The massive multiple system HD 64315
J. Lorenzo, S. Simon-Diaz, I. Negueruela, F. Vilardell, M. Garcia, C., J. Evans, and D. Montes

TL;DR
HD 64315 is a complex multiple star system with at least two binary components, including a rare overcontact binary, providing insights into high-mass star formation and multiplicity.
Contribution
This study reveals the detailed multiplicity and orbital parameters of HD 64315, including the discovery of an overcontact binary and its potential as a merger progenitor.
Findings
HD 64315 consists of two binary systems separated by 0.09 arcsec.
The eclipsing binary has a period of about 1.02 days with nearly identical 14.6 M$_\odot$ stars.
The non-eclipsing binary has a period of about 2.71 days with component masses around 10.2 and 10.8 M$_\odot$.
Abstract
The O6 Vn star HD 64315 is believed to belong to the star-forming region known as NGC 2467, but previous distance estimates do not support this association. We explore the multiple nature of this star with the aim of determining its distance, and understanding its connection to NGC 2467. A total of 52 high-resolution spectra have been gathered over a decade. We use their analysis, in combination with the photometric data from All Sky Automated Survey and Hipparcos catalogues, to conclude that HD 64315 is composed of at least two spectroscopic binaries, one of which is an eclipsing binary. HD 64315 contains two binary systems, one of which is an eclipsing binary. The two binaries are separated by 0.09 arcsec (or 500 AU) if the most likely distance to the system, around 5 kpc, is considered. The presence of fainter companions is not excluded by current observations. The non-eclipsing…
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