CD-44 170
Observation data
Epoch J2000      Equinox J2000
Constellation Phoenix
Right ascension 00h 39m 58.8243s[1]
Declination −44° 15′ 11.5824″[1]
Apparent magnitude (V) 11.401
Characteristics
Evolutionary stage main-sequence star
Spectral type M0.5V[2]
Astrometry
Radial velocity (Rv)11.85±0.19[3] km/s
Proper motion (μ) RA: 483.002[3] mas/yr
Dec.: −221.111[3] mas/yr
Parallax (π)42.3320 ± 0.0248 mas[3]
Distance77.05 ± 0.05 ly
(23.62 ± 0.01 pc)
Details
Mass0.53[2] M☉
Radius0.52[4] R☉
Luminosity0.04597±0.00087[5] L☉
Temperature3604±72[6] K
Metallicity [Fe/H]−0.09±0.09[6] dex
Rotation31.8 d[2]
Other designations
Gaia DR2 4980466929964496128, GJ 27.1, HIP 3143, TYC 7531-1014-1, 2MASS J00395880-4415117[1]
Database references
SIMBADdata

CD-44 170, also known as Gliese 27.1, Gliese 9018 and HIP 3143, is an M-type main-sequence star. Its surface temperature is 3,604 K (6,028 °F; 3,331 °C)±72 K. The star's concentration of heavy elements is similar to that of the Sun.[6]

Planetary system

In 2014, a planet named Gliese 27.1 b with an orbital period of 16 days was announced. It was discovered using the radial velocity method.[7] The planetary equilibrium temperature is 406 K (271 °F; 133 °C).[5] The planet's existence was doubted until 2020 because the putative orbital period is equal to half of the star's rotational period.[2]

The Gliese 27.1 planetary system[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (disputed) > 13+4.1
−6.6 M⊕		 0.101+0.009
−0.013		 15.8190+0.0049
−0.0026		 — — >3.63 R⊕

References

  1. 1 2 3 "CD-44 170". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-04-26.
  2. 1 2 3 4 Feng, Fabo; Butler, R. Paul; Shectman, Stephen A.; Crane, Jeffrey D.; Vogt, Steve; Chambers, John; Jones, Hugh R. A.; Wang, Sharon Xuesong; Teske, Johanna K.; Burt, Jenn; Díaz, Matías R.; Thompson, Ian B. (2020). "Search for Nearby Earth Analogs. II. Detection of Five New Planets, Eight Planet Candidates, and Confirmation of Three Planets around Nine Nearby M Dwarfs". The Astrophysical Journal Supplement Series. 246 (1): 11. arXiv:2001.02577. Bibcode:2020ApJS..246...11F. doi:10.3847/1538-4365/ab5e7c. S2CID 210064560.
  3. 1 2 3 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.
  4. ↑ Newton, Elisabeth R.; Irwin, Jonathan; Charbonneau, David; Berta-Thompson, Zachory K.; Dittmann, Jason A. (2016). "The Impact of Stellar Rotation on the Detectability of Habitable Planets Around M Dwarfs". The Astrophysical Journal. 821 (1): L19. arXiv:1604.03135. Bibcode:2016ApJ...821L..19N. doi:10.3847/2041-8205/821/1/L19. S2CID 73538034.
  5. 1 2 3 Martínez-Rodríguez, Héctor; Caballero, José Antonio; Cifuentes, Carlos; Piro, Anthony L.; Barnes, Rory (2019). "Exomoons in the Habitable Zones of M Dwarfs". The Astrophysical Journal. 887 (2): 261. arXiv:1910.12054. Bibcode:2019ApJ...887..261M. doi:10.3847/1538-4357/ab5640. S2CID 204904780.
  6. 1 2 3 Kuznetsov, M. K.; Del Burgo, C.; Pavlenko, Ya. V.; Frith, J. (2019). "Characterization of a Sample of Southern M Dwarfs Using Harps and X-shooter Spectra". The Astrophysical Journal. 878 (2): 134. Bibcode:2019ApJ...878..134K. doi:10.3847/1538-4357/ab1fe9.
  7. ↑ Tuomi, Mikko; Jones, Hugh R. A.; Barnes, John R.; Anglada-Escudé, Guillem; Jenkins, James S. (2014). "Bayesian search for low-mass planets around nearby M dwarfs – estimates for occurrence rate based on global detectability statistics". Monthly Notices of the Royal Astronomical Society. 441 (2): 1545–1569. arXiv:1403.0430. doi:10.1093/mnras/stu358.


This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.