Open AccessAn extremely slow nova?
Author(s) -
Whitelock Patricia,
Marang Freddy
Publication year - 2001
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 - 10.1046/j.1365-8711.2001.04441.x
Subject(s) - physics , supergiant , astrophysics , white dwarf , nova (rocket) , amplitude , variable star , astronomy , cataclysmic variable star , stars , optics , aeronautics , engineering
The binary companion to the peculiar F supergiant HD 172481 is shown to be a Mira variable with a pulsation period of 312 d. Its characteristics are within the normal range found for solitary Miras of that period, although its pulsation amplitude and mass‐loss rate Ṁ∼3×10 −6 M ⊙ yr −1 are higher than average. Reasons are given for suspecting that the F supergiant, which has L∼10 4 L ⊙ , is a white dwarf burning hydrogen accreted from its companion.