Detection of Hα Emission in a Methane (T Type) Brown Dwarf | Zendy

Adam J. Burgasser | Zendy; J. Davy Kirkpatrick | Zendy; I. Neill Reid | Zendy; James Liebert | Zendy; John E. Gizis | Zendy; Michael E. Brown | Zendy

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Detection of Hα Emission in a Methane (T Type) Brown Dwarf

Author(s) -

Adam J. Burgasser,

J. Davy Kirkpatrick,

I. Neill Reid,

James Liebert,

John E. Gizis,

Michael E. Brown

Publication year - 2000

Publication title -

the astronomical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.61

H-Index - 271

eISSN - 1538-3881

pISSN - 0004-6256

DOI - 10.1086/301423

Subject(s) - physics , brown dwarf , astrophysics , spectrograph , line (geometry) , flux (metallurgy) , astronomy , emission spectrum , methane , stars , spectral line , biology , chemistry , geometry , mathematics , ecology , organic chemistry

We report the detection of H{$\alpha$} emission in the T dwarf (methane browndwarf) 2MASSW J1237392+652615 over three days using the Keck Low ResolutionImaging Spectrograph. The measured line flux, log(L$_{H{\alpha}}$/L$_{bol}$) =$-$4.3, is roughly consistent with early M dwarf activity levels andinconsistent with decreasing activity trends in late M and L dwarfs. Similaremission is not seen in two other T dwarfs. We speculate on several mechanismsthat may be responsible for emission, including a strong magnetic field,continuous flaring, acoustic heat generation, and a close ($a$ $\sim$ 4 - 20R$_{Jup}$) interacting binary, with the cooler component overflowing its Rochelobe. We suggest that the M9.5Ve PC 0025+0447 could be a warm analogue to 2MASSJ1237+65, and may be powered by the latter mechanism.Comment: 14 pages, 3 figures, accepted by A

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