HD 103774

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HD 103774
Observation data
Epoch J2000.0      Equinox J2000.0
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
Distance184.3 ± 0.6 ly
(56.5 ± 0.2 pc)
Absolute magnitude (MV)3.41[2]
Details
Mass1.38±0.01[4] M☉
Radius1.56±0.03[4] R☉
Luminosity3.7±0.1[4] L☉
Surface gravity (log g)4.183±0.002[4] cgs
Temperature6,391±27[4] K
Metallicity [Fe/H]0.29[5] dex
Rotational velocity (v sin i)7.95[5] km/s
Age2.0±0.1 Gyr[4]
1.05±0.64 Gyr[6]
0.26[5] Gyr
Other designations
BD−11°3211, HD 103774, HIP 58263, SAO 157002, PPM 225148
Database references
SIMBADdata
Exoplanet Archivedata
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 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]

The HD 103774 planetary system[6]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
>0.367 ± 0.022 MJ 0.07 ± 0.001 5.8881 ± 0.0005 0.09 ± 0.04 — —

References[]

  1. ^ a b c d e f g 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 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, 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. ^ a b c d e f g Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692. A5.
  5. ^ a b c d Delgado Mena, E.; et al. (April 2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics. 576: 24. arXiv:1412.4618. Bibcode:2015A&A...576A..69D. doi:10.1051/0004-6361/201425433. A69.
  6. ^ a b c d 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. arXiv:1301.2741. Bibcode:2013A&A...551A..59L. doi:10.1051/0004-6361/201220415. S2CID 116916728. A59.
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