HD_49674

HD 49674

HD 49674

Star in the constellation Auriga

HD 49674 is a solar-type star with an exoplanetary companion[7] in the northern constellation of Auriga. It has an apparent visual magnitude of 8.10[2] and thus is an eighth-magnitude star that is too faint to be readily visible to the naked eye. The system is located at a distance of 140.6 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +12 km/s.[1]

Quick Facts Observation data Epoch J2000 Equinox J2000, Constellation ...

HD 49674, and its planetary system, was chosen as part of the 2019 NameExoWorlds campaign organised by the International Astronomical Union, which assigned each country a star and planet to be named. HD 49674 was assigned to Belgium. The winning proposal named the star Nervia and the planet Eburonia, both after prominent Belgic tribes, the Nervii and Eburones, respectively.[8]

This is an ordinary G-type main-sequence star with a stellar classification of G3V,[3] which indicates it is generating energy through hydrogen fusion at its core. Spinning with a projected rotational velocity of 4.7 km/s,[5] it is younger than the Sun, roughly two billion years of age, and is a metal-rich star.[7] HD 49674 has a similar mass and radius as the Sun. It is radiating 96% of the Sun's luminosity from its photosphere at an effective temperature of 5,702 K.[4]

Planetary system

At the time of discovery of the planet HD 49674 b in 2002, it was the least massive planet known, very close to the boundary between sub-Jupiter mass and Neptune mass at 0.1 MJ. This planet orbits very close to the star, with a semimajor axis of 0.0580 AU (8.68 Gm).[9]

More information Companion (in order from star), Mass ...

See also

References

  1. [1]
    Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. [2]
    Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. [3]
    Grieves, N.; et al. (December 2018). "Chemo-kinematics of the Milky Way from the SDSS-III MARVELS survey". Monthly Notices of the Royal Astronomical Society. 481 (3): 3244–3265. arXiv:1803.11538. Bibcode:2018MNRAS.481.3244G. doi:10.1093/mnras/sty2431.
  4. [4]
    Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
  5. [5]
    Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal. 153 (1): 19. arXiv:1611.02897. Bibcode:2017AJ....153...21L. doi:10.3847/1538-3881/153/1/21. S2CID 119511744. 21.
  6. [6]
    "HD 49674". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-24.
  7. [7]
    Butler, R. Paul; et al. (2003). "Seven New Keck Planets Orbiting G and K Dwarfs". The Astrophysical Journal. 582 (1): 455–466. Bibcode:2003ApJ...582..455B. CiteSeerX 10.1.1.7.6988. doi:10.1086/344570. S2CID 17608922.
  8. [8]
    "Belgium". NameExoworlds. Retrieved 2019-12-22.
  9. [9]
    Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. hdl:2299/1103. S2CID 119067572.
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