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Omicron Virginis
Omicron Virginis (ο Vir, ο Virginis) is a binary star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of +4.12. Based upon parallax measurements, it is at a distance of 163 light years.
The components are orbiting around the system's center of mass at a period of 50.7 years, and a nearly circular orbit with eccentricity 0.12 and an average separation of 21 astronomical units.
The primary star is a G-type giant with a stellar classification of G8 IIIa CN-1Ba1CH1. This indicates that it is a Barium star. It is around 11 times larger than the Sun. Although it is slightly cooler, it is radiating about 57 times the luminosity of the Sun. It is over twice as massive as the Sun and is around a billion years old. A simplified statistical analysis suggests that ο Virginis is likely to be a red-giant branch star fusing hydrogen in a shell around an inert helium core, but there is about a 22% chance that it is a horizontal branch star fusing helium in its core.
The secondary is a white dwarf with 94% of the Sun's mass. It contamined the surface of the giant primary with s-process elements when it was on the asymptotic giant branch, causing it to be a Barium star. It may also explain the unexpected SiIV emission flux coming from Omicron Virginis.
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Omicron Virginis
Omicron Virginis (ο Vir, ο Virginis) is a binary star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of +4.12. Based upon parallax measurements, it is at a distance of 163 light years.
The components are orbiting around the system's center of mass at a period of 50.7 years, and a nearly circular orbit with eccentricity 0.12 and an average separation of 21 astronomical units.
The primary star is a G-type giant with a stellar classification of G8 IIIa CN-1Ba1CH1. This indicates that it is a Barium star. It is around 11 times larger than the Sun. Although it is slightly cooler, it is radiating about 57 times the luminosity of the Sun. It is over twice as massive as the Sun and is around a billion years old. A simplified statistical analysis suggests that ο Virginis is likely to be a red-giant branch star fusing hydrogen in a shell around an inert helium core, but there is about a 22% chance that it is a horizontal branch star fusing helium in its core.
The secondary is a white dwarf with 94% of the Sun's mass. It contamined the surface of the giant primary with s-process elements when it was on the asymptotic giant branch, causing it to be a Barium star. It may also explain the unexpected SiIV emission flux coming from Omicron Virginis.