Bibcode
Sabin-Sanjulian, C.
Referencia bibliográfica
Massive Stars: From α to Ω, held 10-14 June 2013 in Rhodes, Greece; Online at http://a2omega-conference.net, id.96
Advertised on:
6
2013
Número de citas
0
Número de citas referidas
0
Descripción
O Vz stars are defined as those O-type stars displaying HeII 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 47 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
automatic tool, a fast, accurate and objective automatic method 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 the O
Vz phenomenon is a natural consecuence of the combination of stellar
parameters and it does not reflect a differencial characteristic in age,
gravity, proximity to ZAMS or wind-strength, when compared to O V stars
from the same region.