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Observational asteroseismology of hot subdwarf stars
Author(s) -
Østensen R.H.
Publication year - 2010
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201011450
Subject(s) - asteroseismology , subdwarf , photometry (optics) , stars , physics , astrophysics , astronomy , observational study , white dwarf , mathematics , statistics
Hot subdwarf stars are particularly challenging for asteroseismology due to their rapid pulsation periods, intrinsic faintness and relative rarity both in the field and in clusters. These features have ensured that the preferred method of observation up to now has been white‐light photometry, and all asteroseismological solutions to date have been made by model fitting of the frequency spectrum. Several attempts have been made to perform asteroseismology using time‐resolved spectroscopy on the brightest of these stars, but with modest results. A few attempts at simultaneous multi‐color photometry have also been made to identify modes with the amplitude ratio method. We will review the most recent observational results and progress in improving the observational methods for ground‐based asteroseismology of these compact pulsators (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)