HD 283750

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]

  1. ^ Cite error: The named reference Strassmeier was invoked but never defined (see the help page).
  2. ^ Cite error: The named reference Olah was invoked but never defined (see the help page).
  3. ^ Cite error: The named reference MAST was invoked but never defined (see the help page).
  4. ^ a b c Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  5. ^ a b Cite error: The named reference vsx was invoked but never defined (see the help page).
  6. ^ a b c d Cite error: The named reference Naftilan1993 was invoked but never defined (see the help page).
  7. ^ a b c Cite error: The named reference EDR3 was invoked but never defined (see the help page).
  8. ^ a b c Cite error: The named reference Catalan2007 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Scholz was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Toonen was invoked but never defined (see the help page).
  11. ^ a b 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. ^ Cite error: The named reference Frick was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference Bondar was invoked but never defined (see the help page).
  14. ^ Cite error: The named reference Saar was invoked but never defined (see the help page).