HD 104067

Last updated
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]
Distance 66.36 ± 0.03  ly
(20.347 ± 0.010  pc)
Absolute magnitude  (MV)6.30 [2]
Details
Mass 0.818+0.024
−0.025 [4]   M☉
Radius 0.771+0.007
−0.006 [4]   R☉
Luminosity 0.307 [5]   L☉
Surface gravity (log g)4.56±0.10 [6]   cgs
Temperature 4,942±14 [4]   K
Metallicity [Fe/H]0.11±0.06 [6]   dex
Rotation 18.3±4.9 d [6]
Rotational velocity (v sin i)2.47±0.96 [4]  km/s
Age 4.8+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
SIMBAD data
Exoplanet Archive data

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]

Contents

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

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±0.001313.8992+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±0.0170.123+0.048
−0.051		——

See also

References

  1. 1 2 3 4 5 6 7 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. 1 2 3 4 5 6 7 8 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. 1 2 3 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. 1 2 3 4 5 6 7 8 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. 1 2 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. 1 2 3 4 5 Kane, Stephen R.; Fetherolf, Tara; et al. (March 2024). "A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World". The Astronomical Journal . 167 (5): 239. arXiv: 2403.17062 . Bibcode:2024AJ....167..239K. doi: 10.3847/1538-3881/ad3820 .
  7. ↑ "HD 104067". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-09-28.
  8. 1 2 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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