The evolution of the helium star sigma orionis E

view Abstract Citations (6) References (11) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS The evolution of the helium star Sigma Orionis E. Odell, A. P. Abstract The helium-rich star sigma Ori E is a member of the quintuple star sigma Ori. The visual binary AB has recently been studied by Heintz, and a solution to its orbit and a distance was determined. It is shown that this new distance to the system resolves the problem of too large a mass for the helium star, and allows helium-rich models to approximate the present star. The upper age to the star is 10 m.y., and with a mass of less than 5 solar masses the star must have been formed with a large helium abundance. It is unlikely that component E is the result of binary mass transfer. It is difficult to understand the star in terms of mass loss from a very massive star. The idea that an original single star broke up into five stars is attractive to the time scale, but the angular momentum of the present system is very large. Alternatively, the system might have resulted from the capture of E, an old star which has been completely mixed through its evolution. Publication: The Astrophysical Journal Pub Date: December 1974 DOI: 10.1086/153285 Bibcode: 1974ApJ...194..645O Keywords: Abundance; Astronomical Models; Helium; Stellar Evolution; Angular Momentum; Mass Transfer; Orion Constellation; Stellar Mass Ejection; Stellar Rotation; Astrophysics full text sources ADS | data products SIMBAD (2)