Astronomy:HD 3443
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Short description: Binary star system in constellation Cetus
Coordinates: 
00h 37m 20.7196s, −24° 46′ 02.1843″
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h 37m 20.7196s[1] |
| Declination | −24° 46′ 02.1843″[1] |
| Apparent magnitude (V) | 5.57[2] |
| Characteristics | |
| HD 3443A | |
| Evolutionary stage | main-sequence star |
| Spectral type | G9V[3] |
| Apparent magnitude (g) | 5.95[4] |
| HD 3443B | |
| Evolutionary stage | main-sequence star |
| Spectral type | K0.5V[3] |
| Astrometry | |
| Radial velocity (Rv) | 18.63[5] km/s |
| Proper motion (μ) | RA: 1450.34[1] mas/yr Dec.: −19.38[1] mas/yr |
| Parallax (π) | 64.93 ± 1.85[3] mas |
| Distance | 50 ± 1 ly (15.4 ± 0.4 pc) |
| Absolute magnitude (MV) | 5.31±0.08[2] |
| Orbit[6] | |
| Primary | HD 3443A |
| Companion | HD 3443B |
| Period (P) | 25.09 y |
| Semi-major axis (a) | 0.4627[7]" (8.9 AU[8]) |
| Eccentricity (e) | 0.235 |
| Inclination (i) | 65.9[9]° |
| Semi-amplitude (K1) (primary) | 18.4 km/s |
| Details[9] | |
| HD 3443A | |
| Mass | 0.915±0.005[3] M☉ |
| Radius | 0.92±0.05 R☉ |
| Luminosity | 1.2[8] L☉ |
| Temperature | 5449[8] K |
| Metallicity [Fe/H] | −0.12[2] dex |
| Rotation | 32.6±4.89 d |
| Rotational velocity (v sin i) | 2.7±1.3 km/s |
| Age | 9.36[2] Gyr |
| HD 3443B | |
| Mass | 0.864±0.005[3] M☉ |
| Other designations | |
CD-25 225, CPD CPD-25 64, Gliese 25, HIP 2941, HR 159, 2MASS J00372057-2446023, WDS 00373–2446 | |
| HD 3443A: Gaia EDR3 2347260998051944448, TYC 6421-1924-1 | |
| HD 3443B: TYC 6421-1924-2 | |
| Database references | |
| SIMBAD | data |
HD 3443 is a binary system composed of medium-mass main sequence stars in the constellation of Cetus about 50 light years away.
System
This binary star system, with an orbital semimajor axis 8.9 AU, has not had any circumstellar dust detected as of 2020.[8] While the habitable zones of the stars stretch from 0.55 to 0.95 AU from the stars, planetary orbits with a semimajor axis beyond 1.87 AU would become unstable due to the influence of the binary companion.[10]
Properties
The star system is enriched in oxygen compared to the Solar System, having 140% of solar oxygen abundance,[11] but is depleted in heavier elements, having 75% of solar abundance of iron.[2]
References
- ↑ 1.0 1.1 1.2 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 2.4 Davidson, James W.; Baptista, Brian J.; Horch, Elliott P.; Franz, Otto; Van Altena, William F. (2009). "A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging". The Astronomical Journal 138 (5): 1354–1364. doi:10.1088/0004-6256/138/5/1354. Bibcode: 2009AJ....138.1354D.
- ↑ 3.0 3.1 3.2 3.3 3.4 Andrade, Manuel (2019). "Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries". Astronomy & Astrophysics 630: A96. doi:10.1051/0004-6361/201936199. Bibcode: 2019A&A...630A..96A.
- ↑ 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.
- ↑ Pourbaix, D. et al. (September 2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics 424: 727–732. doi:10.1051/0004-6361:20041213. Bibcode: 2004A&A...424..727P.
- ↑ Pourbaix, D. (2000). "Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses". Astronomy and Astrophysics Supplement Series 145 (2): 215–222. doi:10.1051/aas:2000237. Bibcode: 2000A&AS..145..215P.
- ↑ Tokovinin, A.; Cantarutti, R.; Tighe, R.; Schurter, P.; Van Der Bliek, N.; Martinez, M.; Mondaca, E. (2010). "High-Resolution Imaging at the SOAR Telescope". Publications of the Astronomical Society of the Pacific 122 (898): 1483–1494. doi:10.1086/657903. Bibcode: 2010PASP..122.1483T.
- ↑ 8.0 8.1 8.2 8.3 Su, Kate Y L.; Kennedy, Grant M.; Yelverton, Ben (2020). "No significant correlation between radial velocity planet presence and debris disc properties". Monthly Notices of the Royal Astronomical Society 495 (2): 1943–1957. doi:10.1093/mnras/staa1316.
- ↑ 9.0 9.1 Justesen, A. B.; Albrecht, S. (2020). "The spin-orbit alignment of visual binaries". Astronomy & Astrophysics 642: A212. doi:10.1051/0004-6361/202039138. Bibcode: 2020A&A...642A.212J.
- ↑ Jaime, Luisa G.; Aguilar, Luis; Pichardo, Barbara (2014). "Habitable zones with stable orbits for planets around binary systems". Monthly Notices of the Royal Astronomical Society 443 (1): 260–274. doi:10.1093/mnras/stu1052. Bibcode: 2014MNRAS.443..260J.
- ↑ Maldonado, J.; Villaver, E. (2016). "Evolved stars and the origin of abundance trends in planet hosts". Astronomy & Astrophysics 588: A98. doi:10.1051/0004-6361/201527883. Bibcode: 2016A&A...588A..98M.
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