar OJ 287 routinely parades high brightness bremsstrahlung flares, which are explained as being a result of a secondary supermassive black hole (SMBH) impacting the accretion disc of a more massive primary SMBH in a binary system. The accretion disc is not rigid but rather bends in a calculable way due to the tidal influence of the secondary. Below we refer to this phenomenon as a variable disc level. We begin by showing that these flares occur at times predicted by a simple analytical formula, based on general relativity inspired modified Kepler equation, which explains impact flares since 1888. The 2022 impact flare, namely flare number 26, is rather peculiar as it breaks the typical pattern of two impact flares per 12-year cycle. This is the third bremsstrahlung flare of the current cycle that follows the already observed 2015 and 2019 impact flares from OJ 287. It turns out that the arrival epoch of flare number 26 is sensitive to the level of primary SMBH’s accretion disc relative to its mean level in our model. We incorporate these tidally induced changes in the level of the accretion disc to infer that the thermal flare should have occurred during July-August 2022, when it was not possible to observe it from the Earth. Thereafter, we explore possible observational evidence for certain pre-flare activity by employing spectral and polarimetric data from our campaigns in 2004/05 and 2021/22. We point out theoretical and observational implications of two observed mini-flares during January-February 2022.