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A Brown Dwarf in the Desert

5 Apr 2021, 14:00 UTC
A Brown Dwarf in the Desert
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Title: ESPRESSO Mass determination of TOI-263b: An extreme inhabitant of the brown dwarf desertAuthors: E. Palle, R. Luque, M. R. Zapatero Osorio, H. Parviainen, M. Ikoma, H. M. Tabernero, M. Zechmeister, A.J. Mustill, V.S.J. Bejar, N. Narita, F. MurgasFirst Author’s Institution: Instituto de Astrofísica de Canarias (IAC), E-38200 La Laguna, Tenerife, SpainStatus: Accepted to A&A [not yet published, access unknown]
The Brown Dwarf DesertBrown dwarfs are typically defined as objects with masses between 13-80 times that of Jupiter, or 0.013-0.08 times that of the sun. They are too low in mass to fuse hydrogen into helium and become main sequence stars (thus labelled “substellar”), but they are massive enough to fuse deuterium, which sets them apart from giant planets. This deuterium burning phase is relatively short-lived (roughly 4-50 million years), after which brown dwarfs fade in luminosity and appear in many ways similar to high-mass planets. Because deuterium burning does not have a major effect on a brown dwarf after very early stages of its existence, some astronomers prefer a different definition to set apart brown dwarfs and planets, in which brown dwarfs form like stars, and planets form in disks around stars. I stick to the mass definition of ...

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