标题： 黑洞X射线双星MAXI J1820$+$070的吸积喷流联系 显示英文标题

标题： The Accretion-Ejection Connection in the Black Hole X-ray Binary MAXI J1820$+$070

摘要： 黑洞X射线双星MAXI J1820$+$070于2018年3月开始了其首次记录的爆发，并在超过四年的时间里一直是一个活跃的射电、X射线和光学源。 由于该源距离较近且本身具有极高的光度，MAXI J1820$+$070在此段时间内被广泛观测，从而在电磁波谱上实现了高频率和准同时的观测。 这些数据集提供了比大多数黑洞X射线双星更详细地研究吸积与喷流发射之间联系的机会。 在本工作中，我们展示了MAXI J1820$+$070在整个爆发期间的射电（Arcminute Microkelvin Imager Large Array，MeerKAT）、X射线（Swift）和光学（Las Cumbres Observatory）观测数据，包括其初始硬态、随后的软态以及后续仅硬态的再次增亮（覆盖2018年3月至2022年8月）。 由于观测数据的规律性和时间密度，我们能够创建一个射电- X射线-光学活动平面，在此我们发现硬态期间三个波段之间有高度的相关性，并观察到当MAXI J1820$+$070进入和退出软态时的滞回现象。 根据光学光变曲线的形态，我们发现在软态到硬态转变期间存在光学喷流贡献的证据，以及在硬态到软态转变之前光学辐射就已减弱。 我们确定再增亮事件的显著相似轮廓大致符合修改后的盘不稳定性模型，其中包含了来自内吸积盘的照射。 显示英文摘要

摘要： The black hole X-ray binary MAXI J1820$+$070 began its first recorded outburst in March 2018, and remained an active radio, X-ray, and optical source for over four years. Due to the low distance to the source and its intrinsically high luminosity MAXI J1820$+$070 was observed extensively over this time period, resulting in high-cadence and quasi-simultaneous observations across the electromagnetic spectrum. These data sets provide the opportunity to probe the connection between accretion and the launch of jets in greater detail than for the majority of black hole X-ray binaries. In this work we present radio (Arcminute Microkelvin Imager Large Array, MeerKAT), X-ray (Swift), and optical (Las Cumbres Observatory) observations of MAXI J1820$+$070 throughout its entire outburst, including its initial hard state, subsequent soft state, and further hard-state-only re-brightenings (covering March 2018 to August 2022). Due to the regularity and temporal density of our observational data we are able to create a Radio - X-ray - Optical activity plane where we find a high degree of correlation between the three wave bands during the hard states, and observe hysteresis as MAXI J1820$+$070 enters and exits the soft state. Based on the morphology of the optical light curves we see evidence for optical jet contributions during the soft-to-hard state transition, as well as fading optical emission well before the hard to soft transition. We establish that the remarkably similar profiles of the re-brightening events are broadly consistent with modified disk instability models where irradiation from the inner accretion disk is included.