COULD THE PLANETS AROUND HR 8799 BE BROWN DWARFS?

被引：26

作者：

Moro-Martin, Amaya ^{[1
,2
]}

Rieke, George H. ^{[3
]}

Su, Kate Y. L. ^{[3
]}

机构：

[1] CSIC, Dept Astrofis, CAB, INTA, Madrid 28850, Spain

[2] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[3] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 721卷 / 02期

关键词：

circumstellar matter; infrared: stars; planetary systems; stars: individual ( HR 8799); EXTRASOLAR GIANT PLANETS; DEBRIS DISK; EVOLUTIONARY MODELS; RESONANCE; SPITZER; STARS; TIME;

D O I：

10.1088/2041-8205/721/2/L199

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We consider the limiting case for orbital stability of the companions to HR 8799. This case is only consistent with ages for the system of similar to 100 Myr, not with the 1 Gyr age proposed from asteroseismology. The discrepancy probably arises because the inclination of the star is smaller than assumed in analyzing the asteroseismology data. Given this young age, the best estimates of the companion masses place them by a small margin on the planet side of the division between planets and brown dwarfs.

引用

页码：L199 / L202

页数：4

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