Journal Article

The pre-main-sequence star HD 34282: a very short-period δ Scuti-type pulsator

P. J. Amado, A. Moya, J. C. Suárez, S. Martín-Ruiz, R. Garrido, E. Rodríguez, C. Catala and M. J. Goupil

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 352, issue 2, pages L11-L15
Published in print August 2004 | ISSN: 0035-8711
Published online August 2004 | e-ISSN: 1365-2966 | DOI:
The pre-main-sequence star HD 34282: a very short-period δ Scuti-type pulsator

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HD 34282 has been found to pulsate during a systematic search for short-term photometric variability in Herbig Ae/Be stars with the goal of determining the position and size of the pre-main-sequence instability strip. Simultaneous Strömgren photometry is used in the frequency analysis, yielding two frequencies with values of ν1= 79.5 and ν2= 71.3 cycle d−1. The light curve with the largest amplitude is that of the u band. This behaviour, which is not common for δ Scuti stars, is explained as pulsation in a high radial order in stars near the blue edge of the instability strip. The main period, with a value of 18.12 min, represents the shortest period observed so far for a δ Scuti-type pulsator. A seismic modelling, including instability predictions and rotation effects, has been attempted. It is found that both main-sequence and pre-main-sequence models predict modes in the range of 56 to 82 cycle d−1 (between 648 and 949 μHz), corresponding to oscillations of radial order n from 6 to 8. The highest of the observed frequencies only becomes unstable for models of low metallicity, in agreement with results from spectroscopic measurements.

Keywords: stars: individual: HD 34282; stars: oscillations; stars: pre-main-sequence; δ Scuti

Journal Article.  2863 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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