HD 102195
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas[1] |
| Distance | 95.8 ± 0.2 ly (29.36 ± 0.05 pc) |
| Absolute magnitude (MV) | 5.76[2] |
| Details[4] | |
| Mass | 0.88±0.03 M☉ |
| Radius | 0.84±0.02 R☉ |
| Luminosity | 0.49±0.01 L☉ |
| Surface gravity (log g) | 4.53±0.03 cgs |
| Temperature | 5,283±29 K |
| Metallicity [Fe/H] | +0.09[5] dex |
| Rotation | 12.3 d[6] |
| Rotational velocity (v sin i) | 2.6[2] km/s |
| Age | 5.9±3.5 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | 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 a separation of 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.[2] 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 MJ.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.45 MJ | 0.0491[12] | 4.113775±0.000557 | 0.0 (assumed) | — | — |
See also
References
- ^ a b c d e f g h 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.
- ^ a b c d e f g h i Melo, C.; et al. (May 2007). "A new Neptune-mass planet orbiting HD 219828". Astronomy and Astrophysics. 467 (2): 721–727. arXiv:astro-ph/0702459. Bibcode:2007A&A...467..721M. doi:10.1051/0004-6361:20066845.
- ^ a b Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
- ^ a b Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. A5.
- ^ 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. arXiv:1606.07929. Bibcode:2016ApJS..225...32B. doi:10.3847/0067-0049/225/2/32.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ a b 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. arXiv:1404.2733. Bibcode:2014MNRAS.441.2361V. doi:10.1093/mnras/stu728.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ "HD 95370". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-08-13.
- ^ 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. Bibcode:2012AJ....143....2N. doi:10.1088/0004-6256/143/1/2.
- ^ "Approved names". NameExoworlds. Retrieved 2020-01-02.
- ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
- ^ 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. arXiv:1502.04004. Bibcode:2015A&A...579A..19A. doi:10.1051/0004-6361/201525889. A19.
- ^ 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. arXiv:astro-ph/0605247. Bibcode:2006ApJ...648..683G. doi:10.1086/505699.
