Astronomy:V471 Tauri

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Short description: Variable star in the constellation Taurus
V471 Tauri
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A light curve for V471 Tauri, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Taurus
Right ascension  03h 50m 24.9667s[2]
Declination 17° 14′ 47.431″[2]
Apparent magnitude (V) 9.40 - 9.71[3]
Characteristics
Evolutionary stage K2V + D2[4]
Variable type Algol + RS CVn[3]
Astrometry
Radial velocity (Rv)37.4±0.5[5] km/s
Proper motion (μ) RA: 127.278[2] mas/yr
Dec.: −22.321[2] mas/yr
Parallax (π)21.0129 ± 0.0158[2] mas
Distance155.2 ± 0.1 ly
(47.59 ± 0.04 pc)
Orbit[6]
Period (P)0.52118 days
Semi-major axis (a)0.01496 AU
Eccentricity (e)0 (assumed)
Inclination (i)80.8°
Details
White dwarf
Mass0.792[6] M☉
Radius0.01134[6] R☉
Luminosity0.145[7] L☉
Surface gravity (log g)8.227[6] cgs
Temperature34,500[7] K
K star
Mass0.852[6] M☉
Radius0.816[6] R☉
Luminosity0.41[8] L☉
Surface gravity (log g)4.49[9] cgs
Temperature5,066[9] K
Rotation0.5211 days[8]
Rotational velocity (v sin i)89.30[9] km/s
Age625[9] Myr
Other designations
471 Tau, BD+16°516, HIP 17962
Database references
SIMBADdata

V471 Tauri (short V471 Tau) is an eclipsing variable star in the constellation of Taurus. The star has a visual magnitude of 9 which makes it impossible to see with the naked eye. It is around 155 light-years away from the Solar System, in the Hyades star cluster.[6]

In 1970, Burt Nelson and Arthur Young announced that the star is a variable star.[10] It was given its variable star designation in 1972.

Physical properties

The V471 Tauri system has at least two members: a white dwarf star of spectral type D2; and a K-type main sequence star (K2 V), together a post-common envelope binary.[6][11] There are variations in the timing of the eclipses that were once thought to be due to a third member of the system, proposed to be a brown dwarf, but a direct imaging search for this object with SPHERE resulted in a non-detection.[12] The eclipse variations may be caused by the Applegate mechanism,[13] or the third body may be a pair of smaller brown dwarfs, which would be too faint to have been detected.[7] Later studies have found that the timing variations cannot be explained solely by additional components of the system; even if one or more brown dwarfs are present, the Applegate mechanism must also be a factor.[14]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 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.
  3. ↑ 3.0 3.1 Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  4. ↑ Hussain, G. A. J.; Allende Prieto, C.; Saar, S. H.; Still, M. (2006). "Spot patterns and differential rotation in the eclipsing pre-cataclysmic variable binary, V471 Tau". Monthly Notices of the Royal Astronomical Society 367 (4): 1699–1708. doi:10.1111/j.1365-2966.2006.10073.x. Bibcode: 2006MNRAS.367.1699H. 
  5. ↑ Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R. et al. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society 349 (3): 1069–1092. doi:10.1111/j.1365-2966.2004.07588.x. Bibcode: 2004MNRAS.349.1069K. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 Muirhead, Philip S.; Nordhaus, Jason; Drout, Maria R. (2022). "Revised Stellar Parameters for V471 Tau, A Post-common Envelope Binary in the Hyades". The Astronomical Journal 163 (1): 34. doi:10.3847/1538-3881/ac390f. Bibcode: 2022AJ....163...34M. 
  7. ↑ 7.0 7.1 7.2 Vaccaro, T. R.; Wilson, R. E.; Van Hamme, W.; Terrell, Dirk (2015). "The V471 Tauri System: A Multi-data-type Probe". The Astrophysical Journal 810 (2): 157. doi:10.1088/0004-637X/810/2/157. Bibcode: 2015ApJ...810..157V. 
  8. ↑ 8.0 8.1 Kővári, Zs; Kriskovics, L.; Oláh, K.; Odert, P.; Leitzinger, M.; Seli, B.; Vida, K.; Borkovits, T. et al. (2021). "A confined dynamo: Magnetic activity of the K-dwarf component in the pre-cataclysmic binary system V471 Tauri". Astronomy and Astrophysics 650: A158. doi:10.1051/0004-6361/202140707. Bibcode: 2021A&A...650A.158K. 
  9. ↑ 9.0 9.1 9.2 9.3 Zaire, B.; Donati, J. -F.; Klein, B. (2021). "Magnetic field and activity phenomena of the K2 dwarf V471 Tau". Monthly Notices of the Royal Astronomical Society 504 (2): 1969. doi:10.1093/mnras/stab1019. Bibcode: 2021MNRAS.504.1969Z. 
  10. ↑ Nelson, Burt; Young, Arthur (June 1970). "A New Eclipsing Binary Containing a Very Hot White Dwarf". Publications of the Astronomical Society of the Pacific 82 (487): 699-706. doi:10.1086/128946. Bibcode: 1970PASP...82..699N. https://articles.adsabs.harvard.edu/pdf/1970PASP...82..699N. Retrieved 4 September 2025. 
  11. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (September 1972). "58th Name-List of Variable Stars". Information Bulletin on Variable Stars 717: 1-36. Bibcode: 1972IBVS..717....1K. https://ibvs.konkoly.hu/pub/ibvs/0701/0717.pdf. Retrieved 4 September 2025. 
  12. ↑ "The Strange Case of the Missing Dwarf". ESO. 18 February 2015. https://www.eso.org/public/news/eso1506/. 
  13. ↑ Hardy, A. et al. (February 2015). "The First Science Results from Sphere: Disproving the Predicted Brown Dwarf Around V471 Tau". The Astrophysical Journal Letters 800 (2): L24. doi:10.1088/2041-8205/800/2/L24. Bibcode: 2015ApJ...800L..24H. 
  14. ↑ Kundra, Emil et al. (December 2022). "Variability of eclipse timing: the case of V471 Tauri". Monthly Notices of the Royal Astronomical Society 517 (4): 5358–5367. doi:10.1093/mnras/stac2812. Bibcode: 2022MNRAS.517.5358K. 



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