Exoplanet Atmosphere Measurements from Direct Imaging
Exoplanet Atmosphere Measurements from Direct Imaging
复制标题
通过直接成像测量系外行星大气
DOI：
10.1007/978-3-319-55333-7_101
复制
发表时间：
2018
期刊：
影响因子：
--
通讯作者：
M. Bonnefoy
中科院分区：
文献类型：
--
作者：
B. Biller;M. Bonnefoy
在过去的十年中，大约有十几颗巨大的系外行星被直接成像为年轻恒星的同伴。通过新的极端日冕仪（如VLT的SPHERE和Gemini的GPI）对这些行星的光度测定和光谱分析，我们开始对这些天体的大气进行表征和分类。最初，人们认为年轻的行星将类似于褐矮星，更大的物体，但共享类似的有效温度和成分。令人惊讶的是，年轻的行星看起来比褐矮星要红得多，这可能是由于它们的表面重力较低，并表明大气结构有很大不同。首先，年轻的自由浮动行星似乎是一样或更多的变化比场褐矮星，由于旋转调制的不均匀的表面特征。最终，这种不均匀性将使这些物体的大气层结构顶部能够通过超大望远镜上的多普勒成像来映射。对巨大系外行星的直接成像光谱学是研究宜居带行星的前奏。最终，将有必要使用LUVOIR等未来望远镜对大量宜居带行星样本进行直接成像光谱分析，以确定多种生物特征，并确定附近恒星宜居带中地球质量系外行星的可居住性。
In the last decade, about a dozen giant exoplanets have been directly imaged in the IR as companions to young stars. With photometry and spectroscopy of these planets in hand from new extreme coronagraphic instruments such as SPHERE at VLT and GPI at Gemini, we are beginning to characterize and classify the atmospheres of these objects. Initially, it was assumed that young planets would be similar to field brown dwarfs, more massive objects that nonetheless share similar effective temperatures and compositions. Surprisingly, young planets appear considerably redder than field brown dwarfs, likely a result of their low surface gravities and indicating much different atmospheric structures. Preliminarily, young free-floating planets appear to be as or more variable than field brown dwarfs, due to rotational modulation of inhomogeneous surface features. Eventually, such inhomogeneity will allow the top of atmosphere structure of these objects to be mapped via Doppler imaging on extremely large telescopes. Direct imaging spectroscopy of giant exoplanets now is a prelude for the study of habitable zone planets. Eventual direct imaging spectroscopy of a large sample of habitable zone planets with future telescopes such as LUVOIR will be necessary to identify multiple biosignatures and establish habitability for Earth-mass exoplanets in the habitable zones of nearby stars.
DOI：
10.1088/0004-637x/777/2/160
发表时间：
2013-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
B. Biller;Michael C. Liu;Z. Wahhaj;E. Nielsen;Thomas L. Hayward;J. Males;A. Skemer;L. Close;M. Chun;C. Ftaclas;F. Clarke;N. Thatte;E. Shkolnik;I. N. Reid;M. Hartung;A. Boss;D. Lin;S. Alencar;E. M. de Gouveia Dal Pino;J. Gregorio-Hetem;D. Toomey
通讯作者：
B. Biller;Michael C. Liu;Z. Wahhaj;E. Nielsen;Thomas L. Hayward;J. Males;A. Skemer;L. Close;M. Chun;C. Ftaclas;F. Clarke;N. Thatte;E. Shkolnik;I. N. Reid;M. Hartung;A. Boss;D. Lin;S. Alencar;E. M. de Gouveia Dal Pino;J. Gregorio-Hetem;D. Toomey