UV absorption by silicate cloud precursors in ultra-hot Jupiter WASP-178b

被引:42
作者
Lothringer, Joshua D. [1 ,2 ]
Sing, David K. [2 ,3 ]
Rustamkulov, Zafar [3 ]
Wakeford, Hannah R. [4 ]
Stevenson, Kevin B. [3 ,5 ]
Nikolov, Nikolay [6 ]
Lavvas, Panayotis [7 ]
Spake, Jessica J. [8 ]
Winch, Autumn T. [9 ]
机构
[1] Utah Valley Univ, Dept Phys, Orem, UT 84058 USA
[2] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
[3] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA
[4] Univ Bristol, Sch Phys, HH Wills Phys Lab, Bristol, Avon, England
[5] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA
[6] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[7] Univ Reims, Grp Spectrometrie Mol & Atmospher, Champagne Ardenne, CNRS UMR, F-7331 Reims, France
[8] CALTECH, Dept Astron, Pasadena, CA 91125 USA
[9] Bryn Mawr Coll, Dept Phys, Bryn Mawr, PA 19010 USA
关键词
ATMOSPHERE; CHEMISTRY; STARS; DWARF; CONTINUUM;
D O I
10.1038/s41586-022-04453-2
中图分类号
O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];
学科分类号
07 ; 0710 ; 09 ;
摘要
Aerosols have been found to be nearly ubiquitous in substellar atmospheres(1-3). The precise temperature at which these aerosols begin to form in exoplanets has yet to be observationally constrained. Theoretical models and observations of muted spectral features indicate that silicate clouds play an important role in exoplanets between at least 950 and 2,100 K (ref. (4)). Some giant planets, however, are thought to be hot enough to avoid condensation altogether(5,6). Here we report the near-ultraviolet transmission spectrum of the ultra-hot Jupiter WASP-178b (approximately 2,450 K), which exhibits substantial absorption. Bayesian retrievals indicate the presence of gaseous refractory species containing silicon and magnesium, which are the precursors to condensate clouds at lower temperatures. SiO, in particular, has not previously, to our knowledge, been detected in exoplanets, but the presence of SiO in WASP-178b is consistent with theoretical expectations as the dominant Si-bearing species at high temperatures. These observations allow us to re-interpret previous observations of HAT-P-41b and WASP-121b that did not consider SiO, to suggest that silicate cloud formation begins on exoplanets with equilibrium temperatures between 1,950 and 2,450 K.
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收藏
页码:49 / +
页数:18
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