Are Delayed Radio Flares Common in Tidal Disruption Events? The Case of the TDE iPTF 16fnl
Are Delayed Radio Flares Common in Tidal Disruption Events? The Case of the TDE iPTF 16fnl
复制标题
延迟射电耀斑在潮汐破坏事件中常见吗？
DOI：
10.3847/2041-8213/ac25fe
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发表时间：
2021
期刊：
影响因子：
--
通讯作者：
J. Bright
中科院分区：
文献类型：
--
作者：
A. Horesh;I. Sfaradi;R. Fender;D. Green;David R. A. Williams;J. Bright
潮汐破裂事件（TDEs）的射电辐射起源于外流与超大质量黑洞（SMBH）的环核物质（CNM）的相互作用。反过来，这种无线电发射可以用来探测事件和CNM发射的外流的性质。直到最近，无线电发射只在相对较少的事件中被检测到。虽然观测到的无线电辐射指向不同性质的相对论或次相对论外流，但它也表明外流是在恒星破裂后不久发射的。然而，最近，在TDE ASASSN-15 oi的情况下，报告了恒星破裂后数月和数年的延迟射电耀斑。这些延迟耀斑表明，在发射外流延迟，从而可能提供新的见解SMBH吸积物理。在这里，我们提出了一个新的无线电数据集的另一个TDE，iPTF 16 fnl，并讨论了延迟的射电耀斑也被观察到在这种情况下，光学发现后15个月的可能性，这表明这种现象可能是常见的TDE。与ASASSN-15 oi不同，iPTF 16 fnl的数据稀疏，延迟的射电耀斑可以用几种替代模型来解释：其中包括复杂的变化的CNM密度结构和延迟的外流喷射。
Radio emission from tidal disruption events (TDEs) originates from an interaction of an outflow with the super-massive black hole (SMBH) circumnuclear material (CNM). In turn, this radio emission can be used to probe properties of both the outflow launched at the event and the CNM. Until recently, radio emission was detected only for a relatively small number of events. While the observed radio emission pointed to either relativistic or sub-relativistic outflows of different nature, it also indicated that the outflow has been launched shortly after stellar disruption. Recently, however, delayed radio flares, several months and years after stellar disruption, were reported in the case of the TDE ASASSN-15oi. These delayed flares suggest a delay in the launching of outflows and thus may provide new insights into SMBH accretion physics. Here, we present a new radio data set of another TDE, iPTF 16fnl, and discuss the possibility that a delayed radio flare also has been observed in this case, ∼5 months after optical discovery, suggesting that this phenomenon may be common in TDEs. Unlike ASASSN-15oi, the data for iPTF 16fnl is sparse and the delayed radio flare can be explained by several alternative models: among them are a complex varying CNM density structure and a delayed outflow ejection.
影响因子：
14.1
作者：
R. Stein;S. Velzen;M. Kowalski;A. Franckowiak;S. Gezari;J. Miller-Jones;S. Frederick;I. Sfaradi
通讯作者：
R. Stein;S. Velzen;M. Kowalski;A. Franckowiak;S. Gezari;J. Miller-Jones;S. Frederick;I. Sfaradi