HD 61859
| Observation data Epoch . Equinox . | |
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| Apparent magnitude (V) | . |
| Characteristics | |
| Evolutionary stage | . |
| Spectral type | . |
| Apparent magnitude (.) | . |
| Apparent magnitude (.) | . |
| Apparent magnitude (..) | . |
| Apparent magnitude (..) | . |
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| B−V color index | . |
| Astrometry | |
| Radial velocity (Rv) | . km/s |
| Proper motion (μ) | RA: .. mas/yr Dec.: .. mas/yr |
| Parallax (π) | . ± .. mas |
| Distance | . ly (. pc) |
| Absolute magnitude (MV) | . |
| Details | |
| Mass | . M☉ |
| Radius | . R☉ |
| Luminosity | . L☉ |
| Surface gravity (log g) | . cgs |
| Temperature | .. K |
| Metallicity [Fe/H] | . dex |
| Rotational velocity (v sin i) | . km/s |
| Age | . Gyr |
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| Database references | |
| SIMBAD | data |
HD 61859 is a spectroscopic binary in the constellation Gemini, located next the bright star Castor. It is made up of two F-type main-sequence stars which orbit each other every 32 days.[1] The system has an apparent magnitude of 6.06, meaning that it is faintly visible to the naked eye under dark skies. It is located at a distance of 64.983 light-years (19.924 parsecs) from Earth.[2]
Characteristics[edit]
HD 61859 is a spectroscopic binary system, more specifically a double-lined spectroscopic binary, where the spectrum of both stars are seen.[3] It is made up of two F-type main sequence stars that have the same spectral type of F7V.[4] Both stars orbit each other every 32 days, and are separated by a distance of 30 R☉.[1][lower-alpha 1] The orbit of the system is highly inclined in relation to Earth (i = 94.73°) and has an eccentricity of 0.1951, causing the distance between both components to vary from 25 to 36 R☉.[1]
The Transiting Exoplanet Survey Satellite (TESS) detected very weak eclipses 0.1% in the system, when the secondary star passes in front of the primary. This observation, however, is still insufficient to classify the system as an eclipsing binary.[1]
Notes[edit]
- ↑ From angular separation in milliarcseconds and distance.
References[edit]
- ↑ 1.0 1.1 1.2 1.3 Lester, Kathryn V.; Schaefer, Gail H.; Fekel, Francis C.; Gies, Douglas R.; Henry, Todd J.; Jao, Wei-Chun; Paredes, Leonardo A.; Hubbard-James, Hodari-Sadiki; Farrington, Christopher D.; Gordon, Kathryn D.; Chojnowski, S. Drew; Monnier, John D.; Kraus, Stefan; Bouquin, Jean-Baptiste Le; Anugu, Narsireddy (2022-11-01). "Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692". The Astronomical Journal. 164 (6): 228. arXiv:2209.09993. Bibcode:2022AJ....164..228L. doi:10.3847/1538-3881/ac9385. ISSN 0004-6256.
- ↑ Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
- ↑ Tokovinin, Andrei (2014). "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal. 147 (4): 87. arXiv:1401.6827. Bibcode:2014AJ....147...87T. doi:10.1088/0004-6256/147/4/87.
- ↑ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424: 727. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
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