Gliese 54

Last updated
Gliese 54
Observation data
Epoch J2000       Equinox J2000
Constellation Tucana
Right ascension 01h 10m 22.8809s [1]
Declination −67° 26 41.9487 [1]
Apparent magnitude  (V)9.80
Characteristics
Spectral type M2.5 (composite)
Astrometry
Proper motion (μ)RA: 386.2±0.2 [2]   mas/yr
Dec.: 579.7±0.1 [2]   mas/yr
Parallax (π)126.9 ± 0.4  mas [2]
Distance 25.70 ± 0.08  ly
(7.88 ± 0.02  pc)
Absolute magnitude  (MV)+10.23
Orbit [3]
PrimaryGliese 54 A
CompanionGliese 54 B
Period (P)1.14434+0.00022
0.00022
yr
Semi-major axis (a)0.12619±0.00039"
(1.00 AU)
Eccentricity (e)0.1718±0.0024
Inclination (i)125.32+0.35
0.35
°
Details [4]
Gliese 54 A
Mass 0.43  M
Radius 0.51  R
Temperature 4250  K
Metallicity 0.17 [3]
Rotational velocity (v sin i)-15.0 km/s
Gliese 54 B
Mass 0.3  M
Other designations
CD−68°47, Gaia DR2  4704272495284592512, HIP  5496, LHS  1208, 2MASS J01102281-6726425
Database references
SIMBAD data
ARICNS data

Gliese 54 (GJ 54 / HIP 5496 / LHS 1208) [5] is a star near the Solar System located at 25.7 light years away. [2] It is located in the constellation of Tucana, close to the edge, almost in the neighboring Hydrus. It is below the threshold of brightness to be observable to the naked eye with an apparent magnitude of +9.80. [5]

Gliese 54 is a red dwarf of spectral type M2 with an effective temperature of 4250 K. [6] In the SIMBAD database it appears listed as a variable star, getting the provisional variable designation NSV 427. [5] It has a companion with which it forms a binary system whose orbital period is 427 ± 9 days. The companion, a red dwarf whose brightness is ~1 magnitude lower than Gliese 54, has been resolved with the instrument NICMOS installed in the Hubble Space Telescope. [7]

The known stars closest to Gliese 54 are ζ Tucanae, solar analog 3.1 light years, and β Hydri 5.1 light years [8]

See also

Related Research Articles

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<span class="mw-page-title-main">Gliese 445</span> Star in the constellation Camelopardalis

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<span class="mw-page-title-main">Gliese 22</span> Star in the constellation Cassiopeia

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<span class="mw-page-title-main">Gliese 752</span> Binary star system in the constellation Aquila

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<span class="mw-page-title-main">GL Virginis</span> Star in the constellation Virgo

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References

  1. 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.
  2. 1 2 3 4 Benedict, G. F.; et al. (2016). "The Solar Neighborhood. XXXVII: The Mass-Luminosity Relation for Main-sequence M Dwarfs". The Astronomical Journal. 152 (5). 141. arXiv: 1608.04775 . Bibcode: 2016AJ....152..141B . doi: 10.3847/0004-6256/152/5/141 .
  3. 1 2 Mann, Andrew W.; Dupuy, Trent; Kraus, Adam L.; Gaidos, Eric; Ansdell, Megan; Ireland, Michael; Rizzuto, Aaron C.; Hung, Chao-Ling; Dittmann, Jason; Factor, Samuel; Feiden, Gregory; Martinez, Raquel A.; Ruíz-Rodríguez, Dary; Chia Thao, Pa (2019), "How to constrain your M dwarf. II. The Mass-Luminosity-Metallicity relation from 0.075 to 0.70 solar masses", The Astrophysical Journal, 871 (1): 63, arXiv: 1811.06938 , Bibcode:2019ApJ...871...63M, doi: 10.3847/1538-4357/aaf3bc , S2CID   119372932
  4. Henry, Todd J.; Jao, Wei-Chun; Winters, Jennifer G.; Dieterich, Sergio B.; Finch, Charlie T.; Ianna, Philip A.; Riedel, Adric R.; Silverstein, Michele L.; Subasavage, John P.; Vrijmoet, Eliot Halley (2018), "The Solar Neighborhood XLIV: RECONS Discoveries within 10 Parsecs", The Astronomical Journal, 155 (6): 265, arXiv: 1804.07377 , Bibcode:2018AJ....155..265H, doi: 10.3847/1538-3881/aac262 , S2CID   53983430
  5. 1 2 3 "CD-68 47". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 6 May 2017.
  6. Morales, J. C.; Ribas, I.; Jordi, C. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics . 478 (2): 507. arXiv: 0711.3523 . Bibcode:2008A&A...478..507M. doi:10.1051/0004-6361:20078324. S2CID   16238033. pp. 507-512 (Table consulted on CDS).
  7. Golimowski, David A.; Henry, Todd J.; Krist, John E.; Dieterich, Sergio; Ford, Holland C.; Illingworth, Garth D.; Ardila, David R.; Clampin, Mark; Franz, Otto G.; Wasserman, Lawrence H.; Benedict, G. Fritz; McArthur, Barbara E.; Nelan, Edmund G. (2004). "The Solar Neighborhood. IX. Hubble Space Telescope Detections of Companions to Five M and L Dwarfs Within 10 parsecs of the Sun". The Astronomical Journal . 128 (4): 1733–1747. arXiv: astro-ph/0406664 . Bibcode:2004AJ....128.1733G. doi:10.1086/423911. S2CID   12310839.
  8. Stars Within 15 light-years of Cape Photographic Durchmusterung -68 ° 41 (The Internet Stellar Database)