Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· References in the article
· Citations to the Article (6) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
High Temporal Resolution Spectroscopic Observations of the Flare Star V1054 Oph
Authors:
Crespo-Chacón, Inés; Montes, David; Fernández-Figueroa, María José; López-Santiago, Javier; García-Alvarez, David; Foing, Bernard H.
Affiliation:
AA(Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, Madrid, Spain. ), AB(Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, Madrid, Spain), AC(Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, Madrid, Spain), AD(Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, Madrid, Spain), AE(Armagh Observatory, College Hill, Armagh, Northern Ireland; Harvard-Smithsonian CfA, Cambridge, MA, USA), AF(Research Division, ESA Space Science Department, ESTEC/SCI-R, AG Noordwijk, The Netherlands)
Publication:
Astrophysics and Space Science, v. 292, Issue 1, p. 697-703 (2004). (Ap&SS Homepage)
Publication Date:
08/2004
Origin:
KLUWER; SPRINGER
Keywords:
stars: V1054 Oph, stars: flares: spectroscopic, stars: activity, stars: late-type
DOI:
10.1023/B:ASTR.0000045077.58363.e4
Bibliographic Code:
2004Ap&SS.292..697C

Abstract

We present the results of a high temporal resolution spectroscopic monitoring of the flare (UV Cet type) star V1054 Oph (Wolf 630AB), classified as a dM3.5e visual binary system. Intermediate resolution spectra have been taken during four nights (2 5 April 2001) using the IDS spectrograph of the 2.5 m Isaac Newton Telescope (INT) (La Palma, Canary Islands, Spain). The V1054 Oph spectra show very strong emission lines even in its quiescent state. The analysis of the temporal evolution of the observed emission lines (from Hβ to H11 and the Ca II H and K lines) reveals four strong flares and several weak flares. We have studied in detail the behaviour of the chromospheric lines during the different phases (pre-flare, impulsive and gradual decay) of these flares. The observed flares last from ˜25 to 95 min. The equivalent width of the Hβ line changes by a factor up to ˜2.3. Broad wings and asymmetric (red-shifted) lines are observed as well.
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