Astronomy:CD-44 170
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Short description: Star in the constellation Phoenix
Coordinates: 
00h 39m 58.8243s, −44° 15′ 11.5824″
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[3] mas |
| Distance | 77.05 ± 0.05 ly (23.62 ± 0.01 pc) |
| Details | |
| Mass | 0.53[2] M☉ |
| Radius | 0.52[4] R☉ |
| Luminosity | 0.04597±0.00087[5] L☉ |
| Temperature | 3604±72[6] K |
| Metallicity [Fe/H] | −0.09±0.09[6] dex |
| Rotation | 31.8 d[2] |
| Other designations | |
| Database references | |
| SIMBAD | data |
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]
| 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
- ↑ 1.0 1.1 1.2 "CD-44 170". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=CD-44+170.
- ↑ 2.0 2.1 2.2 2.3 Feng, Fabo; Butler, R. Paul; Shectman, Stephen A.; Crane, Jeffrey D.; Vogt, Steve; Chambers, John; Jones, Hugh R. A.; Wang, Sharon Xuesong et al. (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. doi:10.3847/1538-4365/ab5e7c. Bibcode: 2020ApJS..246...11F.
- ↑ 3.0 3.1 3.2 3.3 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 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. doi:10.3847/2041-8205/821/1/L19. Bibcode: 2016ApJ...821L..19N.
- ↑ 5.0 5.1 5.2 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. doi:10.3847/1538-4357/ab5640. Bibcode: 2019ApJ...887..261M.
- ↑ 6.0 6.1 6.2 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. doi:10.3847/1538-4357/ab1fe9. Bibcode: 2019ApJ...878..134K.
- ↑ 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. doi:10.1093/mnras/stu358.
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