HD 3443
| Observation data Epoch J2000 Equinox 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[3] |
| Spectral type | G9V[3] |
| Apparent magnitude (g) | 5.95[4] |
| HD 3443B | |
| Evolutionary stage | main sequence[3] |
| Spectral type | K0.5V[3] |
| Astrometry | |
| Radial velocity (Rv) | 18.63[5] km/s |
| Proper motion (μ) | RA: 1450.34 mas/yr[1] Dec.: −19.38 mas/yr[1] |
| Parallax (π) | 64.93±1.85 mas[3] |
| Distance | 50 ± 1 ly (15.4 ± 0.4 pc) |
| Absolute magnitude (MV) | 5.31±0.08[2] |
| Orbit[6] | |
| Primary | HD 3443A |
| Name | 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 | |
| HD 3443A | |
| Mass | 0.915±0.005[3] M☉ |
| Radius | 1.31[10] R☉ |
| Luminosity | 1.2[8] L☉ |
| Surface gravity (log g) | 4.23[11] cgs |
| Temperature | 5449[8] K |
| Metallicity [Fe/H] | −0.12[2] dex |
| Rotation | 32.6±4.89 d[9] |
| Rotational velocity (v sin i) | 2.7±1.3[9] km/s |
| Age | 9.36[2] Gyr |
| HD 3443B | |
| Mass | 0.864±0.005[3] M☉ |
| Other designations | |
| CD−25 225, CPD−25 64, GJ 25, HIP 2941, HR 159, WDS 00373−2446, 2MASS J00372057−2446023 | |
| HD 3443A: 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.[12]
Properties
The star system is enriched in oxygen compared to the Solar System, having 140% of solar oxygen abundance,[13] but is depleted in heavier elements, having 75% of solar abundance of iron.[2]
References
- 1 2 3 4 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.
- 1 2 3 4 5 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. Bibcode:2009AJ....138.1354D. doi:10.1088/0004-6256/138/5/1354.
- 1 2 3 4 5 6 7 Andrade, Manuel (2019). "Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries". Astronomy & Astrophysics. 630: A96. Bibcode:2019A&A...630A..96A. doi:10.1051/0004-6361/201936199.
- ↑ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 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. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID 119387088.
- ↑ 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. Bibcode:2000A&AS..145..215P. doi:10.1051/aas:2000237.
- ↑ 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. arXiv:1010.4176. Bibcode:2010PASP..122.1483T. doi:10.1086/657903. S2CID 26826524.
- 1 2 3 4 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. arXiv:2005.03573. doi:10.1093/mnras/staa1316.
- 1 2 3 Justesen, A. B.; Albrecht, S. (2020). "The spin-orbit alignment of visual binaries". Astronomy & Astrophysics. 642: A212. arXiv:2008.12068. Bibcode:2020A&A...642A.212J. doi:10.1051/0004-6361/202039138. S2CID 221340982.
- ↑ Tuchow, Noah W.; Stark, Christopher C.; Mamajek, Eric (2024). "HPIC: The Habitable Worlds Observatory Preliminary Input Catalog". The Astronomical Journal. 167 (3): 139. Bibcode:2024AJ....167..139T. doi:10.3847/1538-3881/ad25ec.
- ↑ Souza Dos Santos, P. V.; Porto De Mello, G. F.; Costa-Bhering, E.; Lorenzo-Oliveira, D.; Almeida-Fernandes, F.; Dutra-Ferreira, L.; Ribas, I. (2024). "Fine structure of the age-chromospheric activity relation in solar-type stars: II. Hα line". Monthly Notices of the Royal Astronomical Society. 532 (1): 563. arXiv:2406.12519. Bibcode:2024MNRAS.532..563S. doi:10.1093/mnras/stae1532.
- ↑ 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. arXiv:1401.1006. Bibcode:2014MNRAS.443..260J. doi:10.1093/mnras/stu1052.
- ↑ Maldonado, J.; Villaver, E. (2016). "Evolved stars and the origin of abundance trends in planet hosts". Astronomy & Astrophysics. 588: A98. arXiv:1602.00835. Bibcode:2016A&A...588A..98M. doi:10.1051/0004-6361/201527883. S2CID 119212009.
