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)
· arXiv e-print (arXiv:0707.4540)
· References in the article
· Citations to the Article (4) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The first high-amplitude δ Scuti star in an eclipsing binary system
Authors:
Christiansen, J. L.; Derekas, A.; Ashley, M. C. B.; Webb, J. K.; Hidas, M. G.; Hamacher, D. W.; Kiss, L. L.
Affiliation:
AA(School of Physics, University of New South Wales, Sydney 2052, Australia), AB(School of Physics, University of Sydney, Sydney 2006, Australia), AC(School of Physics, University of New South Wales, Sydney 2052, Australia), AD(School of Physics, University of New South Wales, Sydney 2052, Australia), AE(School of Physics, University of New South Wales, Sydney 2052, Australia; Las Cumbres Observatory Global Telescope, Goleta, CA 93117, USA; Department of Physics, University of California, Santa Barbara, CA 93106, USA), AF(School of Physics, University of New South Wales, Sydney 2052, Australia), AG(School of Physics, University of Sydney, Sydney 2006, Australia)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 382, Issue 1, pp. 239-244. (MNRAS Homepage)
Publication Date:
11/2007
Origin:
MNRAS
MNRAS Keywords:
binaries: eclipsing, δ Scuti
Abstract Copyright:
(c) 2007 The Authors. Journal compilation © 2007 RAS
DOI:
10.1111/j.1365-2966.2007.12338.x
Bibliographic Code:
2007MNRAS.382..239C

Abstract

We report the discovery of the first high-amplitude δ Scuti star in an eclipsing binary, which we have designated UNSW-V-500. The system is an Algol-type semi-detached eclipsing binary of maximum brightness V = 12.52 mag. A best-fitting solution to the binary light curve and two radial velocity curves is derived using the Wilson-Devinney code. We identify a late-A spectral-type primary component of mass 1.49 +/- 0.02Msolar and a late-K spectral-type secondary of mass 0.33 +/- 0.02Msolar, with an inclination of , and a period of 5.3504751 +/- 0.0000006 d. A Fourier analysis of the residuals from this solution is performed using PERIOD04 to investigate the δ Scuti pulsations. We detect a single pulsation frequency of f1 = 13.621 +/- 0.015 cd-1, and it appears that this is the first overtone radial mode frequency. This system provides the first opportunity to measure the dynamical mass for a star of this variable type; previously, masses have been derived from stellar evolution and pulsation models.
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
    


SAO/NASA ADS Homepage | ADS Sitemap | Query Form | Basic Search | Preferences | HELP | FAQ