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HD 63765

"Yvaga" redirects here. For the fictional planet, see Alien: Romulus.
HD 63765 / Tapecue
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Carina
Right ascension 07h 47m 49.720s[1]
Declination −54° 15′ 50.92″[1]
Apparent magnitude (V) 8.10[2]
Characteristics
Spectral type G9V[3]
Apparent magnitude (B) 8.845[2]
Apparent magnitude (J) 6.768±0.024[2]
Apparent magnitude (H) 6.442±0.027[2]
Apparent magnitude (K) 6.316±0.021[2]
B−V color index 0.745±0.012[2]
Astrometry
Radial velocity (Rv)22.1±0.2[2] km/s
Proper motion (μ) RA: 148.628 mas/yr[1]
Dec.: −278.753 mas/yr[1]
Parallax (π)30.7532 ± 0.0176 mas[1]
Distance106.06 ± 0.06 ly
(32.52 ± 0.02 pc)
Absolute magnitude (MV)5.49[2]
Details
Mass0.85±0.03[4] M☉
Radius0.84±0.02[4] R☉
Luminosity0.58±0.01[4] L☉
Surface gravity (log g)4.51±0.04[4] cgs
Temperature5,483±421[4] K
Metallicity [Fe/H]−0.16[5] dex
Rotation26.7±6.7 d[5]
Age7.2±3.6[4] Gyr
Other designations
CD−53°2007, HD 63765, HIP 38041, SAO 235521, PPM 336398, LTT 2952, NLTT 18486[6]
Database references
SIMBADdata
Exoplanet Archivedata

HD 63765 is a star with an orbiting exoplanet in the southern constellation of Carina. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 8.10.[2] The distance to this system is 106 light years based on parallax measurements, and it is drifting further away with a heliocentric radial velocity of 22 km/s.[2]

The star HD 63765 has the proper name 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.[7][8]

This is an ordinary G-type main-sequence star with a stellar classification of G9V.[3] It has 84% of the radius of the Sun and 85% of the Sun's mass.[4] The star is roughly seven billion[4] years old and is spinning with a rotation period of around 27 days.[5] It is considered to have a moderate level of magnetic activity in its chromosphere.[9] HD 63765 has lower iron abundance with approximately 69% of the Sun's iron-to-hydrogen ratio.[5] It is radiating 58% of the luminosity of the Sun from its photosphere at an effective temperature of 5,483 K.[4]

Planetary system

HD 63765 b is an extrasolar planet which orbits the star, first observed in 2006. This presumably gas giant 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.[9] The planet was announced in a press release dating from October 2009.

The HD 63765 planetary system[9]
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. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d e f g h i j 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. ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. ^ a b c d e f g h i 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. ^ a b c d 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.
  6. ^ "HD 63765". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-12-17.
  7. ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  8. ^ "Approved names". NameExoworlds. Retrieved 2020-01-02.
  9. ^ a b c 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.


Quelle: https://en.wikipedia.org/wiki/HD_63765_b