Astronomy:HD 102195

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Short description: Star in the constellation Virgo
HD 102195 / Flegetonte
Observation data
Equinox J2000.0]] (ICRS)
Constellation Virgo
Right ascension  11h 45m 42.29278s[1]
Declination +02° 49′ 17.3262″[1]
Apparent magnitude (V) 8.07[2]
Characteristics
Spectral type K0 V[3]
B−V color index 0.835[2]
Astrometry
Radial velocity (Rv)1.85±0.15[1] km/s
Proper motion (μ) RA: −188.735[1] mas/yr
Dec.: −113.403[1] mas/yr
Parallax (π)34.0560 ± 0.0555[1] mas
Distance95.8 ± 0.2 ly
(29.36 ± 0.05 pc)
Absolute magnitude (MV)5.76[2]
Details[4]
Mass0.88±0.03 M☉
Radius0.84±0.02 R☉
Luminosity0.49±0.01 L☉
Surface gravity (log g)4.53±0.03 cgs
Temperature5,283±29 K
Metallicity [Fe/H]+0.09[5] dex
Rotation12.3 d[6]
Rotational velocity (v sin i)2.6[2] km/s
Age5.9±3.5 Gyr
Other designations
BD+03°2549, HD 102195, HIP 57370, HR 4293, SAO 119033, LTT 13232, NLTT 28458[7]
Database references
SIMBADdata
Extrasolar Planets
Encyclopaedia		data

HD 102195 is an orange-hued star in the zodiac constellation of Virgo with a confirmed exoplanet companion.[2] With an apparent visual magnitude of 8.07,[2] the star is too faint to be seen with the naked eye. The distance to HD 102195 can be estimated from its annual parallax shift of 34.06 mas,[1] yielding 95.8 light years. It is moving further away from the Earth with a heliocentric radial velocity of 1.85 km/s.[1] This is a high proper motion star and a possible member of the η Cha stellar kinematic group.[8]

The star HD 102195 is named Flegetonte. The name was selected in the NameExoWorlds campaign by Italy, during the 100th anniversary of the IAU. Flegetonte is the underworld river of fire from Greek Mythology in the Italian narrative poem on the afterlife Divina Commedia.[9][10]

This K-type main-sequence star has a stellar classification of K0 V.[3] It is a quasi-periodic variable star with a cycle of 11.5 days, a variation range of 3.65%, and a phased amplitude of 94%.[11] HD 102195 is around six billion years old with a rotation period of 12.3 days.[6] It has 88% of the Sun's mass and 84% of the Sun's radius. It is radiating 49% of the Sun's luminosity from its photosphere at an effective temperature of 5,283 K.[4]

In 2005, an orbiting companion was detected using the Exoplanet Tracker instrument.[12] This near Jupiter-mass exoplanet has an orbital period of 4.1 days with a circular orbit. By comparing the rotation period and radius of the star with the projected rotational velocity, Melo et al. (2007) derived an orbital inclination of 47°. This would suggest a planetary mass of 0.62 Jupiter mass.[2]

The HD 102195 planetary system[2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b / Lete ≥0.45 MJ 0.0491[12] 4.113775±0.000557 0.0 (assumed) — —

See also

  • List of extrasolar planets

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Melo, C. et al. (May 2007). "A new Neptune-mass planet orbiting HD 219828". Astronomy and Astrophysics 467 (2): 721–727. doi:10.1051/0004-6361:20066845. Bibcode: 2007A&A...467..721M. 
  3. ↑ 3.0 3.1 Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey 5, Bibcode: 1999MSS...C05....0H. 
  4. ↑ 4.0 4.1 Bonfanti, A. et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics 585: 14. doi:10.1051/0004-6361/201527297. A5. Bibcode: 2016A&A...585A...5B. 
  5. ↑ Brewer, John M.; Fischer, Debra A.; Valenti, Jeff A.; Piskunov, Nikolai (2016). "Spectral Properties of Cool Stars: Extended Abundance Analysis of 1,617 Planet-Search Stars". The Astrophysical Journal Supplement Series 225 (2): 32. doi:10.3847/0067-0049/225/2/32. Bibcode: 2016ApJS..225...32B. 
  6. ↑ 6.0 6.1 Vidotto, A. A. et al. (July 2014). "Stellar magnetism: empirical trends with age and rotation". Monthly Notices of the Royal Astronomical Society 441 (3): 2361–2374. doi:10.1093/mnras/stu728. Bibcode: 2014MNRAS.441.2361V. 
  7. ↑ "HD 95370". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+95370. 
  8. ↑ Nakajima, Tadashi; Morino, Jun-Ichi (January 2012). "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun". The Astronomical Journal 143 (1): 2. doi:10.1088/0004-6256/143/1/2. Bibcode: 2012AJ....143....2N. 
  9. ↑ "Approved names" (in en). http://www.nameexoworlds.iau.org/final-results. 
  10. ↑ "International Astronomical Union | IAU". https://www.iau.org/news/pressreleases/detail/iau1912/. 
  11. ↑ Armstrong, D. J. et al. (July 2015). "K2 Variable Catalogue: Variable stars and eclipsing binaries in K2 campaigns 1 and 0". Astronomy & Astrophysics 579: 6. doi:10.1051/0004-6361/201525889. A19. Bibcode: 2015A&A...579A..19A. 
  12. ↑ 12.0 12.1 Ge, Jian et al. (2006). "The First Extrasolar Planet Discovered with a New-Generation High-Throughput Doppler Instrument". The Astrophysical Journal 648 (1): 683–695. doi:10.1086/505699. Bibcode: 2006ApJ...648..683G. 

Coordinates: Sky map 11h 45m 42.2920s, +02° 49′ 17.340″



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