HD 101930
Template:Short description Template:Starbox begin Template:Starbox observe Template:Starbox character Template:Starbox astrometry Template:Starbox detail Template:Starbox catalog Template:Starbox reference Template:Starbox end
HD 101930, also known as Gliese 3683, is an orange hued star with an orbiting exoplanet located in the southern constellation Centaurus. It has an apparent magnitude of 8.21,<ref name = Anderson2012/> making it faintly visible in binoculars but not to the naked eye. The system is located relatively close at a distance of 98 light years<ref name = GaiaDR3/> but is receding with a heliocentric radial velocity of Template:Val.<ref name="Lovis2005"/> It has a relatively large proper motion, traversing the celestial sphere with an angular velocity of Template:Val·yr−1.<ref name=Luyten_1979/>
HD 101930 has a stellar classification of K2 V+,<ref name = Gray2006/> indicating that it is an ordinary K-type main-sequence star. It has a current mass of Template:Solar mass<ref name = Turnbull2015/> and is said to be 5.4 billion years old,<ref name="Bonfanti2015"/> which is slightly older than the Sun. The object has 87% the radius of the Sun<ref name = Stassun2019/> and an effective temperature of Template:Val.<ref name="Lovis2005"/> When combined, these parameters yield a luminosity 43% that of the Sun from its photosphere.<ref name="Bonfanti2015"/> As expected with planetary hosts, HD 101930 is metal enriched, having a metallicity 26% above solar levels.<ref name = Tsantaki2014/> The star's projected rotational velocity is similar to the Sun's, having a value of Template:Val.<ref name = LDA2021/>
A 2007 multicity survey found a co-moving companion located Template:Val away,<ref name = Mugrauer2007/> making it a binary star. It has a class of M0-1<ref name = Lindgren2016/> and a mass of Template:Solar mass.<ref name = Mugrauer2007/>
Planetary systemEdit
In 2005, the discovery of an exoplanet orbiting the star was announced. This is another discovery using the radial velocity method with the HARPS spectrograph. As the inclination of the orbital plane is unknown, only a lower bound on the mass can be determined. It has at least 30% of the mass of Jupiter.<ref name="Lovis2005"/>
Template:OrbitboxPlanet begin Template:OrbitboxPlanet Template:Orbitbox end
See alsoEdit
ReferencesEdit
External linksEdit
- {{#invoke:citation/CS1|citation
|CitationClass=web }}