A new investigation of the binary HD 48099

TL;DR

This study provides a comprehensive spectroscopic analysis of the binary system HD 48099, revealing detailed stellar parameters, spectral classifications, and wind properties, and offers a new orbital solution based on long-term observations.

Contribution

The paper introduces a new orbital solution and detailed stellar parameters for HD 48099 using long-term spectroscopic data and advanced modeling techniques.

Findings

HD 48099 is an O5.5 V((f))+O9 V binary with low orbital inclination.

The primary star is a fast rotator with a strongly clumped wind.

The primary's nitrogen abundance is about 8 times solar.

Abstract

With an orbital period of about 3.078 days, the double-lined spectroscopic binary HD 48099 is, still 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 IUE spectra. This investigation reveals that HD 48099 is an O5.5 V((f))+O9 V binary with M_1 sin^3 i = 0.70 M_{\sun} and M_2 sin^3 i = 0.39 M_{\sun}, implying a rather low orbital inclination. This result, combined with both a large effective temperature and log g, suggests that the primary star (v sini ~ 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.