61 Virginis b

61 Virginis b (abbreviated 61 Vir b) is an extrasolar planet, orbiting the 5th magnitude G-type star 61 Virginis, in Virgo. This planet has a minimum mass of 5.1 times that of Earth and is an example of a super-Earth planet. It orbits very close to the star, at a distance of 0.050201 AU with an eccentricity of 0.12. This planet was discovered on 14 December 2009 using the radial velocity method taken at Keck and Anglo-Australian Observatories.[1][2]

61 Virginis b
Artist's impression of 61 Virginis b as a hot super-Earth, with some sporadic volcanic activity.
Discovery
Discovered byVogt et al.
Discovery siteKeck Observatory
Anglo-Australian Observatory
Discovery date14 December 2009
Radial velocity
Orbital characteristics
Apastron0.056163 AU
Periastron0.044239 AU
0.050201±0.000005 AU
Eccentricity0.12±0.11
4.2150±0.0006 d
101.16 h
130.01
2453369.166
105±54
Star61 Virginis
Physical characteristics
Mean radius
~1.6 R🜨
Mass≥ 5.1 M🜨
Temperature1,054 K (781 °C; 1,438 °F)

    Characteristics

    Mass, radius and temperature

    61 Virginis b is a super-Earth, an exoplanet with a radius and mass bigger than Earth, but smaller than that of the ice giants Neptune and Uranus. It has an equilibrium temperature of 1,054 K (781 °C; 1,438 °F).[3] It has an estimated minimum mass of around 5.1 M🜨, and a potential radius of 1.6 R🜨, based on its mass.

    Host star

    The planet orbits a (G-type) star named 61 Virginis, orbited by a total of three planets.[1] The star has a mass of 0.94 M☉ and a radius of 0.98 R☉. It has a temperature of 5531 K and is about 8.96 billion years old.[1] In comparison, the Sun is 4.6 billion years old[4] and has a temperature of 5778 K.[5] The star has slightly less metals then the Sun, with a metallicity ([Fe/H]) of −0.03, or 94% of the solar amount.[1] Its luminosity (L☉) is 80% that of the Sun.[1]

    The star's apparent magnitude, or how bright it appears from Earth's perspective, is 4.74. Therefore, it can be seen with the naked eye.

    Orbit

    61 Virginis b orbits its host star with an orbital period of 4.21 days at a distance of about 0.05 AU (compared to Mercury's from the Sun, which is 0.38 AU). It receives 296.5 times more sunlight that Earth does from the Sun.[3]

    The planet may be tidally locked meaning that there is a permanent day side and a permanent night side.

    Discovery

    The search for 61 Virginis b started when its host star was chosen an ideal target for a planet search using the radial velocity method (in which the gravitational pull of a planet on its star is measured by observing the resulting Doppler shift), as stellar activity would not overly mask or mimic Doppler spectroscopy measurements. It was also confirmed that 61 Virginis is neither a binary star nor a quickly rotating star, common false positives when searching for transiting planets.

    Analysis of the resulting data found that the radial velocity variations most likely indicated the existence of a planet.[1] The net result was an estimate of a 5.1 M🜨 planetary companion orbiting the star at a distance of 0.05 AU with an eccentricity of 0.12.

    An attempt to determine if the planet transits its host star using the Spitzer Space Telescope unfortunately failed due to technical issues related to the brightness of the star.[6]

    See also

    References
    1. Vogt, Steven (2010). "A Super-Earth and two Neptunes Orbiting the Nearby Sun-like star 61 Virginis". The Astrophysical Journal. 708 (2): 1366–1375. arXiv:0912.2599. Bibcode:2010ApJ...708.1366V. doi:10.1088/0004-637X/708/2/1366. S2CID 1979253.
    2. Tim Stephens (2009-12-14). "New planet discoveries suggest low-mass planets are common around nearby stars". UCSC News. UC Santa Cruz. Archived from the original on 23 December 2009. Retrieved 2009-12-14.
    3. "61 Vir b (G-Hot Spuerterran)". May 2014. Retrieved July 7, 2022.
    4. Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
    5. Fraser Cain (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
    6. Gillon, M.; et al. (2017). "The Spitzer search for the transits of HARPS low-mass planets. II. Null results for 19 planets". Astronomy and Astrophysics. 601. A117. arXiv:1701.01303. Bibcode:2017A&A...601A.117G. doi:10.1051/0004-6361/201629270. S2CID 86862862.
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