HD 283750
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 36m 48.2413s[1] |
| Declination | 27° 07′ 55.8983″[1] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | K5Ve[2] |
| B−V color index | 1.12[2] |
| Variable type | BY Draconis |
| Astrometry | |
| Radial velocity (Rv) | 42±3[3] km/s |
| Proper motion (μ) | RA: 232.17±0.06 mas/yr[3] Dec.: -147.48±0.04 mas/yr[3] |
| Parallax (π) | 57.49 ± 0.05 mas[3] |
| Distance | 56.73 ± 0.05 ly (17.39 ± 0.02 pc) |
| Details[2] | |
| Mass | 0.8 M☉ |
| Radius | 0.8 R☉ |
| Surface gravity (log g) | 4.5 cgs |
| Temperature | 4250±100 K |
| Rotational velocity (v sin i) | 7.4 km/s |
| Age | 1[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 283750, also known as V833 Tauri, is a K-type main-sequence star about 57 light-years away. The star's age is much younger than the Sun's at 1 billion years.[4] HD 283750 is similar to the Sun in concentration of heavy elements.[2]
The star has a co-moving white dwarf companion WD 0443+270 at projected separation 124″,[5] both possibly an ejected members of Hyades. The white dwarf companion has a rather exotic iron core.[4] The white dwarf belongs to spectral class DA9 and have the mass of 0.62±0.02M☉.[6]
Although HD 283750 was classified as a multi-period variable,[7] paper in 2020 claims its variability is not exceeding the variability of the Sun, and no period can be identified.[8]
The HD 283750 is covered by a large amount of starspots, filling up to 28% of stellar surface at the maxima of magnetic cycle.[9] In November 1993, the star has emitted an extremely powerful flare with energy of 7.47×1034 ergs, which is on or even above the upper limit of possible energy releases in flare stars.[7] The flares of HD 283750 are accompanied by the particle beams strong enough to affect the polarization properties of stellar photosphere.[10]
Suspected substellar companion
In 1996 a brown dwarf HD 283750b on a 1.79-days orbit around HD 283750 was detected by differential Doppler spectroscopy method. By 2007, the mass of companion was refined to 0.19M☉, making it a red dwarf star.[11]
References
- ^ a b c "HD 283750". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 30 June 2021.
- ^ a b c d Abundance Analysis of the BY Draconis Variable, Hot Flare Star V833 Tauri
- ^ a b c 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.
- ^ a b c WD0433+270: an old Hyades stream member or an Fe-core white dwarf?, 2007, arXiv:0710.3999
- ^ New nearby white dwarfs from Gaia DR1 TGAS and UCAC5/URAT, 2017, arXiv:1711.10778
- ^ The binarity of the local white dwarf population, 2017, arXiv:1703.06893
- ^ a b Time-series photometric spot modeling. IV. The multi-periodic K5Ve binary V833 Tauri
- ^ Wavelet analysis of the long-term activity of V833 Tau
- ^ Photometric period and rotational brightness modulation of V833 Tau
- ^ Possible detection of a stellar flare-generated particle beam in polarized light
- ^ [https://www.aanda.org/articles/aa/pdf/2016/09/aa28231-16.pdf SPOTS: The Search for Planets Orbiting Two Stars II. First constraints on the frequency of sub-stellar companions on wide circumbinary orbits}}
