HD 283750

A light curve for V833 Tauri. The main plot (adapted from Strassmeier et al.[1] and Oláh et al.[2]) shows the long term visual band variation, and the inset plot (plotted from TESS data[3]) shows the periodic variability.
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 04h 36m 48.2413s[4]
Declination 27° 07′ 55.8983″[4]
Apparent magnitude (V) 8.02 - 8.40[5]
Characteristics
Evolutionary stage Main sequence
Spectral type K5Ve[6]
B−V color index 1.12[6]
Variable type BY Dra + Flare[5]
Astrometry
Radial velocity (Rv)42±3[7] km/s
Proper motion (μ) RA: 232.17±0.06 mas/yr[7]
Dec.: -147.48±0.04 mas/yr[7]
Parallax (π)57.49 ± 0.05 mas[7]
Distance56.73 ± 0.05 ly
(17.39 ± 0.02 pc)
Details[6]
Mass0.8 M☉
Radius0.8 R☉
Surface gravity (log g)4.5 cgs
Temperature4250±100 K
Rotational velocity (v sin i)7.4 km/s
Age1[8] Gyr
Other designations
V833 Tauri, BD+26 730, Gaia DR2 151650076838458112, GJ 171.2, HIP 21482, TYC 1838-564-1, 2MASS J04364822+2707559[4]
Database references
SIMBADdata

HD 283750, also known as V833 Tauri, is a K-type main-sequence star 57 light-years away from the Sun. The star is much younger than the Sun's at 1 billion years.[8] HD 283750 is similar to the Sun in its concentration of heavy elements.[6]

The star has a co-moving white dwarf companion WD 0443+270 at a projected separation of 124″,[9] both possibly ejected members of the Hyades cluster. The white dwarf companion has a rather exotic iron core[8] and belongs to spectral class DA9 and has the mass of 0.62±0.02M☉.[10]

Although HD 283750 was classified as a multi-period variable,[11] a paper in 2020 claims its variability is not exceeding the variability of the Sun, and no period can be identified.[12]

HD 283750 is covered by a large amount of starspots, filling up to 28% of the stellar surface at the maxima of the magnetic cycle.[13] In November 1993, the star 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.[11] The flares of HD 283750 are accompanied by particle beams strong enough to affect the polarization properties of the stellar photosphere.[14]

Suspected substellar companion

In 1996 a suspected 50-MJ brown dwarf HD 283750b on a 1.79-day orbit around HD 283750 was detected by the differential Doppler spectroscopy method. By 2007, the mass of the companion was refined to 0.19M☉, making it a red dwarf star.[15]

References

  1. ↑ Strassmeier, K. G.; Bartus, J.; Cutispoto, G.; Rodono, M. (October 1997). "Starspot photometry with robotic telescopes: Continuous UBV and V(RI)_C photometry of 23 stars in 1991-1996". Astron. Astrophys. Suppl. Ser. 125 (1): 11–63. Bibcode:1997A&AS..125...11S. doi:10.1051/aas:1997369. Retrieved 29 June 2022.
  2. ↑ Oláh, K.; Kolláth, Z.; Strassmeier, K. G. (April 2000). "Multiperiodic light variations of active stars". Astronomy and Astrophysics. 356: 643–653. Bibcode:2000A&A...356..643O. Retrieved 29 June 2022.
  3. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  4. 1 2 3 "HD 283750". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 30 June 2021.
  5. 1 2 "V833 Tauri". International Variable Star Index. AAVSO. Retrieved 2022-06-29.
  6. 1 2 3 4 Naftilan, S. A.; Fairchild, K. (1993). "Abundance Analysis of the BY Draconis Variable, Hot Flare Star V833 Tauri". Publications of the Astronomical Society of the Pacific. 105: 565. doi:10.1086/133194. S2CID 121761886.
  7. 1 2 3 4 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.
  8. 1 2 3 Catalán, S.; Ribas, I.; Isern, J.; García-Berro, E. (2007), "WD0433+270: An old Hyades stream member or an Fe-core white dwarf?", Astronomy & Astrophysics, 477 (3): 901–906, arXiv:0710.3999, doi:10.1051/0004-6361:20078230, S2CID 1559222
  9. ↑ Scholz, R.-D.; Meusinger, H.; Jahreiß, H. (2018), "New nearby white dwarfs from Gaia DR1 TGAS and UCAC5/URAT", Astronomy & Astrophysics, 613: A26, arXiv:1711.10778, Bibcode:2018A&A...613A..26S, doi:10.1051/0004-6361/201731753, S2CID 59423840
  10. ↑ Toonen, S.; Hollands, M.; Gänsicke, B. T.; Boekholt, T. (2017), "The binarity of the local white dwarf population", Astronomy & Astrophysics, 602: A16, arXiv:1703.06893, Bibcode:2017A&A...602A..16T, doi:10.1051/0004-6361/201629978, S2CID 12367523
  11. 1 2 Oláh, K.; Strassmeier, K. G.; Kővári, Zs.; Guinan, E. F. (2001). "Time-series photometric spot modeling. IV. The multi-periodic K5Ve binary V833 Tauri". Astronomy & Astrophysics. 372: 119–129. Bibcode:2001A&A...372..119O. doi:10.1051/0004-6361:20010362.
  12. ↑ Frick, P.; Sokoloff, D.; Katsova, M. M.; Bondar', N. I.; Stepanov, R. (2020). "Wavelet analysis of the long-term activity of V833 Tau". Monthly Notices of the Royal Astronomical Society. 495 (4): 3788–3794. arXiv:2005.11136. doi:10.1093/mnras/staa1458.
  13. ↑ Bondar', N. I. (2017). "Photometric period and rotational brightness modulation of V833 Tau". Astronomy Reports. 61 (2): 130–137. Bibcode:2017ARep...61..130B. doi:10.1134/S1063772917010024. S2CID 126233507.
  14. ↑ Saar, S. H.; Martens, P. C. H.; Huovelin, J.; Linnaluoto, S. (1994). "Possible detection of a stellar flare-generated particle beam in polarized light". Astronomy and Astrophysics. 286: 194. Bibcode:1994A&A...286..194S.
  15. ↑ Bonavita, M.; Desidera, S.; Thalmann, C.; Janson, M.; Vigan, A.; Chauvin, G.; Lannier, J. (2016). "SPOTS: The Search for Planets Orbiting Two Stars II. First constraints on the frequency of sub-stellar companions on wide circumbinary orbits". Astronomy and Astrophysics. 593: 593. arXiv:1605.03962. Bibcode:2016A&A...593A..38B. doi:10.1051/0004-6361/201628231. S2CID 55950739.
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