Infrared radiation from an extrasolar planet

被引:460
作者
Deming, D
Seager, S
Richardson, LJ
Harrington, J
机构
[1] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA
[2] NASA, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA
[3] NASA, Goddard Space Flight Ctr, Exoplanet & Stellar Astrophys Lab, Greenbelt, MD 20771 USA
[4] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA
[5] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA
基金
美国国家航空航天局;
关键词
D O I
10.1038/nature03507
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
A class of extrasolar giant planets-the so-called 'hot Jupiters' (ref. 1)-orbit within 0.05 AU of their primary stars ( 1 AU is the Sun-Earth distance). These planets should be hot and so emit detectable infrared radiation(2). The planet HD 209458b (refs 3, 4) is an ideal candidate for the detection and characterization of this infrared light because it is eclipsed by the star. This planet has an anomalously large radius (1.35 times that of Jupiter(5)), which may be the result of ongoing tidal dissipation(6), but this explanation requires a non-zero orbital eccentricity (similar to 0.03; refs 6, 7), maintained by interaction with a hypothetical second planet. Here we report detection of infrared (24-mu m) radiation from HD 209458b, by observing the decrement in flux during secondary eclipse, when the planet passes behind the star. The planet's 24-mu m flux is 55 +/- 10 mu Jy (1 sigma), with a brightness temperature of 1,130 +/- 150 K, confirming the predicted heating by stellar irradiation(2,8). The secondary eclipse occurs at the midpoint between transits of the planet in front of the star (to within +/- 7 min, 1 sigma), which means that a dynamically significant orbital eccentricity is unlikely.
引用
收藏
页码:740 / 743
页数:4
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