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Title:
High-resolution spectra of very low-mass stars
Authors:
Tinney, C. G.; Reid, I. N.
Affiliation:
AA(Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia), AB(Palomar Observatory, 105-24, California Institute of Technology, Pasadena, CA 91125, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 301, Issue 4, pp. 1031-1048. (MNRAS Homepage)
Publication Date:
12/1998
Origin:
MNRAS
MNRAS Keywords:
TECHNIQUES: RADIAL VELOCITIES, STARS: ACTIVITY, STARS: CHROMOSPHERES, STARS: KINEMATICS, STARS: LOW-MASS, BROWN DWARFS, STARS: ROTATION
DOI:
10.1046/j.1365-8711.1998.02079.x
Bibliographic Code:
1998MNRAS.301.1031T

Abstract

We present the results of high-resolution (1-0.4Angstroms) optical spectroscopy of a sample of very low-mass stars. These data are used to examine the kinematics of the stars at the bottom of the hydrogen-burning main sequence. No evidence is found for a significant difference between the kinematics of the stars in our sample with I-K>3.5 (M_bol>~12.8) and those of more massive M dwarfs (M_bol~7-10). A spectral atlas at high (0.4-Angstroms) resolution for M8-M9+ stars is provided, and the equivalent widths of CsI, RbI and Hα lines present in our spectra are examined. We analyse our data to search for the presence of rapid rotation, and find that the brown dwarf LP944-20 is a member of the class of `inactive, rapid rotators'. Such objects seem to be common at and below the hydrogen-burning main sequence. It seems that in low-mass/low-temperature dwarf objects either the mechanism that heats the chromosphere, or the mechanism that generates magnetic fields, is greatly suppressed.

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