Bibcode
Sabín-Sanjulián, C.; Simón-Díaz, S.; Herrero, A.; García, M.; Vlt-Flames Tarantula Survey Collaboration
Referencia bibliográfica
Highlights of Spanish Astrophysics VII, Proceedings of the X Scientific Meeting of the Spanish Astronomical Society (SEA), held in Valencia, July 9 - 13, 2012, Eds.: J.C. Guirado, L.M. Lara, V. Quilis, and J. Gorgas., pp.623-627
Advertised on:
5
2013
Número de citas
0
Número de citas referidas
0
Descripción
O Vz stars are defined as those O-type stars displaying He II 4686
absorption line stronger than other He line in the blue spectral region.
These stars have been hypothesized on spectroscopic grounds to be O-type
stars on or close to the Zero-Age-Main-Sequence (ZAMS), also having
weaker winds than normal O V stars. We have tested these hypothesis by
performing a quantitative spectroscopic analysis of a sample of 37 O Vz
(plus 49 O V stars used for comparison) discovered by the VLT-FLAMES
Tarantula Survey (VFTS) in the 30 Doradus region within the Large
Magellanic
Cloud. To this aim, we have used the IACOB grid based tool, a fast,
accurate and objective automatic tool to determine the stellar and wind
parameters of large samples of O stars in a reasonable amount of time. A
first inspection of the resulting physical properties of the O Vz stars
in 30 Dor is presented here. The main outcome from our quantitative
spectroscopic analysis is that O Vz stars in 30 Dor are not particularly
closer to the ZAMS, nor necessarily have weaker winds when compared to
normal O V stars in the same region.