Astronomy:HD 103774
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Corvus |
| Right ascension | 11h 56m 55.58949s[1] |
| Declination | −12° 6′ 28.4700″[1] |
| Apparent magnitude (V) | 7.13[2] |
| Characteristics | |
| Spectral type | F6 V[3] |
| B−V color index | 0.503±0.014[2] |
| Astrometry | |
| Radial velocity (Rv) | −3.19±0.17[1] km/s |
| Proper motion (μ) | RA: −124.888[1] mas/yr Dec.: −20.159[1] mas/yr |
| Parallax (π) | 17.6990 ± 0.0555[1] mas |
| Distance | 184.3 ± 0.6 ly (56.5 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.41[2] |
| Details | |
| Mass | 1.38±0.01[4] M☉ |
| Radius | 1.56±0.03[4] R☉ |
| Luminosity | 3.7±0.1[4] L☉ |
| Surface gravity (log g) | 4.183±0.002[4] cgs |
| Temperature | 6,391±27[4] K |
| Metallicity [Fe/H] | 0.29[5] dex |
| Rotational velocity (v sin i) | 7.95[5] km/s |
| Age | 2.0±0.1 Gyr[4] 1.05±0.64 Gyr[6] 0.26[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
HD 103774 is a star with a close orbiting planetary companion in the southern constellation of Corvus. With an apparent visual magnitude of 7.13,[2] it is too faint to be readily visible to the naked eye. Parallax measurements provide a distance estimate of 184 light years from the Sun. It is drifting closer with a radial velocity of −3 km/s.[1] The star has an absolute magnitude of 3.41.[2]
The stellar classification of HD 103774 is F6 V,[3] indicating this is an F-type main-sequence star that is generating energy through core hydrogen fusion. It is a young star with age estimates ranging from 260 million up to 2 billion years of age. The star is mildly active and is spinning with a projected rotational velocity of 8 km/s.[5] It has 1.4 times the mass and 1.56 times the radius of the Sun. The star is radiating 3.7 times the luminosity of the Sun from its photosphere at an effective temperature of 6,391 K.[4]
Planetary system
This star has been under observation as part of a survey using the HARPS spectrogram for a period of 7.5 years. In 2012, the detection of an exoplanetary companion using the radial velocity method was announced. This result was published in January 2013. The object is orbiting close to the host star at a distance of 0.07 astronomical unit|AU (10 Gm) with a period of just 5.9 days and an eccentricity (ovalness) of 0.09.[6] As the inclination of the orbital plane is unknown, only a lower limit on the mass can be determined; this lower bound is about equal to the mass of Saturn.
There is marginal evidence for an infrared excess at a wavelength of 12 μm, indicating the likely grain size. More measurements are needed to confirm this signal.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >0.367 ± 0.022 MJ | 0.07 ± 0.001 | 5.8881 ± 0.0005 | 0.09 ± 0.04 | — | — |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 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.
- ↑ 2.0 2.1 2.2 2.3 2.4 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey (Ann Arbor, Michigan: Department of Astronomy, University of Michigan) 5. Bibcode: 1999MSS...C05....0H.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Bonfanti, A. et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics 585: A5. doi:10.1051/0004-6361/201527297. A5. Bibcode: 2016A&A...585A...5B.
- ↑ 5.0 5.1 5.2 5.3 Delgado Mena, E. et al. (April 2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics 576: 24. doi:10.1051/0004-6361/201425433. A69. Bibcode: 2015A&A...576A..69D.
- ↑ 6.0 6.1 6.2 6.3 Lo Curto, G. et al. (2013). "The HARPS search for southern extrasolar planets: XXXVI. New multi-planet systems in the HARPS volume limited sample: a super-Earth and a Neptune in the habitable zone". Astronomy & Astrophysics 551: 7. doi:10.1051/0004-6361/201220415. A59. Bibcode: 2013A&A...551A..59L.
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