Velocity dispersion of nearby M dwarfs

Journal Article · Wed Oct 01 00:00:00 EDT 1975 · Publ. Astron. Soc. Pac., v. 87, no. 519, pp. 699-703

DOI:https://doi.org/10.1086/129830· OSTI ID:4108991

Krisciunas, K

It is shown that the velocity dispersion of a large sample of stars can be determined by their distribution on the sky as a function of angular distance from the solar apex. Known or suspected M dwarfs from Gliese's catalog were divided into groups according to distance from the sun, angular distance from the solar apex, whether or not the stars had emission lines, and whether or not they were members of binary or multiple systems. It was found that with this method only a lower limit of the transverse velocity dispersion could be derived. This value was 13 km sec$sup -1$. Based on the present technique and the presently available data, the existence of low-velocity M dwarfs cannot be ruled out. (auth)

• Research Organization: Univ. of California, Santa Cruz
• Sponsoring Organization: USDOE
• NSA Number: NSA-33-018059
• OSTI ID: 4108991
• Journal Information: Publ. Astron. Soc. Pac., v. 87, no. 519, pp. 699-703, Other Information: Orig. Receipt Date: 30-JUN-76
• Country of Publication: United States
• Language: English

Related Subjects

N56200* -Physics (Astrophysics & Cosmology)-Stars
640102* -Physics Research-Astrophysics & Cosmology-Stars
*DWARF STARS- BINARY STARS
DISTANCE
EMISSION SPECTRA
PROPER MOTION
SPATIAL DISTRIBUTION
VELOCITY