NLTT5306B: an inflated, weakly irradiated brown dwarf
NLTT5306B: an inflated, weakly irradiated brown dwarf
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NLTT5306B：一颗膨胀的、受弱辐射的褐矮星
DOI：
10.1093/mnras/staa3184
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发表时间：
2020
影响因子：
4.8
通讯作者：
J. Kirkpatrick
中科院分区：
文献类型：
--
作者：
S. Casewell;J. Debes;I. Braker;M. Cushing;G. Mace;M. Marley;J. Kirkpatrick
我们在3.6和4.5 μm的斯皮策观测和辐射褐矮星NLTT 5306B的近红外IRTF SpeX光谱。我们确定棕矮星的光谱类型为L5，并且可能是膨胀的，尽管白色矮星的主星星的有效温度很低。我们计算的亮度温度在斯皮策波段的模型半径，和罗氏瓣半径的棕矮星，并得出结论，有很小的昼夜侧温差。我们讨论了NLTT 5306 B可能膨胀的各种机制，并确定虽然低质量的棕矮星（M < 35 MJup）很容易通过其宿主星星的照射而膨胀，但很少有更高质量的棕矮星会膨胀。质量较高的棕矮星可能是由于磁相互作用而膨胀，或者可能有更厚的云。
We present Spitzer observations at 3.6 and 4.5 µm and a near-infrared IRTF SpeX spectrum of the irradiated brown dwarf NLTT5306B. We determine that the brown dwarf has a spectral type of L5 and is likely inflated, despite the low effective temperature of the white dwarf primary star. We calculate brightness temperatures in the Spitzer wavebands for both the model radius, and Roche Lobe radius of the brown dwarf, and conclude that there is very little day–night side temperature difference. We discuss various mechanisms by which NLTT5306B may be inflated, and determine that while low-mass brown dwarfs (M < 35 MJup) are easily inflated by irradiation from their host star, very few higher mass brown dwarfs are inflated. The higher mass brown dwarfs that are inflated may be inflated by magnetic interactions or may have thicker clouds.
影响因子：
4.8
作者：
S. Casewell;I. Braker;S. Parsons;J. Hermes;M. Burleigh;C. Belardi;A. Chaushev;N. Finch;M. Roy;S. Littlefair;M. Goad;E. Dennihy
通讯作者：
S. Casewell;I. Braker;S. Parsons;J. Hermes;M. Burleigh;C. Belardi;A. Chaushev;N. Finch;M. Roy;S. Littlefair;M. Goad;E. Dennihy
影响因子：
6.5
作者：
Baraffe, Isabelle;Homeier, Derek;Chabrier, Gilles
通讯作者：
Chabrier, Gilles