70 Virginis b
The exoplanet 70 Virginis b (min mass ~7.5 MJ) as rendered by Celestia
Discovery
Discovered byGeoffrey Marcy
R. Paul Butler
Discovery site United States
Discovery date17 January 1996[1]
Doppler Spectroscopy
Orbital characteristics
0.484 ± 0.028 AU (72,400,000 ± 4,200,000 km)
Eccentricity0.4007 ± 0.0035
116.6884 ± 0.0044 d
2,447,239.82 ± 0.21
358.71 ± 0.54
Semi-amplitude316.3 ± 1.7
Star70 Virginis

    70 Virginis b (abbreviated 70 Vir b) is an extrasolar planet approximately 60 light-years away in the constellation of Virgo. Announced in 1996 by Geoffrey Marcy and R. Paul Butler, 70 Virginis was one of the first stars confirmed to have planets orbiting it.[2] When first announced, 70 Virginis b was considered to be within its star's habitable zone (preferably in the "Goldilocks zone"), but it was later confirmed that the planet has an eccentric orbit, closer to its parent.

    Characteristics

    Radial velocity changes over time of 70 Virginis caused by the orbit of 70 Virginis b.

    70 Virginis b is a gas giant extrasolar planet that is 7.4 times the mass of Jupiter and is in an eccentric 116-day orbit about its host. Its surface gravity is expected to be about six to eight times that of Jupiter's. At the time of discovery in January 1996, it was believed that the star was only 29 ly away resulting in the star being less luminous based on its apparent magnitude. As a result, the planet's orbit was thought to be in the habitable zone and the planet was nicknamed Goldilocks (not too cold or too hot).[3]

    The Hipparcos satellite later showed that the star was more distant from Earth and therefore brighter resulting in the planet being too hot to be in the habitable zone.[4]

    A significant update to the 70 Virginis system revised the orbit of the planet and used interferometry to show that, although the host star is similar in mass and temperature to the Sun, it is almost twice the radius of the Sun.[5] The accuracy of these stellar parameters allowed the Habitable Zone to be calculated much more precisely, and orbital dynamics simulations show that a terrestrial planet can retain a stable orbit in the Habitable Zone despite the presence of the nearby eccentric giant planet.

    See also

    References

    1. ↑ Sanders, Robert (January 17, 1996). "Discovery of two new planets -- the second and third within the last three months -- proves they aren't rare in our galaxy" (Press release). University of California, Berkeley. Retrieved December 22, 2017.
    2. ↑ Marcy, Geoffrey W.; Butler, R. Paul (1996). "A Planetary Companion to 70 Virginis". The Astrophysical Journal Letters. 464 (1): L147–L151. Bibcode:1996ApJ...464L.147M. doi:10.1086/310096. S2CID 9528214.
    3. ↑ Powell, Corey (1996-05-27). "A Parade of New Planets". Scientific American. Retrieved 2007-05-13.
    4. ↑ Perryman, M. A. C.; et al. (1996). "Hipparcos distances and mass limits for the planetary candidates: 47 Ursae Majoris, 70 Virginis, 51 Pegasi". Astron. Astrophys. 310: L21–L24. Bibcode:1996A&A...310L..21P.
    5. ↑ Kane, Stephen R.; et al. (2015). "A Comprehensive Characterization of the 70 Virginis Planetary System". The Astrophysical Journal. 806 (1): 60. arXiv:1504.04066. Bibcode:2015ApJ...806...60K. doi:10.1088/0004-637X/806/1/60. S2CID 42414832.


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