Astronomy:HD 283750

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Short description: Star in the constellation Taurus

Coordinates: Sky map 04h 36m 48.2413s, +27° 07′ 55.8983″

HD 283750
250px
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
Equinox J2000.0]] (ICRS)
Constellation Taurus
Right ascension  04h 36m 48.2422s[4]
Declination 27° 07′ 55.888″[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[4] km/s
Proper motion (μ) RA: +232.17±0.06[4] mas/yr
Dec.: −147.48±0.04[4] mas/yr
Parallax (π)57.49 ± 0.05[4] mas
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
Temperature4,250±100 K
Rotational velocity (v sin i)7.4 km/s
Age1[7] Gyr
Other designations
V833 Tauri, BD+26°730, Gaia DR2 151650076838458112, GJ 171.2, HIP 21482, TYC 1838-564-1, 2MASS J04364822+2707559[8]
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 at 1 billion years.[7] 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[7] and belongs to spectral class DA9 and has the mass of 0.62±0.02 M☉.[10]

In 1981, Lee William Hartmann et al. announced their discovery that the star, then known as BD+26°730, is a variable star.[11][12] It was given its variable star designation, V833 Tauri, in 1985.[13] Although HD 283750 was classified as a multi-period variable,[14] a paper in 2020 claims its variability does not exceed the variability of the Sun, and no period can be identified.[15]

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.[16] 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.[14] The flares of HD 283750 are accompanied by particle beams strong enough to affect the polarization properties of the stellar photosphere.[17]

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 0.19 M☉, making it a red dwarf star.[18]

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. doi:10.1051/aas:1997369. Bibcode: 1997A&AS..125...11S. 
  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. 
  3. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  5. ↑ 5.0 5.1 "V833 Tauri". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=35850. 
  6. ↑ 6.0 6.1 6.2 6.3 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. 
  7. ↑ 7.0 7.1 7.2 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, doi:10.1051/0004-6361:20078230 
  8. ↑ "HD 283750". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+283750. 
  9. ↑ Scholz, R.-D.; Meusinger, H.; Jahreiß, H. (2018), "New nearby white dwarfs from Gaia DR1 TGAS and UCAC5/URAT", Astronomy & Astrophysics 613: A26, doi:10.1051/0004-6361/201731753, Bibcode: 2018A&A...613A..26S 
  10. ↑ Toonen, S.; Hollands, M.; Gänsicke, B. T.; Boekholt, T. (2017), "The binarity of the local white dwarf population", Astronomy & Astrophysics 602: A16, doi:10.1051/0004-6361/201629978, Bibcode: 2017A&A...602A..16T 
  11. ↑ Hartmann, L.; Bopp, B. W.; Dussault, M.; Noah, P. V.; Klimke, A. (October 1981). "Evidence for a starspot cycle on BD +26 730". Astrophysical Journal 249: 662–665. doi:10.1086/159326. Bibcode: 1981ApJ...249..662H. 
  12. ↑ Olah, K.; Pettersen, B. R. (February 1991). "Long-term behaviour of starpots. I. Polar starspots, rotational modulation and flare activity of V 833 Tauri". Astronomy and Astrophysics 242: 443–448. Bibcode: 1991A&A...242..443O. 
  13. ↑ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Perova, N. B. (March 1985). "The 67th Name-List of Variable Stars". Information Bulletin on Variable Stars 2681: 1–32. Bibcode: 1985IBVS.2681....1K. https://ibvs.konkoly.hu/pub/ibvs/2601/2681.pdf. Retrieved 3 September 2025. 
  14. ↑ 14.0 14.1 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. doi:10.1051/0004-6361:20010362. Bibcode: 2001A&A...372..119O. 
  15. ↑ 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. doi:10.1093/mnras/staa1458. 
  16. ↑ Bondar', N. I. (2017). "Photometric period and rotational brightness modulation of V833 Tau". Astronomy Reports 61 (2): 130–137. doi:10.1134/S1063772917010024. Bibcode: 2017ARep...61..130B. 
  17. ↑ 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. 
  18. ↑ 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. doi:10.1051/0004-6361/201628231. Bibcode: 2016A&A...593A..38B. 



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