Could the planets around HR 8799 be brown dwarfs?

Amaya Moro-Martín, George H. Rieke, Kate Y.L. Su

Research output: Contribution to journalArticlepeer-review

26 Scopus citations

Abstract

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 ∼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.

Original languageEnglish (US)
Pages (from-to)L199-L202
JournalAstrophysical Journal Letters
Volume721
Issue number2 PART 2
DOIs
StatePublished - Oct 1 2010

Keywords

  • Circumstellar matter
  • Infrared: stars
  • Planetary systems
  • Stars: individual (HR 8799)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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