Gliese 22

A blue band light curve for a flare of Gliese 22A, adapted from Pettersen (1975)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
Gliese 22 A
Right ascension 00h 32m 29.4336s
Declination +67° 14′ 08.409″
Apparent magnitude (V) 10.29
Gliese 22 B
Right ascension 00h 32m 29.575s
Declination +67° 14′ 04.63″
Apparent magnitude (V) 12.19
Gliese 22 C
Right ascension 00h 32m 29.4s
Declination +67° 14′ 08″
Apparent magnitude (V) 13.2
Characteristics
Spectral type M2.5Ve / M3V
U−B color index 1.16
B−V color index 1.54
R−I color index 0.99
Variable type Flare stars
Astrometry
Radial velocity (Rv)10 km/s
Proper motion (μ) RA: 1739.0 mas/yr
Dec.: −224.93 mas/yr
Parallax (π)99.35 ± 2.17 mas[2]
Distance32.8 ± 0.7 ly
(10.1 ± 0.2 pc)
Absolute magnitude (MV)11.83
Orbit[3]
PrimaryGliese 22 AC
CompanionGliese 22 B
Period (P)223.3 yr
Semi-major axis (a)3.322″
Eccentricity (e)0.293
Inclination (i)47.3°
Longitude of the node (Ω)174.9°
Periastron epoch (T)JD 1859.4
Argument of periastron (ω)
(secondary)		146.3°
Orbit[4]
PrimaryGliese 22 A (Aa)
CompanionGliese 22 C (Ab)
Period (P)5,694.2±14.9 days
Semi-major axis (a)0.5106±0.0007″
Eccentricity (e)0.163±0.002
Inclination (i)43.7±0.2°
Longitude of the node (Ω)178.3±0.2°
Periastron epoch (T)JD 51817.2
Argument of periastron (ω)
(secondary)		284.5±0.5°
Details[5]
Mass0.378(A) + 0.136(C) M☉
Radius0.5(A) R☉
Luminosity0.04 L☉
Temperature2000–3500 K
Details
B
Mass0.382[6] M☉
Radius0.394[6] R☉
Luminosity0.011[7] L☉
Temperature3,339[8] K
Metallicity [Fe/H]−0.24[9] dex
Rotational velocity (v sin i)<4[10] km/s
Other designations
2MASS J00322970+6714080, BD+66°34, CCDM J00325+6714, GJ 22, HIP 2552, LFT 47, V547 Cassiopeiae, ADS 440
Database references
SIMBADdata
Exoplanet Archivedata

Gliese 22, also catalogued V547 Cassiopeiae or ADS 440, is a hierarchical star system approximately 33 light-years away in the constellation of Cassiopeia. The system consists of pair of red dwarf stars, Gliese 22A and Gliese 22C, orbited by a third red dwarf Gliese 22B in an outer orbit of about 223 years.

Planetary system

As of 2008, it was announced that a possible extrasolar planet, Gliese 22B b, orbits Gliese 22B but this is currently unconfirmed. The study in 2011 has indicated the orbit of the purported planet is stable.[11]

The Gliese 22 B planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (unconfirmed) 16 MJ — 5,500 0 — —

References

  1. ↑ Pettersen, B. R. (June 1975). "Discovery of flare activity on BD +66 34 (= Gliese 22 A)". Astronomy and Astrophysics. 41: 113. Bibcode:1975A&A....41..113P. Retrieved 27 November 2021.
  2. ↑ van Leeuwen, F. (November 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. ↑ Docobo, J. A.; Tamazian, V. S.; Balega, Y. Y.; Andrade, M.; Schertl, D.; Weigelt, G.; Campo, P.; Palacios, M. (2008). "A methodology for studying physical and dynamical properties of multiple stars. Application to the system of red dwarfs Gl 22". Astronomy and Astrophysics. 478 (1): 187. Bibcode:2008A&A...478..187D. doi:10.1051/0004-6361:20078594.
  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.
  5. ↑ McCarthy, D. W.; Henry, Todd J.; McLeod, Brian; Christou, Julian C. (1991). "The Low-Mass Companion of Gliese 22A: First Results of the Steward Infrared Speckle Camera". The Astronomical Journal. 101: 214. Bibcode:1991AJ....101..214M. doi:10.1086/115681.
  6. 1 2 Newton, Elisabeth R.; Irwin, Jonathan; Charbonneau, David; Berlind, Perry; Calkins, Michael L.; Mink, Jessica (2017). "The Hα Emission of Nearby M Dwarfs and its Relation to Stellar Rotation". The Astrophysical Journal. 834 (1): 85. arXiv:1611.03509. Bibcode:2017ApJ...834...85N. doi:10.3847/1538-4357/834/1/85. S2CID 55000202.
  7. ↑ McLean, M.; Berger, E.; Reiners, Ansgar (February 2012). "The Radio Activity-Rotation Relation of Ultracool Dwarfs". The Astrophysical Journal. 746 (1): 23. arXiv:1108.0415. Bibcode:2012ApJ...746...23M. doi:10.1088/0004-637X/746/1/23. S2CID 119159519.
  8. ↑ Houdebine, Éric R.; Mullan, D. J.; Doyle, J. G.; de la Vieuville, Geoffroy; Butler, C. J.; Paletou, F. (2019). "The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs". The Astronomical Journal. 158 (2): 56. arXiv:1905.07921. Bibcode:2019AJ....158...56H. doi:10.3847/1538-3881/ab23fe. S2CID 159041104.
  9. ↑ 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
  10. ↑ Jeffers, S. V.; Schöfer, P.; Lamert, A.; Reiners, A.; Montes, D.; Caballero, J. A.; Cortés-Contreras, M.; Marvin, C. J.; Passegger, V. M.; Zechmeister, M.; Quirrenbach, A.; Alonso-Floriano, F. J.; Amado, P. J.; Bauer, F. F.; Casal, E.; Diez Alonso, E.; Herrero, E.; Morales, J. C.; Mundt, R.; Ribas, I.; Sarmiento, L. F. (2018). "CARMENES input catalogue of M dwarfs. III. Rotation and activity from high-resolution spectroscopic observations". Astronomy and Astrophysics. 614: A76. arXiv:1802.02102. Bibcode:2018A&A...614A..76J. doi:10.1051/0004-6361/201629599. S2CID 56147445.
  11. ↑ Andrade, Manuel; Docobo, José A. (2011). "On the dynamical stability of the very low-mass object Gliese 22 Bb". Icarus. 215 (2): 712. Bibcode:2011Icar..215..712A. doi:10.1016/j.icarus.2011.07.008.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.