HD 283750

In this article, we will address the topic of HD 283750 from a comprehensive and analytical perspective, with the aim of offering a complete and detailed vision of this matter. Throughout the text, we will explore different aspects related to HD 283750, from its origin and history to its relevance today. Likewise, we will examine different opinions and theories on the matter, in order to provide the reader with a broad and enriching perspective on HD 283750. In addition, we will present concrete examples and case studies that will help illustrate and exemplify the impact of HD 283750 in various areas. There is no doubt that HD 283750 is a topic of great interest and complexity, which is why it is essential to address it with the depth and rigor it deserves.

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. ^ a b c "HD 283750". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 30 June 2021.
  5. ^ a b "V833 Tauri". International Variable Star Index. AAVSO. Retrieved 2022-06-29.
  6. ^ a b c d 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. ^ 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.
  8. ^ a b c 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. ^ 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. ^ 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.