Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· References in the article
· Citations to the Article (1) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· Reads History
·
· Translate This Page
Title:
Spectroscopy of the variable K-dwarf UNSW-V-760: is it a pre-main-sequence pulsator?
Authors:
Koen, C.; Gray, R. O.; Kawaler, S.; Crawford, S. M.
Affiliation:
AA(Department of Statistics, University of the Western Cape, Private Bag X17, Bellville, 7535 Cape, South Africa; ), AB(Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608, USA), AC(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA), AD(South African Astronomical Observatory, PO Box 9, Observatory, 7935 Cape, South Africa)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 435, Issue 3, p.2494-2500 (MNRAS Homepage)
Publication Date:
11/2013
Origin:
OUP
Astronomy Keywords:
stars: individual: UNSW-V-760, stars: pre-main-sequence, stars: variables: T Tauri, Herbig Ae/Be
Abstract Copyright:
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stt1478
Bibliographic Code:
2013MNRAS.435.2494K

Abstract

The star UNSW-V-760 is a known variable, showing both flares and two non-sinusoidal periodicities. Availability of high signal-to-noise spectra reported in this paper has enabled a revision of the spectral type of this star to K3 IV-Vk. The star is a very rapid rotator (v sin i ˜ 140 km s-1), and the abundance of lithium appears to be enhanced. 48 radial velocity measurements were obtained over the course of three successive nights. These may show the same two frequencies detected photometrically, but there is some uncertainty in the interpretation. Application of pulsation theory suggests that photometric frequencies could be explained as low l pulsation modes, but an excitation mechanism remains to be found.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints