Atmospheric study of brown dwarf HD 984 B

Paper Title:

Fresh view of the hot brown dwarf HD 984 B through high-resolution spectroscopy

Published on:

17 April 2024

Primary Category:

Solar and Stellar Astrophysics

Paper Authors:

J. C. Costes,

J. W. Xuan,

A. Vigan,

J. Wang,

V. D'Orazi,

P. Mollière,

A. Baker,

R. Bartos,

G. A. Blake,

B. Calvin,

S. Cetre,

J. Delorme,

G. Doppmann,

D. Echeveri,

L. Finnerty,

M. P. Fitzgerald,

C. Hsu,

N. Jovanovic,

R. Lopez,

D. Mawet,

E. Morris,

J. Pezzato,

C. L. Phillips,

J. Ruffio,

B. Sappey,

A. Schneeberger,

T. Schofield,

A. J. Skemer,

J. K. Wallace,

J. Wang

Bullets

Key Details

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HD 984 B has carbon-to-oxygen ratio equal to its host star

•

Its 12CO/13CO ratio is similar to the Sun's

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The brown dwarf has substellar metallicity

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Atmospheric properties suggest gravitational collapse / disk instability formation

Explore the topics in this paper

atmospheric characterization

brown dwarf

formation processes

infrared spectroscopy

isotopologue ratio

AI generated summary

Atmospheric study of brown dwarf HD 984 B

Using high-resolution infrared spectroscopy from the Keck Planet Imager and Characterizer, researchers analyzed the atmosphere of the young brown dwarf HD 984 B. They measured its carbon-to-oxygen ratio, 12CO/13CO isotopologue ratio, metallicity, and other properties. Their analysis suggests HD 984 B likely formed through gravitational collapse or disk instability rather than core accretion, the favored mechanism for giant exoplanets. More brown dwarf atmospheric characterization is needed to clarify details of formation processes.