The nature of the high Galactic latitude O-star HD 93521: new results from X-ray and optical spectroscopy
Abstract
Context. Owing to its unusual location and its isolation, the nature of the high Galactic latitude O9.5 Vp object HD 93521 is still uncertain.
Aims: We have collected X-ray and optical observations to characterize the star and its surroundings.
Methods: X-ray images and spectra are analysed to search for traces of a recent star formation event around HD 93521 and to search for the signature of a possible compact companion. Optical echelle spectra are analysed with plane-parallel model atmosphere codes, assuming either a spherical star or a gravity darkened rotationally flattened star, to infer the effective temperature and surface gravity, and to derive the He, C, N and O abundances of HD 93521.
Results: The X-ray images reveal no traces of a population of young low-mass stars coeval with HD 93521. The X-ray spectrum of HD 93521 is consistent with a normal late O-type star although with subsolar metallicity. No trace of a compact companion is found in the X-ray data. In the optical spectrum, He and N are found to be overabundant, in line with the effect of rotational mixing in this very fast rotator, whilst C and O are subsolar. A critical comparison with the properties of subdwarf OB stars, indicates that, despite some apparent similarities, HD 93521 does not belong to this category.
Conclusions: Despite some ambiguities on the runaway status of the star, the most likely explanation is that HD 93521 is a Population I massive O-type star that was ejected from the Galactic plane either through dynamical interactions or a result of a supernova event in a binary system.
- Publication:
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Astronomy and Astrophysics
- Pub Date:
- October 2012
- DOI:
- 10.1051/0004-6361/201219865
- arXiv:
- arXiv:1209.2606
- Bibcode:
- 2012A&A...546A..77R
- Keywords:
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- stars: early-type;
- stars: fundamental parameters;
- stars: abundances;
- stars: massive;
- stars: individual: HD 93521;
- X-rays: stars;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- Accepted for publication in Astronomy &