• Source: HD 216770

      • HD 216770 is a star with an orbiting exoplanet in the southern constellation of Piscis Austrinus. With an apparent visual magnitude of 8.11, it is too faint to be visible to the naked eye. It is located at a distance of 120 light years from the Sun, as determined by parallax measurements, and is drifting further away with a radial velocity of 31.1 km/s. The star shows a high proper motion, traversing the celestial sphere at an angular rate of 0.302 arcsec yr−1.
      The spectrum of HD 216770 presents as a late G-type main-sequence star, a yellow dwarf, with a stellar classification of G9VCN+1, where the suffix notation indicates anomalously strong band of CN. The star is smaller than the Sun, with 74% of the Sun's mass and 93% of the Sun's radius. It is about three billion years old and is spinning slowly with a rotation period of 35.6 days. The abundance of iron, a measure of the metallicity of the star, is higher than solar. The star is radiating 79% of the luminosity of the Sun from its photosphere at an effective temperature of 5,399 K.
      In 2003 an exoplanet was announced orbiting it by the Geneva Extrasolar Planet Search team. As the inclination of the orbital plane is unknown, only a lower bound on the mass of the object can be determined. It has at least 65% of the mass of Jupiter. The body has an eccentric orbit with a period of 118.5 days.


      See also


      HD 10647
      HD 108874
      HD 111232
      HD 142415
      HD 169830
      HD 41004
      HD 65216
      Lists of exoplanets


      References




      External links


      "Notes for star HD 216770". Extrasolar Planets Encyclopaedia. Archived from the original on June 2, 2006.

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