The pre-main sequence star HD 34282: A very short period delta Scuti-type pulsator

Details The pre-main sequence star HD 34282: A very short period delta Scuti-type pulsator The pre-main sequence star HD 34282: A very short period delta Scuti-type pulsator

2004-06-04

arxiv.org/abs/astro-ph/0406110v1

Mon.Not.Roy.Astron.Soc. 352 (2004) L11

Astronomy and Astrophysics

Astrophysics

5 pages, 5 figures, Accepted by MNRAS

Scientific paper

10.1111/j.1365-2966.2004.08116.x

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 Stromgren photometry is used in the frequency analysis, yielding two frequencies with values of nu1=79.5 and nu2=71.3 c/d. The light curve with the largest amplitude is that of the u band. This behaviour, which is not common for delta 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 delta 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 c/d (between 648 and 949 microHz), 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.

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