Pulsations in pre-Main Sequence stars: The case of HD 34282

Details Pulsations in pre-Main Sequence stars: The case of HD 34282 Pulsations in pre-Main Sequence stars: The case of HD 34282

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..224..863a&link_type=abstract

The A-Star Puzzle, held in Poprad, Slovakia, July 8-13, 2004. Edited by J. Zverko, J. Ziznovsky, S.J. Adelman, and W.W. Weiss,

Computer Science

3

Stars: Early-Type, Stars: Emission-Line Ae, Stars: Fundamental Parameters, Stars: Individual: (Hd 34282), Stars: Oscillations, Stars: Pre-Main-Sequence, Δ Scuti.

Scientific paper

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 main period, with a value of 18.12 min, represents the shortest period observed up to now for a δ Scuti-type pulsator. A preliminary seismic modelling, including instability predictions and rotation effects, has been attempted. 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 mode identification is not discriminating due to the large error bars attached to the data, therefore, all possible non-radial and radial modes up to ℓ = 3 are compatible with the observed oscillations.

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