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Gliese 393, or GJ 393, is a single[7] star in the equatorial constellation of Sextans, positioned about 1.5° to the NNW of Beta Sextantis.[8] At an apparent visual magnitude of 9.65,[2] it is much too faint to be seen with the unaided eye. This star is located at a distance of 22.9 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +8.3 km/s.[2] It has a large proper motion, traversing the celestial sphere at the rate of 0.950″ per year.[9] The net velocity of this star relative to the Sun is 32.9 km/s.[2] It shares a similar space motion as members of the AB Doradus moving group, but is considered a random interloper.[5]

Gliese 393
Observation data
Epoch J2000      Equinox J2000
Constellation Sextans
Right ascension 10h 28m 55.55130s[1]
Declination +00° 50′ 27.6018″[1]
Apparent magnitude (V) 9.65[2]
Characteristics
Spectral type M2V[3]
U−B color index 1.192[2]
B−V color index 1.507±0.014[2]
Astrometry
Radial velocity (Rv)+8.34±0.10[2] km/s
Proper motion (μ) RA: −603.003[1] mas/yr
Dec.: −732.075[1] mas/yr
Parallax (π)142.0951 ± 0.0212 mas[4]
Distance22.953 ± 0.003 ly
(7.038 ± 0.001 pc)
Absolute magnitude (MV)10.40[2]
Details[3]
Mass0.432±0.011 M☉
Radius0.4459±0.0073 R☉
Luminosity0.02687±0.00054 L☉
Surface gravity (log g)4.88±0.07 cgs
Temperature3,579±51 K
Metallicity [Fe/H]−0.09±0.16 dex
Rotational velocity (v sin i)1.5[5] km/s
Other designations
BD+01°2447, GJ 393, HIP 51317, LTT 12805, 2MASS J10285555+0050275[6]
Database references
SIMBADdata

The stellar classification of GJ 393 is M2V,[3] indicating this is a small red dwarf star that is generating energy through core hydrogen fusion. It is rotating slowly and appears to be chromospherically inactive, suggesting it is an older star; perhaps as much as 10 billion years old.[5] The star has 43% of the mass of the Sun and 44.6% of the Sun's radius. The metallicity, what astronomers term the abundance of heavy elements, is lower than in the Sun. It is radiating just 2.7% of the Sun's luminosity from its photosphere at an effective temperature of 3,579 K.[3]


Planetary system


In 2019 one candidate planet was detected by the radial velocity method. It is classified as a hot super-Earth, with an orbital period of one week and a semimajor axis of 8.2 Gm. Longer period signals found in the data were interpreted as stellar activity.[10]

In 2021, the planet was confirmed as real after being detected independently in three different datasets.[11]

The Gliese 393 planetary system[10][11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.71±0.24 M🜨 0.05402±0.00072 7.0268±0.00082 0 — —

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. 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. Schweitzer, A.; et al. (May 2019). "The CARMENES search for exoplanets around M dwarfs. Different roads to radii and masses of the target stars". Astronomy & Astrophysics. 625: 16. arXiv:1904.03231. Bibcode:2019A&A...625A..68S. doi:10.1051/0004-6361/201834965. S2CID 102351979. A68.
  4. Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  5. Schaefer, G. H.; et al. (May 2018), "AB Dor Moving Group Stars Resolved with the CHARA Array", The Astrophysical Journal, 858 (2): 14, Bibcode:2018ApJ...858...71S, doi:10.3847/1538-4357/aaba71, 71
  6. "GJ 393". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-08.
  7. Winters, Jennifer G.; et al. (June 2019). "The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc". The Astronomical Journal. 157 (6): 32. arXiv:1901.06364. Bibcode:2019AJ....157..216W. doi:10.3847/1538-3881/ab05dc. S2CID 86859146. 216.
  8. Sinnott, Roger W.; Perryman, Michael A. C. (1997). Millennium Star Atlas. Vol. 2. Sky Publishing Corporation and the European Space Agency. p. 779. ISBN 0-933346-83-2.
  9. Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)". The Astronomical Journal. 129 (3): 1483–1522. arXiv:astro-ph/0412070. Bibcode:2005AJ....129.1483L. doi:10.1086/427854. S2CID 2603568.
  10. Barnes, J. R.; et al. (2019-06-11). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP].
  11. Amado, Pedro J.; Bauer, Florian F.; Rodríguez López, Cristina; Rodríguez, Eloy; Cardona Guillén, C.; Perger, M.; Caballero, José A.; López-González, Maria J.; Muñoz Rodríguez, I.; Pozuelos, F. J.; Sánchez-Rivero, A.; Schlecker, M.; Quirrenbach, Andreas; Ribas, Ignasi; Reiners, Ansgar; Almenara, J.; Astudillo-Defru, N.; Azzaro, M.; Béjar, Victor J. S.; Bohemann, R.; Bonfils, X.; Bouchy, F.; Cifuentes, C.; Cortés-Contreras, M.; Delfosse, Xavier; Dreizler, Stefan; Forveille, Thierry; Hatzes, Artie P.; Henning, Thomas K.; Jeffers, Sandra V.; Kaminski, Adrian; Kürster, Martin; Lafarga, M.; Lodieu, Nicolas; Lovis, C.; Mayor, M.; Montes, David; Morales, Juan Carlos; Morales, Nicolás; Murgas, F.; Ortiz, José L.; Pepe, F.; Perdelwitz, V.; Pollaco, D.; Santos, N. C.; Schöfer, P.; Schweitzer, A.; Ségransan, N. C.; Shan, Y.; Stock, S.; Tal-Or, Lev; Udry, S.; Zapatero-Osorio, María Rosa; Zechmeister, Mathias (2021-05-28). "The CARMENES search for exoplanets around M dwarfs". Astronomy & Astrophysics. 650: A188. arXiv:2105.13785. doi:10.1051/0004-6361/202140633. S2CID 235248027.

На других языках

[de] Gliese 393

Gliese 393 ist ein roter Zwergstern im Sternbild Sextant. Bei einer scheinbaren Helligkeit von 9,65 mag leuchtet der Stern viel zu schwach, um mit dem bloßen Auge gesehen zu werden. Als kleiner Stern hat er etwa 41 % der Masse und des Radius der Sonne, aber nur 2,35 % ihrer Leuchtkraft.
- [en] Gliese 393


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