论文标题
在复发的Nova V2487 OPH上发现极端，每天大约每天的超级流量
Discovery of Extreme, Roughly-Daily Superflares on the Recurrent Nova V2487 Oph
论文作者
论文摘要
V2487 OPH是1900年和1998年检测到的爆发的复发性新星。令人震惊的是，V2487 OPH显示出耀斑，称为“ Superflares”，最高1.10个MAG振幅，快速升起，一分钟以下的快速上升，始终是最初的冲动尖峰，最初是一个随机的尾巴，典型地播出了一个典型的尾巴，并且一度典型的次数，并且曾经是典型的，并且曾经是终于的，并且一度时间均匀，并且均为终点。典型的耀斑能量$ e $超过10 $^{38} $ ergs，而年度能源预算为10 $^{41} $ ergs。 V2487 OPH Superflares遵守三个关系；耀斑能量的数量分布量表为$ e^{ - 2.34 \ pm0.35} $，从一个耀斑到下一个耀斑的等待时间与第一个事件的$ e $成正比，而火炬持续时间量表为$ e^{0.44 \ pm0.03} $。涉及重力和核能的场景无法满足这三个关系。但是，磁能情景可以解释所有三个关系。这种情况在圆盘上方的磁场线被其足迹的动作扭曲和放大，磁重新连接释放出作为超叶片光出来的能量。这种确切的机制已经众所周知，它发生在白光太阳耀斑，普通的M型耀斑之星以及H-R图中观察到的许多超叶状恒星中。超级恒星上的超级流量有上升时间，光曲线形状和持续时间，与V2487 OPH上的持续时间非常相似。因此，我们得出的结论是，V2487 OPH超级流是由大规模磁重新连接引起的。 V2487 OPH现在是最极端的Superflare恒星，表现出最大的已知耀斑能量（1.6 $ \ times $ 10 $^{39} $ ergs），并且出现率最快。
V2487 Oph is a recurrent nova with detected eruptions in 1900 and 1998. Startlingly, V2487 Oph shows flares, called `Superflares', with up to 1.10 mag amplitude, fast rises of under one-minute, always with an initial impulsive spike followed by a roughly-exponential tail, typically one-hour durations, and with random event times averaging once-per-day. The typical flare energy $E$ is over 10$^{38}$ ergs, while the yearly energy budget is 10$^{41}$ ergs. V2487 Oph Superflares obey three relations; the number distribution of flare energies scales as $E^{-2.34\pm0.35}$, the waiting time from one flare to the next is proportional to $E$ of the first event, and flare durations scale as $E^{0.44\pm0.03}$. Scenarios involving gravitational energy and nuclear energy fail to satisfy the three relations. The magnetic energy scenario, however, can explain all three relations. This scenario has magnetic field lines above the disc being twisted and amplified by the motions of their footprints, with magnetic reconnection releasing energy that comes out as Superflare light. This exact mechanism is already well known to occur in white light solar flares, in ordinary M-type flare stars, and in the many Superflare stars observed all across the H-R diagram. Superflares on Superflare stars have rise times, light curve shapes and durations that are very similar to those on V2487 Oph. So we conclude that the V2487 Oph Superflares are caused by large-scale magnetic reconnection. V2487 Oph is now the most extreme Superflare star, exhibiting the largest known flare energy (1.6$\times$10$^{39}$ ergs) and the fastest occurrence rate.
