λ Tauri
Location of λ Tauri (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Taurus
Right ascension 04h 00m 40.81572s[1]
Declination +12° 29′ 25.2259″[1]
Apparent magnitude (V) +3.37 (- 3.54) - 3.91[2]
Characteristics
Spectral type B3 V + A4 IV[3]
U−B color index −0.62[4]
B−V color index −0.12[4]
Variable type Algol[2]
Astrometry
Radial velocity (Rv)+17.8[5] km/s
Proper motion (μ) RA: −8.02[1] mas/yr
Dec.: −14.42[1] mas/yr
Parallax (π)6.74 ± 0.17 mas[1]
Distance480 ± 10 ly
(148 ± 4 pc)
Absolute magnitude (MV)−2.45[6]
Orbit[7]
Primaryλ Tau A
Companionλ Tau B
Period (P)3.9529552 days
Semi-major axis (a)21.91 R☉[8]
Eccentricity (e)0.025±0.015
Inclination (i)76[9]°
Periastron epoch (T)2,444,667.3±2.1 HJD
Semi-amplitude (K1)
(primary)		56.9±0.6 km/s
Semi-amplitude (K2)
(secondary)		215.6±0.7 km/s
Details
λ Tau A
Mass7.18[9] M☉
Radius6.40[9] R☉
Luminosity5,801[3] L☉
Surface gravity (log g)3.38[10] cgs
Temperature18,700[3] K
Rotational velocity (v sin i)85[8] km/s
Age33.2±3.9[11] Myr
λ Tau B
Mass1.89[9] M☉
Radius5.30[9] R☉
Luminosity128[3] L☉
Temperature8,405[3] K
Rotational velocity (v sin i)76[8] km/s
Other designations
35 Tauri, BD+12 539, FK5 150, HD 25204, HIP 18724, HR 1239, SAO 93719.[12]
Database references
SIMBADdata

Lambda Tauri (λ Tau, λ Tauri) is a triple star system in the constellation Taurus. In the Calendarium of Al Achsasi Al Mouakket, this star was designated Sadr al Tauri, which was translated into Latin as Pectus Tauri, meaning "the bull chest".[13] In 1848, the light from this system was found to vary periodically and it was determined to be an eclipsing binary system—the third such discovered.[7] The components of this system have a combined apparent visual magnitude of +3.37 at its brightest, making it one of the brighter members of the constellation. Based upon parallax measurements from the Hipparcos mission, the distance to this system is approximately 480 light-years (150 parsecs).[1]

System

A light curve for Lambda Tauri, plotted from TESS data[14]

The inner pair of this triple star system, Lambda Tauri AB, orbit around each other with a period of 3.95 days and a low eccentricity of about 0.025.[7] Their orbital plane is inclined by around 76° to the line of sight from the Earth,[9] so it is being viewed from nearly edge on and the two stars form an Algol-like eclipsing binary system. The combined brightness of the pair varies from magnitude +3.37 to +3.91 as first one star and then the other pass in front of its companion. The primary member, λ Tau A, undergoes a decrease of 0.435±0.050 in magnitude during an eclipse, while the secondary component, λ Tau B, decreases by 0.09–0.10 in magnitude.[15] The mean physical separation between these two stars is estimated at 21.91 times the radius of the Sun, or 0.1 Astronomical Units.[8]

The primary component has a stellar classification of B3 V, making this a massive B-type main sequence star. It has over seven times the mass of the Sun[15] and 6.4 times the Sun's radius.[8] This star is the brightest member of the system, radiating about 5,801[3] times the luminosity of the Sun from its outer envelope at an effective temperature of 18,700 K, which gives it a blue-white hue common to the B-type stars.[16] Lambda Tauri A is rotating rapidly with a projected rotational velocity of 85 km/s.[8] It, along with δ Librae, were the first stars on which rotational line broadening was observed, by Frank Schlesinger in 1909.[17]

The third component, λ Tau C, is orbiting the inner pair over a 33.025 day period with an eccentricity of roughly 0.15. The orbital plane of this component is nearly coplanar with the orbit of Lambda Tauri AB, differing by no more than 7°. It has about half the mass of the Sun.[15] The orbit of this star causes perturbation effects on the orbit of the AB pair, resulting in periodic changes in their orbital eccentricity and other orbital elements.[7]

Physical characteristics

The spectrum of Lambda Tauri A shows an under abundance of carbon relative to the norm for this category of star. A possible explanation for this is a loss of mass by the star some time in the past. An inner region of the star became depleted by the conversion of carbon into nitrogen during the nuclear fusion process, and this region was later exposed when the outer envelope of the star was lost. Alternatively, the star may have undergone a period of convective mixing, bringing the carbon-depleted material to the surface. However, the cause of such a fully convective behavior in a main sequence star of this mass is unclear.[10]

The secondary companion has a stellar classification of A4 IV,[3] suggesting that it is a subgiant star that has nearly exhausted the supply of hydrogen at its core and is in the process of evolving into a giant star. It has nearly 1.9 times the mass of the Sun, 5.3 times the Sun's radius,[8] and is radiating 128 times the Sun's luminosity at an effective temperature of 8,405 K.[3] As with the primary, this star is spinning rapidly with a projected rotational velocity of 76 km/s.[8] The side of the secondary facing the more massive star is being heated by an additional 1,440 K, which produces a rotational effect that causes the strength of the secondary's spectral lines to vary over the course of its orbit.[7]

A conundrum with this system is the large radius of the secondary star. In stellar evolutionary terms, the more massive primary should be the first to reach the subgiant stage. Hence the enlarged radius of the secondary must be caused by a means other than the star's age. This suggests that the pair Lambda Tauri AB form a semidetached binary with the secondary filling its Roche lobe, giving it a distorted shape.[7]

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
  2. 1 2 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869
  3. 1 2 3 4 5 6 7 8 Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349–360, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483
  4. 1 2 Nicolet, B. (October 1978). "Catalogue of homogeneous data in the UBV photoelectric photometric system". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
  5. ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E
  6. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  7. 1 2 3 4 5 6 Fekel, F. C. Jr.; Tomkin, J. (December 1982), "Secondaries of eclipsing binaries. IV - The triple system Lambda Tauri", Astrophysical Journal, Part 1, 263: 289–301, Bibcode:1982ApJ...263..289F, doi:10.1086/160503, hdl:2152/34674
  8. 1 2 3 4 5 6 7 8 Vesper, David; Honeycutt, Kent; Hunt, Thomas (May 2001), "Survey of Hα Mass Transfer Structures in Classical Algol-Type Binaries", The Astronomical Journal, 121 (5): 2723–2736, Bibcode:2001AJ....121.2723V, doi:10.1086/320381
  9. 1 2 3 4 5 6 Dervişoğlu, A.; Tout, Christopher A.; Ibanoğlu, C. (August 2010), "Spin angular momentum evolution of the long-period Algols", Monthly Notices of the Royal Astronomical Society, 406 (2): 1071–1083, arXiv:1003.4392, Bibcode:2010MNRAS.406.1071D, doi:10.1111/j.1365-2966.2010.16732.x, S2CID 119198387
  10. 1 2 Cugier, H.; Hardorp, J. (August 1988), "Carbon abundance in Beta Persei and Lambda Tauri", Astronomy and Astrophysics, 202 (1–2): 101–108, Bibcode:1988A&A...202..101C
  11. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873
  12. ↑ "HD 25204 -- Eclipsing binary of Algol type", SIMBAD Astronomical Database, retrieved 2007-01-26
  13. ↑ Knobel, E. B. (June 1895), "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of", Monthly Notices of the Royal Astronomical Society, 55: 429–438, Bibcode:1895MNRAS..55..429K, doi:10.1093/mnras/55.8.429
  14. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  15. 1 2 3 Soderhjelm, S. (August 1975), "The three-body problem and eclipsing binaries – Application to algol and lambda Tauri", Astronomy and Astrophysics, 42 (2): 229–236, Bibcode:1975A&A....42..229S
  16. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
  17. ↑ Schlesinger, Frank (1911), "Rotation of Stars about their Axes", Monthly Notices of the Royal Astronomical Society, 71 (9): 719, Bibcode:1911MNRAS..71..719S, doi:10.1093/mnras/71.9.719
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