Tungsten versus Selenium as a potential source of kilonova nebular emission observed by Spitzer
Tungsten versus Selenium as a potential source of kilonova nebular emission observed by Spitzer
复制标题
钨与硒作为斯皮策观测到的千新星星云发射的潜在来源
DOI：
10.1093/mnrasl/slac071
复制
发表时间：
2022
影响因子：
--
通讯作者：
Gaigalas Gediminas
中科院分区：
文献类型：
--
作者：
Hotokezaka Kenta;Tanaka Masaomi;Kato Daiji;Gaigalas Gediminas
由重元素的精细结构能级之间的跃迁产生的红外发射线预计将产生千诺瓦星云发射。对于GW 170817中的千新星，斯皮策太空望远镜在晚些时候探测到了强辐射，但在晚些时候没有探测到辐射源。这一奇特的光谱表明，强线发射体存在于周围，而周围没有强线。为了对光谱进行建模，我们根据NIST数据库中实验校准的能级的LS耦合中的选择规则准备了一个线列表。该方法能够生成具有精确线波长的合成光谱。我们发现，光谱是敏感的丰度模式是否包括第一r-过程峰元素。在这两种情况下，合成光谱可以匹配观察到的数据，导致两种可能的解释。如果第一峰元素丰富，则硒线占主导地位。如果不是这样的话，威尔与奥西、里尔和塞夫可以成为主要的来源。在更宽的波长范围内观测未来千诺瓦的星云光谱可以提供更确凿的元素鉴定。
Infrared emission lines arising from transitions between fine structure levels of heavy elements are expected to produce kilonova nebular emission. For the kilonova in GW170817, strong emission atat late times was detected by theSpitzer Space Telescopebut no source was detected at. This peculiar spectrum indicates that strong line emitters exist aroundand the absence of strong lines around. To model the spectrum we prepare a line list based on the selection rules in LS coupling from the experimentally calibrated energy levels in the NIST database. This method enables to generate the synthetic spectra with accurate line wavelengths. We find that the spectrum is sensitive to the abundance pattern whether or not the first r-process peak elements are included. In both cases, the synthetic spectra can match the observed data, leading to two possible interpretations. If the first peak elements are abundant, a Seiiiline dominates the flux. If otherwise, Wiiiwith Osiii, Rhiii, and Ceivcan be the main sources. Observing nebular spectra for the future kilonova in a wider wavelength range can provide more conclusive elemental identification.