HD 104067

Coordinates: Sky map 11h 59m 10.0100s, −20° 21′ 13.609″
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HD 104067
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corvus
Right ascension 11h 59m 10.00884s[1]
Declination −20° 21′ 13.6121″[1]
Apparent magnitude (V) 7.92[2]
Characteristics
Spectral type K3V[3]
Apparent magnitude (B) 8.894[2]
Apparent magnitude (J) 6.212±0.019[2]
Apparent magnitude (H) 5.754±0.023[2]
Apparent magnitude (K) 5.614±0.024[2]
B−V color index 0.974±0.010[2]
Astrometry
Radial velocity (Rv)+14.89±0.12[1] km/s
Proper motion (μ) RA: 141.706 mas/yr[1]
Dec.: −423.780 mas/yr[1]
Parallax (π)49.1470 ± 0.0235 mas[1]
Distance66.36 ± 0.03 ly
(20.347 ± 0.010 pc)
Absolute magnitude (MV)6.30[2]
Details
Mass0.818+0.024
−0.025[4] M☉
Radius0.771+0.007
−0.006[4] R☉
Luminosity0.307[5] L☉
Surface gravity (log g)4.56±0.10[6] cgs
Temperature4,942±14[4] K
Metallicity [Fe/H]0.11±0.06[6] dex
Rotation18.3±4.9 d[6]
Rotational velocity (v sin i)2.47±0.96[4] km/s
Age4.8+3.3
−3.0[4] Gyr
Other designations
BD−19°3382, GJ 1153, HD 104067, HIP 58451, SAO 180353, PPM 259710, LTT 4461, NLTT 29176[7]
Database references
SIMBADdata
Exoplanet Archivedata

HD 104067 is a star with a planetary system in the southern constellation of Corvus. It has an apparent visual magnitude of 7.92[2] which is too faint to be visible with the naked eye. The distance to this star is 66.4 light-years (20.4 parsecs) based on parallax. It is drifting further away with a radial velocity of +15 km/s.[1]

This is an ordinary K-type main-sequence star with a stellar classification of K3V.[3] It is a moderately active star[8] with an age of roughly five billion years. HD 104067 is spinning with a projected rotational velocity of 2.5 km/s,[4] giving it a rotation period of approximately a month.[3] The star has 82% of the mass and 77% of the radius of the Sun.[4] It is radiating 31%[5] of the Sun's luminosity from its photosphere at an effective temperature of 4,942 K. The metal content of this star is close to that in the Sun.[4]

Planetary system[edit]

HD 104067 has been observed as part of the HARPS planet-finding survey since 2004. The detection of an exoplanetary companion using the radial velocity method was announced in 2011. This sub-Saturn planet, HD 104067 b, has at least 0.2 times the mass of Jupiter and takes 55.8 days to orbit the star at a distance of 0.26 AU.[8] The discovery of a second, Uranus-mass planet, HD 104067 c, was announced in 2024 based on HARPS and HIRES data. TESS observations also show evidence of a third candidate planet, slightly larger than Earth and orbiting closer to the star than the other two planets, with a period of just 2.2 days. Modeling suggests that this inner planet candidate may experience significant tidal heating.[6]

The HD 104067 planetary system[6]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
TOI-6713.01 (unconfirmed) — 0.03054(37) 2.1538197(41) — 86.5±2.0° 1.30±0.12 R🜨
c ≥13.2±1.9 M🜨 0.1058±0.0013 13.8992+0.0047
−0.0037 		0.29+0.12
−0.13 		— —
b ≥62.1+3.3
−3.2 M🜨 		0.2674+0.0032
−0.0033 		55.851±0.017 0.123+0.048
−0.051 		— —

See also[edit]

References[edit]

  1. ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 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 c Suárez Mascareño, A.; et al. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv:1506.08039. Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441. S2CID 119181646.
  4. ^ a b c d e f g h Soto, M. G.; Jenkins, J. S. (2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy and Astrophysics. 615: A76. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. S2CID 119107228.
  5. ^ a b 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.
  6. ^ a b c d e Kane, Stephen R.; Fetherolf, Tara; et al. (March 2024). "A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World". The Astronomical Journal. arXiv:2403.17062.
  7. ^ "HD 104067". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-09-28.
  8. ^ a b Ségransan, D.; et al. (2011). "The HARPS search for southern extra-solar planets. XXIX. Four new planets in orbit around the moderately active dwarfs HD 63765, HD 104067, HD 125595, and HIP 70849". Astronomy and Astrophysics. 535. A54. arXiv:1107.0339. Bibcode:2011A&A...535A..54S. doi:10.1051/0004-6361/200913580. S2CID 119197766.


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