A New Investigation of the Binary HD 48099

With an orbital period of about 3.078 days, the double-lined spectroscopic binary HD 48099 is, until now, the only short-period O+O system known in the Mon OB2 association. Even though an orbital solution has already been derived for this system, few information are available about the individual st...

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Bibliographic Details
Published in:The Astrophysical journal 2010-01, Vol.708 (2), p.1537-1544
Main Authors: Mahy, L, Rauw, G, Martins, F, Nazé, Y, Gosset, E, De Becker, M, Sana, H, Eenens, P
Format: Article
Language:English
Subjects:
ABUNDANCE
Astronomy
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
ATMOSPHERES
Aérospatiale, astronomie & astrophysique
binaries: spectroscopic
CLASSIFICATION
Earth, ocean, space
ELECTROMAGNETIC RADIATION
ELEMENTS
Exact sciences and technology
INCLINATION
NITROGEN
NONMETALS
Physical, chemical, mathematical & earth Sciences
Physique, chimie, mathématiques & sciences de la terre
RADIATIONS
Space science, astronomy & astrophysics
SPECTRA
STARS
stars: fundamental parameters
stars: individual: HD 48099
ULTRAVIOLET RADIATION
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Summary:With an orbital period of about 3.078 days, the double-lined spectroscopic binary HD 48099 is, until now, the only short-period O+O system known in the Mon OB2 association. Even though an orbital solution has already been derived for this system, few information are available about the individual stars. We present, in this paper, the results of a long-term spectroscopic campaign. We derive a new orbital solution and apply a disentangling method to recover the mean spectrum of each star. To improve our knowledge concerning both components, we determine their spectral classifications and their projected rotational velocities. We also constrain the main stellar parameters of both stars by using the CMFGEN atmosphere code and provide the wind properties for the primary star through the study of International Ultraviolet Explorer spectra. This investigation reveals that HD 48099 is an O5.5 V ((f)) + O9 V binary with M 1sin3 i = 0.70 M and M 2sin3 i = 0.39 M, implying a rather low orbital inclination. This result, combined with both a large effective temperature and log g, suggests that the primary star (vsin i 91 km s-1) is actually a fast rotator with a strongly clumped wind and a nitrogen abundance of about 8 times the solar value.
ISSN:0004-637X
1538-4357
1538-4357
DOI:10.1088/0004-637X/708/2/1537