Open AccessObservations of the pulsating subdwarf B star Feige 48: Constraints on evolution and companions
Author(s) -
Reed M. D.,
Kawaler S. D.,
Zola S.,
Jiang X. J.,
Dreizler S.,
Schuh S. L.,
Deetjen J. L.,
Kalytis R.,
Meištas E.,
Janulis R.,
Ališauskas D.,
Krzesiński J.,
Vuckovic M.,
Moskalik P.,
Ogłoza W.,
Baran A.,
Stachowski G.,
Kurtz D. W.,
González Pérez J. M.,
Mukadam A.,
Watson T. K.,
Koen C.,
Bradley P. A.,
Cunha M. S.,
Kilic M.,
Klumpe E. W.,
Carlton R. F.,
Handler G.,
Kilkenny D.,
Riddle R.,
Dolez N.,
Vauclair G.,
Chevreton M.,
Wood M. A.,
Grauer A.,
Bromage G.,
Solheim J. E.,
Østensen R.,
Ulla A.,
Burleigh M.,
Good S.,
Hürkal Ö.,
Anderson R.,
Pakstiene E.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.07438.x
Subject(s) - physics , subdwarf , astrophysics , stars , amplitude , astronomy , star (game theory) , mode (computer interface) , stellar evolution , white dwarf , quantum mechanics , computer science , operating system
Since pulsating subdwarf B (sdBV or EC14026) stars were first discovered, observational efforts have tried to realize their potential for constraining the interior physics of extreme horizontal branch stars. Difficulties encountered along the way include uncertain mode identifications and a lack of stable pulsation mode properties. Here we report on Feige 48, an sdBV star for which follow‐up observations have been obtained spanning more than four years. These observations show some stable pulsation modes. We resolve the temporal spectrum into five stable pulsation periods in the range 340–380 s with amplitudes less than 1 per cent, and two additional periods that appear in one data set each. The three largest amplitude periodicities are nearly equally spaced, and we explore the consequences of identifying them as a rotationally split ℓ= 1 triplet by consulting a representative stellar model. The general stability of the pulsation amplitudes and phases allows us to use the pulsation phases to constrain the time‐scale of evolution for this sdBV star. Additionally, we are able to place interesting limits on any stellar or planetary companion to Feige 48.