HD 46375
Observation data
Epoch J2000      Equinox J2000
Constellation Monoceros
Right ascension 06h 33m 12.62259s[1]
Declination +05° 27′ 46.5278″[1]
Apparent magnitude (V) 7.91[2]
Characteristics
Spectral type G9V[3] + M0V[4]
B−V color index 0.860[2]
Variable type Constant[5]
Astrometry
Radial velocity (Rv)−1.07±0.20[1] km/s
Proper motion (μ) RA: +111.477[1] mas/yr
Dec.: –96.918[1] mas/yr
Parallax (π)33.8088 ± 0.0435 mas[1]
Distance96.5 ± 0.1 ly
(29.58 ± 0.04 pc)
Absolute magnitude (MV)5.20[2]
Details
A
Mass0.91±0.01[6] M☉
Radius1.01±0.01[6] R☉
Luminosity0.77±0.01[6] L☉
Surface gravity (log g)4.38±0.01[6] cgs
Temperature3,663±15[7] K
Metallicity [Fe/H]+0.27±0.06[3] dex
Rotation42+9
−7[8]
Rotational velocity (v sin i)0.86[9] km/s
Age2.6±0.8 Gyr[8]
4.38±2.54 Gyr[3]
11.9±1.1[6] Gyr
B
Mass0.576±0.013[10] M☉
Other designations
BD+05°1295, HD 46375, HIP 31246, SAO 114040[11]
Database references
SIMBADdata

HD 46375 is double star[10] with an exoplanetary companion in the equatorial constellation of Monoceros. It presents as an 8th-magnitude star with an apparent visual magnitude of 7.91,[2] which is too dim to be readily visible to the naked eye. The system is located at a distance of 96.5 light-years from the Sun based on parallax measurements,[1] but is slowly drifting closer with a radial velocity of −1 km/s.[1] The common proper motion stellar companion, designated HD 46375 B, has a linear projected separation of 346±13 AU.[10]

The primary component is a solar-type[8] star with a stellar classification of G9V,[3] matching a G-type main-sequence star. Age estimates for this star range from 2.6[8] up to 11.9[6] billion years. It is a chromospherically inactive star and is spinning slowly[5] with a projected rotational velocity of 0.86 km/s.[9] The absolute magnitude of this star places it one magnitude brighter than the equivalent for a zero age main sequence.[5] It has 91% of the mass and 101% of the radius of the Sun. The star is radiating 77%[6] of the luminosity of the Sun from its photosphere at an effective temperature of 3,663 K.[7]

This star has sometimes been classified as a member of the NGC 2244 star cluster in the Rosette Nebula, but in reality it just happens to lie in the foreground. The distance to the cluster is much greater, about 4500 light-years.

Planetary system

On March 29, 2000, the planet HD 46375 b with a minimum mass three quarters that of Saturn was discovered by Marcy, Butler, and Vogt in California, together with 79 Ceti b.[12][5] This planet was discovered using the "wobble method" or radial velocity method, which calculates the rate and shape of the stellar wobble caused by the revolving planet's gravity.

The HD 46375 planetary system[9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >0.226 ± 0.019 MJ 0.0398 ± 0.0023 3.023573 ± 0.000065 0.063 ± 0.026 — —

See also

References

  1. 1 2 3 4 5 6 7 8 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. 1 2 3 4 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 4 Grieves, N.; et al. (December 2018). "Chemo-kinematics of the Milky Way from the SDSS-III MARVELS survey". Monthly Notices of the Royal Astronomical Society. 481 (3): 3244–3265. arXiv:1803.11538. Bibcode:2018MNRAS.481.3244G. doi:10.1093/mnras/sty2431.
  4. ↑ Terrien, Ryan C.; et al. (March 2012). "An H-band Spectroscopic Metallicity Calibration for M Dwarfs". The Astrophysical Journal Letters. 747 (2): 6. arXiv:1202.1800. Bibcode:2012ApJ...747L..38T. doi:10.1088/2041-8205/747/2/L38. S2CID 118403568. L38.
  5. 1 2 3 4 Marcy, Geoffrey W.; et al. (2000). "Sub-Saturn Planetary Candidates of HD 16141 and HD 46375". The Astrophysical Journal Letters. 536 (1): L43–L46. arXiv:astro-ph/0004326. Bibcode:2000ApJ...536L..43M. doi:10.1086/312723. PMID 10849416. S2CID 119530785.
  6. 1 2 3 4 5 6 7 Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692. A5.
  7. 1 2 Rojas-Ayala, Bárbara; et al. (April 2012), "Metallicity and Temperature Indicators in M Dwarf K-band Spectra: Testing New and Updated Calibrations with Observations of 133 Solar Neighborhood M Dwarfs", The Astrophysical Journal, 748 (2): 93, arXiv:1112.4567, Bibcode:2012ApJ...748...93R, doi:10.1088/0004-637X/748/2/93, S2CID 41902340.
  8. 1 2 3 4 Gaulme, P.; Deheuvels, S.; Weiss, W. W.; Mosser, B.; Moutou, C.; Bruntt, H.; Donati, J. -F.; Vannier, M.; Guillot, T.; Appourchaux, T.; Michel, E.; Auvergne, M.; Samadi, R.; Baudin, F.; Catala, C.; Baglin, A. (December 2010). "HD 46375: seismic and spectropolarimetric analysis of a young Sun hosting a Saturn-like planet". Astronomy and Astrophysics. 524: 8. arXiv:1011.2671. Bibcode:2010A&A...524A..47G. doi:10.1051/0004-6361/201014142. S2CID 119221790. A47.
  9. 1 2 3 Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.
  10. 1 2 3 Mugrauer, M.; et al. (May 2006). "A search for wide visual companions of exoplanet host stars: The Calar Alto Survey". Astronomische Nachrichten. 327 (4): 321. arXiv:astro-ph/0602067. Bibcode:2006AN....327..321M. doi:10.1002/asna.200510528. S2CID 118902770.
  11. ↑ "HD 46375". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-23.
  12. ↑ "Keck astronomers discover planets smaller than saturn" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. March 29, 2000. Retrieved August 13, 2019.
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