Gliese 402

A visual band light curve for EE Leonis, adapted from Weis (1994)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Leo
Right ascension 10h 50m 52.03129s[2]
Declination +06° 48′ 29.2278″[2]
Apparent magnitude (V) 11.64 - 11.70[3]
Characteristics
Spectral type M4.0V[4]
U−B color index +1.16[5]
B−V color index +1.66[5]
V−R color index +1.24[5]
R−I color index +1.57[5]
Variable type BY Dra[3]
Astrometry
Radial velocity (Rv)-1.04[6] km/s
Proper motion (μ) RA: −856.185[7] mas/yr
Dec.: −818.607[7] mas/yr
Parallax (π)143.5391 ± 0.0286 mas[8]
Distance22.722 ± 0.005 ly
(6.967 ± 0.001 pc)
Absolute magnitude (MV)12.47[5]
Details
Mass0.255 ± 0.014[9] M☉
Radius0.3[10] R☉
Surface gravity (log g)4.5[11] cgs
Temperature3100[11] K
Metallicity [Fe/H]-0.06[9] dex
Other designations
EE Leo, HIP 53020, Gliese 402, LTT 12891, LHS 294, Wolf 358
Database references
SIMBADdata
ARICNSdata

Gliese 402 is a star located 22.7 light years from the Solar System. Located in the constellation of Leo, it is also known as Wolf 358 from its entry in Max Wolf's star catalogue. The stars nearest to Gliese 402 are Gliese 393, at 3.43 light years, Gliese 408, at 6.26 light years, and Gliese 382 at 6.66 light years.[12]

Gliese 402 is a BY Draconis variable, with its apparent magnitude varying between 11.64 and 11.70. The brightness changes are due to starspots and chromospheric activity combined with the rotation of the star. It has been given the variable star designation EE Leonis.[3]

Like the vast majority of stars in the Solar neighborhood, Gliese 402 is a dim red dwarf. With an apparent magnitude +11.66, it is far too dim to be seen with the naked eye; it can only be seen with a telescope. Its luminosity is only 0.091% that of the Sun.[12] Its spectral type is M4V (sometimes cited as M5V) and its effective temperature is about 3100 K. Its physical characteristics are quite similar to those of Ross 128 or Kruger 60 B, with a radius of about 30% of the Sun.[10] Its projected rotation speed is at most 2.3 km/s or less,[9] while its metallicity is slightly lower than that of the Sun.[9]

References

  1. ↑ Weis, Edward W. (March 1994). "Long Term Variability in Dwarf M Stars". The Astronomical Journal. 107 (3): 1135–1140. Bibcode:1994AJ....107.1135W. doi:10.1086/116925. Retrieved 19 January 2022.
  2. 1 2 van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  3. 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. ↑ Alonso-Floriano, F. J.; Morales, J. C.; Caballero, J. A.; Montes, D.; Klutsch, A.; Mundt, R.; Cortés-Contreras, M.; Ribas, I.; Reiners, Ansgar; Amado, P. J.; Quirrenbach, A.; Jeffers, S. V. (2015). "CARMENES input catalogue of M dwarfs" (PDF). Astronomy & Astrophysics. 577: A128. arXiv:1502.07580. Bibcode:2015A&A...577A.128A. doi:10.1051/0004-6361/201525803. S2CID 53135130.
  5. 1 2 3 4 5 "ARICNS 4C00824". ARICNS. Retrieved 23 January 2017.
  6. ↑ Nidever, David L.; et al. (2013). "Radial Velocities for 889 Late-Type Stars". The Astrophysical Journal Supplement Series. 141 (2): 503–522. arXiv:astro-ph/0112477. Bibcode:2002ApJS..141..503N. doi:10.1086/340570. S2CID 51814894.
  7. 1 2 Brown, A. G. A; Vallenari, A; Prusti, T; De Bruijne, J. H.J; Mignard, F; Drimmel, R; Babusiaux, C; Bailer-Jones, C. A.L; Bastian, U; Biermann, M; Evans, D. W; Eyer, L; Jansen, F; Jordi, C; Katz, D; Klioner, S. A; Lammers, U; Lindegren, L; Luri, X; o'Mullane, W; Panem, C; Pourbaix, D; Randich, S; Sartoretti, P; Siddiqui, H. I; Soubiran, C; Valette, V; Van Leeuwen, F; Walton, N. A; et al. (2016). "Gaia Data Release 1". Astronomy & Astrophysics. 595: A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512. S2CID 1828208.
  8. ↑ 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.
  9. 1 2 3 4 Jenkins, J. S.; Ramsey, L. W.; Jones, H. R. A.; Pavlenko, Y.; Gallardo, J.; Barnes, J. R.; Pinfield, D. J. (2009). "Rotational Velocities for M Dwarfs". The Astrophysical Journal. 704 (2): 975–988. arXiv:0908.4092. Bibcode:2009ApJ...704..975J. doi:10.1088/0004-637X/704/2/975. S2CID 119203469.
  10. 1 2 Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics". Astronomy & Astrophysics. 367 (2): 521–24. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID 425754.
  11. 1 2 Lépine, Sébastien; et al. (2013). "A Spectroscopic Catalog of the Brightest (J < 9) M Dwarfs in the Northern Sky". The Astronomical Journal. 145 (4): 102. arXiv:1206.5991. Bibcode:2013AJ....145..102L. doi:10.1088/0004-6256/145/4/102. S2CID 117144290.
  12. 1 2 "Stars within 15 light-years of Wolf 358". The Internet Stellar Database.
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