HD 103197
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension 11h 52m 52.97822s[1]
Declination –50° 17′ 34.1592″[1]
Apparent magnitude (V) 9.40[2]
Characteristics
Spectral type K1V(p)[3]
Apparent magnitude (B) 10.26[2]
Apparent magnitude (J) 7.916±0.023[2]
Apparent magnitude (H) 7.600±0.051[2]
Apparent magnitude (K) 7.426±0.027[2]
B−V color index 0.860±0.023[2]
Astrometry
Radial velocity (Rv)−4.55±0.21[1] km/s
Proper motion (μ) RA: –80.938[1] mas/yr
Dec.: +7.188[1] mas/yr
Parallax (π)17.4700 ± 0.0294 mas[1]
Distance186.7 ± 0.3 ly
(57.24 ± 0.10 pc)
Absolute magnitude (MV)5.79[2]
Details
Mass0.90[4] M☉
Radius0.95±0.02[1] R☉
Luminosity0.566+0.002
−0.001[1] L☉
Surface gravity (log g)4.40±0.11[4] cgs
Temperature5,303±58[4] K
Metallicity [Fe/H]0.21±0.04[4] dex
Rotation51±5 d[4]
Rotational velocity (v sin i)0.602[5] km/s
Age4.872±4.294[5] Gyr
Other designations
CD−49°6573, HD 103197, HIP 57931, PPM 769972
Database references
SIMBADdata
Exoplanet Archivedata

HD 103197 is a star with a planetary companion in the southern constellation of Centaurus. It has an apparent visual magnitude of 9.40,[2] which is too faint to be viewed with the naked eye. Based on parallax measurements, HD 103197 is located at a distance of 187 light years from the Sun. It is drifting closer with a radial velocity of −4.6 km/s.[1]

This is a K-type main-sequence star with a stellar classification of K1V(p). In 1978, N. Houk noted that the cores of the star's H and K lines are weakly in emission; hence the 'p' code indicating a spectral peculiarity.[3] The star is an estimated five billion years old with a projected rotational velocity of approximately 0.6 km/s[5] and it appears to be very inactive. It has 90% of the mass and 95% of the radius of the Sun. Its metal content is five-eighths greater than in the Sun.[4]

In 2009, a gas giant exoplanet companion was discovered using the radial velocity method. This object is orbiting the host star at a distance of 0.249 AU (37.2 Gm) and a period of 47.84 d, with what is assumed to be a circular orbit.[4]

The HD 103197 planetary system[4]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥31.2 ± 2.0 M🜨 0.249 ± 0.004 47.84 ± 0.03 0.0(fixed) — —

See also

References

  1. ^ a b c d e f g h i 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.
  2. ^ a b c d e f g h 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 Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 2. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  4. ^ a b c d e f g h Mordasini, C.; et al. (2011). "The HARPS search for southern extrasolar planets XXIV. Companions to HD 85390, HD 90156, and HD 103197: a Neptune analog and two intermediate-mass planets". Astronomy and Astrophysics. 526. A111. arXiv:1010.0856. Bibcode:2011A&A...526A.111M. doi:10.1051/0004-6361/200913521. S2CID 59062607.
  5. ^ a b c Costa Silva, A. R.; et al. (February 2020). "Chemical abundances of 1111 FGK stars from the HARPS-GTO planet search sample. III. Sulfur". Astronomy & Astrophysics. 634: 10. arXiv:1912.08659. Bibcode:2020A&A...634A.136C. doi:10.1051/0004-6361/201936523. S2CID 209405391. A136.


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