HD 4113

HD 4113 is a dual star system in the southern constellation of Sculptor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.88.[2] The distance to this star, as estimated by parallax measurements, is 137 light years.[1] It is receding away from the Sun with a radial velocity of +5 km/s.[1]

HD 4113
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Sculptor
Right ascension 00h 43m 12.5957s[1]
Declination –37° 58′ 57.4794″[1]
Apparent magnitude (V) 7.880±0.013 and 12.70±0.02[2]
Characteristics
Spectral type G5V and M0–1V[2]
B−V color index 0.716±0.003[2]
Astrometry
Radial velocity (Rv)+5.13±0.12[1] km/s
Proper motion (μ) RA: +49.344±0.062[1] mas/yr
Dec.: −114.176±0.051[1] mas/yr
Parallax (π)23.8531 ± 0.0536[1] mas
Distance136.7 ± 0.3 ly
(41.92 ± 0.09 pc)
Absolute magnitude (MV)4.780±0.046 and 9.600±0.049[2]
Details[3]
A
Mass1.02+0.02
−0.03 M☉
Radius1.08+0.02
−0.04[1] R☉
Luminosity1.085+0.04
−0.03[1] L☉
Surface gravity (log g)4.31±0.04 cgs
Temperature5,638±50 K
Metallicity [Fe/H]0.20±0.04 dex
Rotational velocity (v sin i)2.324[2] km/s
Age7.29+1.91
−1.46 or 5.0+1.3
−1.7[2] Gyr
B
Mass0.55[2] M☉
Surface gravity (log g)4.76[2] cgs
Temperature3,833[2] K
Other designations
CD−38°223, GC 858, HD 4113, HIP 3391, SAO 192693, GSC 03654-02131[4]
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

The primary member of this system, component A, is a Sun-like G-type main-sequence star with a stellar classification of G5V.[2] Estimates of its age are five[2] to seven[3] billion years old, and it is spinning with a leisurely projected rotational velocity of 2.3 km/s.[2] The star is metal rich, with nearly the same mass,[3] radius, and luminosity[1] as the Sun.

Orbiting this star is a giant planet and a brown dwarf; the latter has been directly imaged. It also has a co-moving stellar companion, designated component B, which is a red dwarf with a class of M0–1V at an angular separation of 43″. This angle is equivalent to a projected separation of 2,000 AU.[2]

Planetary system

On 26 October 2007, Tamuz used the radial velocity method and found a planet with a minimum mass one and half times that of Jupiter orbiting at 1.28 AU away from HD 4113.

The HD 4113 planetary system[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥ 1.56±0.04 MJ 1.28 526.62±0.3 0.903±0.005 — —

See also

References
  1. 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. Cheetham, A.; et al. (June 2018). "Direct imaging of an ultracool substellar companion to the exoplanet host star HD 4113 A". Astronomy & Astrophysics. 614: 19. arXiv:1712.05217. Bibcode:2018A&A...614A..16C. doi:10.1051/0004-6361/201630136. S2CID 119084543. A16.
  3. Aguilera-Gómez, Claudia; et al. (June 2018). "Lithium abundance patterns of late-F stars: an in-depth analysis of the lithium desert". Astronomy & Astrophysics. 614: 15. arXiv:1803.05922. Bibcode:2018A&A...614A..55A. doi:10.1051/0004-6361/201732209. S2CID 62799777. A55.
  4. "HD 4113". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-04.
  5. Tamuz, O.; et al. (2008). "The CORALIE survey for southern extra-solar planets XV. Discovery of two eccentric planets orbiting HD 4113 and HD 156846". Astronomy and Astrophysics. 480 (3): L33–L36. arXiv:0710.5028. Bibcode:2008A&A...480L..33T. doi:10.1051/0004-6361:20078737. S2CID 11350536.

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