Modelling the spectra of planets, brown dwarfs and stars using vstar

被引:49
作者
Bailey, Jeremy [1 ]
Kedziora-Chudczer, Lucyna [1 ]
机构
[1] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia
关键词
radiative transfer; techniques: spectroscopic; planets and satellites: atmospheres; stars: atmospheres; brown dwarfs; INTERNAL PARTITION SUMS; COMPUTED LINE LIST; BAND Q-BRANCH; MU-M SPECTRA; TEMPERATURE-DEPENDENCE; MOLECULAR OPACITIES; INFRARED-ABSORPTION; THERMAL STRUCTURE; LIGHT-SCATTERING; THERMOCHEMICAL PROPERTIES;
D O I
10.1111/j.1365-2966.2011.19845.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We describe a new software package capable of predicting the spectra of Solar system planets, exoplanets, brown dwarfs and cool stars. The Versatile Software for Transfer of Atmospheric Radiation (vstar) code combines a line-by-line approach to molecular and atomic absorption with a full multiple scattering treatment of radiative transfer. vstar is a modular system incorporating an ionization and chemical equilibrium model, a comprehensive treatment of spectral line absorption using a data base of more than 2.9 billion spectral lines, a scattering package and a radiative transfer module. We test the methods by comparison with other models and benchmark calculations. We present examples of the use of vstar to model the spectra of terrestrial and giant planet in our own Solar system, brown dwarfs and cool stars.
引用
收藏
页码:1913 / 1929
页数:17
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