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HD 63765 is an 8th-magnitude G-type main sequence star located approximately 106 light years away in the constellation Carina. This star is smaller, cooler, dimmer, and less massive than the Sun, and has a lower iron content with approximately 69% of the Sun's iron-to-hydrogen ratio. In 2009, a gas giant planet was found in orbit around the star.

HD 63765
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Carina
Right ascension 07h 47m 49.719s[1]
Declination −54° 15′ 50.93″[1]
Apparent magnitude (V) 8.10
Characteristics
Spectral type G9V
Apparent magnitude (B) 8.85
Apparent magnitude (J) 6.768
Apparent magnitude (H) 6.442
Apparent magnitude (K) 6.316
B−V color index 0.75
Astrometry
Radial velocity (Rv)22.1 km/s
Proper motion (μ) RA: 147.67 ± 0.66[1] mas/yr
Dec.: −279.19 ± 0.71[1] mas/yr
Parallax (π)30.07 ± 0.56 mas[1]
Distance108 ± 2 ly
(33.3 ± 0.6 pc)
Absolute magnitude (MV)5.537
Details
Mass0.85 ± 0.03[2] M☉
Radius0.84 ± 0.02[2] R☉
Luminosity0.58 ± 0.01[2] L☉
Surface gravity (log g)4.51 ± 0.04[2] cgs
Temperature5483 ± 421[2] K
Metallicity [Fe/H]−0.16 dex
Rotation26.7±6.7 d[3]
Age7.2 ± 3.6[2] Gyr
Other designations
CD−53°2007, HIP 38041, LTT 2952, NLTT 18486, PPM 336398, SAO 235521
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

The star HD 63765 is named Tapecue. The name was selected by Bolivia during the 100th anniversary of the IAU as part of the IAU's NameExoWorlds project. Tapecue (modern Tapekue), literally 'eternal path' in Guarani, is the Milky Way through which the first inhabitants of the Earth arrived and could return. The planet HD 63765 b is named Yvaga. Yvága means 'sky' or 'heaven' in Guarani and the Milky Way was known as the road to yvága.[4][5] The planet HD 23079 b is named Guarani. A name selected by Brazil.


Planetary system


HD 63765 b is an extrasolar planet which orbits the star. This planet has at least 0.64 times the mass of Jupiter and takes 358 days to orbit the star at a semimajor axis of 0.94 AU.[6] The planet was announced in a press release dating from October 2009.

The HD 63765 planetary system[6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥0.64 ± 0.05 MJ 0.940 ± 0.016 358.0 ± 1.0 0.240 ± 0.043 — —

See also



References


  1. van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.Vizier catalog entry
  2. 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.
  3. Suárez Mascareño, A.; et al. (September 2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators", Monthly Notices of the Royal Astronomical Society, 452 (3): 2745–2756, arXiv:1506.08039, Bibcode:2015MNRAS.452.2745S, doi:10.1093/mnras/stv1441, S2CID 119181646.
  4. "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  5. "Approved names". NameExoworlds. Retrieved 2020-01-02.
  6. Ségransan, D.; et al. (2011). "The HARPS search for southern extra-solar planets. XXIX. Four new planets in orbit around the moderately active dwarfs HD 63765, HD 104067, HD 125595, and HIP 70849". Astronomy and Astrophysics. 535. A54. arXiv:1107.0339. Bibcode:2011A&A...535A..54S. doi:10.1051/0004-6361/200913580. S2CID 119197766.


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