Could the Planets Around HR 8799 be Brown Dwarfs?

Could the Planets Around HR 8799 be Brown Dwarfs?

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 {approx}100 Myr, not with the 1 Gyr age proposed from asteroseismology. The discrepancy probably arises because the inclination of the star is smaller than assum...

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Veröffentlicht in:Astrophysical journal. Letters 2010-10, Vol.721 (2), p.L199-L202
Hauptverfasser: Moro-Martín, Amaya, Rieke, George H, Su, Kate Y. L
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Sprache:eng
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ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
INCLINATION
MASS
MATTER
PLANETS
STARS
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container_title Astrophysical journal. Letters
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creator Moro-Martín, Amaya
Rieke, George H
Su, Kate Y. L
description 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 {approx}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.
doi_str_mv 10.1088/2041-8205/721/2/L199
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subjects ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
INCLINATION
MASS
MATTER
PLANETS
STARS
title Could the Planets Around HR 8799 be Brown Dwarfs?
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