41 Tauri

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41 Tauri
The Baby Eagle Nebula LBN777.jpg
41 Tauri is the brightest star on the right of the molecular cloud LBN 777.
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Taurus
Right ascension 04h 06m 36.413s [1]
Declination +27° 35′ 59.64″ [1]
Apparent magnitude  (V)5.19 [2]
Characteristics
Spectral type B9 p Si [3]
U−B color index −0.47 [2]
B−V color index −0.12 [2]
Variable type α2 CVn [4]
Astrometry
Radial velocity (Rv)−2.0 [5]  km/s
Proper motion (μ)RA: +21.153  mas/yr [1]
Dec.: −51.792  mas/yr [1]
Parallax (π)8.0667 ± 0.1063  mas [1]
Distance 404 ± 5  ly
(124 ± 2  pc)
Orbit [6]
Period (P)7.2274 d
Eccentricity (e)0.18
Semi-amplitude (K1)
(primary)		16.60 km/s
Details
Mass 2.9 [6]   M☉
Radius 3.54 [7]   R☉
Luminosity 190 [8]   L☉
Surface gravity (log g)3.87 [9]   cgs
Temperature 12,600 [9]   K
Metallicity [Fe/H]0.43 [9]   dex
Rotational velocity (v sin i)23 [10]  km/s
Age 146 [11]   Myr
Other designations
GS Tau, BD+27°633, HD  25823, HIP  19171, HR  1268, SAO  76455 [12]
Database references
SIMBAD data

41 Tauri is the Flamsteed designation for a single-lined spectroscopic binary system in the zodiacal constellation of Taurus. The star has a visual magnitude of 5.19, [2] making it visible to the naked eye from brighter suburban skies (according to the Bortle scale). Parallax measurements put it at a distance of roughly 404  light years from the Sun. [1]

A light curve for GS Tauri (41 Tauri), plotted from TESS data GSTauLightCurve.png
A light curve for GS Tauri (41 Tauri), plotted from TESS data

This is a chemically peculiar star and was first classified as a silicon star by American astronomer William Morgan in 1933. The stellar spectrum displays an overabundance of heavier elements; [9] particularly silicon and gallium. These abundances may be caused by the magnetic field of the star, which produces concentrations of the observed elements in the outer atmosphere. [14] It is a α² Canum Venaticorum-type variable star, ranging in magnitude from 5.15 down to 5.22. These variations are likely due to large spots or rings on the side of the star being observed. [4]

The star and its companion orbit each other closely with a period of a week and an eccentricity of 0.18. The rotation period of the primary star has become locked to its orbit, so that one face is always pointed toward its companion. The abundance of gallium and silicon varies in a sinusoidal pattern that matches this period. [14]

The primary has around 2.9 times the mass of the Sun, [6] 3.5 times the Sun's radius, [7] and is emitting 190 times the luminosity of the Sun. [8] The effective temperature of the star's photosphere is 12,600 K, [9] giving it the blue-white hue of a B-type star. [15]

Related Research Articles

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Gamma Volantis Star in the constellation Volans

Gamma Volantis, Latinized from γ Volantis, is a wide binary star system in the southern constellation of Volans. Based upon parallax measurements, it is approximately 133 light years from Earth. It is bright enough to be seen with the naked eye and can be found around 9° to the east-southeast of the Large Magellanic Cloud.

14 Aurigae Quadruple star system in the constellation Auriga

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Tau<sup>4</sup> Eridani Star in the constellation Eridanus

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Tau Puppis Star in the southern constellation of Puppis

Tau Puppis, Latinized from τ Puppis, is a star in the southern constellation of Puppis, near the southern constellation boundary with Carina. It is visible to the naked with an apparent visual magnitude of +2.95 and is located at a distance of about 182 light-years from Earth. The variable radial velocity of this system was detected by H. D. Curtis and H. K. Palmer in 1908, based on observations made at the D. O. Mills Observatory. It is a spectroscopic binary star system, with the presence of the secondary component being revealed by the shifts of absorption lines in the spectrum resulting from the Doppler effect. The two components orbit each other with a period of 1,066.0 days and a low eccentricity of 0.090.

HD 85725 is a star in the constellation Antlia. It’s barely visible to the naked eye due to an apparent magnitude of 6.29. Located around 175 light-years away, it is drifting away at a heliocentric radial velocity of 61.95 km/s.

HD 164712 is a giant star in the southern constellation of Apus. It is 229 light-years (70 pc) away and shows indications of an infrared excess, suggesting there may be a dusty disk in orbit around the star.

4 Camelopardalis is a probable multiple star in the northern constellation of Camelopardalis, located 177 light years away from the Sun, based upon parallax. With a combined apparent visual magnitude of 5.29, it is visible to the naked eye as a faint, white-hued star. The pair have a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.158″ per year. The system's proper motion makes it a candidate for membership in the IC 2391 supercluster. They are moving away from the Earth with a heliocentric radial velocity of 22.5 km/s.

HD 27245 is a solitary star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.52, making it faintly visible to the naked eye. Parallax measurements place it approximately 607 light years away from it the Solar System; it is drifting further away with a heliocentric radial velocity of 25.16 km/s.

HD 30442 is a solitary star in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye with an apparent magnitude of 5.47 and is estimated to be 403 light years away from the Solar System. The object has a heliocentric radial velocity of −37 km/s, indicating that it is drifting closer.

Omega1 Cygni, Latinized from ω1 Cygni, is the Bayer designation for a solitary star in the northern constellation of Cygnus. It is visible to the naked eye with an apparent visual magnitude of 4.94. Based upon an annual parallax shift of 2.59 mas, it is estimated to lie roughly 1,260 light years from the Sun. Relative to its neighbors, this star has a peculiar velocity of 25.7±2.2 km/s.

Tau9 Eridani is a binary star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 4.63. The distance to this system can be estimated using the parallax method, which yields a value of roughly 327 light years.

Iota Delphini Star in the constellation Delphinus

Iota Delphini is a star in the constellation Delphinus. It has an apparent magnitude of about 5.4, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Gaia spacecraft, this star is located at a distance of 196 light years.

32 Tauri is the Flamsteed designation for a solitary star in the zodiac constellation of Taurus. It has a visual magnitude of 5.64, making it visible to the naked eye from suburban skies. The position of this star near the ecliptic plane means that it is subject to occultations by the Moon. Parallax measurements put it at a distance of 144 light years from the Sun. It is drifting further away with a radial velocity of +31.9 km/s, having come to within 88.9 light-years some 759,000 years ago.

HD 126053 is the Henry Draper Catalogue designation for a star in the equatorial constellation of Virgo. It has an apparent magnitude of 6.25, which means it is faintly visible to the naked eye. According to the Bortle scale, it requires dark suburban or rural skies to view. Parallax measurements made by the Hipparcos spacecraft provide an estimated distance of 57 light years to this star. It is drifting closer with a heliocentric radial velocity of −19.2 km/s.

9 Ceti G-type star in the constellation Cetus

9 Ceti is the Flamsteed designation for a star in the equatorial constellation of Cetus. It has an apparent visual magnitude of 6.39, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun. There is a magnitude 12.57 optical companion at an angular separation of 214 arc seconds along a position angle of 294°, although the pair are not physically associated as they have different proper motions.

Nu Horologii Star in the constellation Horologium

Nu Horologii, Latinized from ν Horologii, is the Bayer designation for a single star in the southern constellation of Horologium. It was catalogued by the Dutch explorer Frederick de Houtman in 1603. With an apparent visual magnitude of 5.3, this star can be seen with the naked eye from the southern hemisphere. Based upon parallax, Nu Horologii lies at a distance of 169 light-years from Earth. It is drifting closer to the Sun with a radial velocity of +31 km/s.

HD 219623 is a solitary star in the northern circumpolar constellation of Cassiopeia. HD 219623 is its Henry Draper Catalogue designation. It has an apparent visual magnitude of 5.59, which lies in the brightness range that is visible to the naked eye. According to the Bortle scale, it can be observed from dark suburban skies. Parallax measurements place it at an estimated distance of around 67.2 light years. It has a relatively high proper motion, advancing 262 mas per year across the celestial sphere.

HD 33266 is a solitary star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 6.17, making it faintly visible to the naked eye. Located 481 light years away, it is approaching the Sun with a heliocentric radial velocity of −4.4 km/s.

HD 46815 is a solitary star in the southern constellation Columba. It is faintly visible to the naked eye with an apparent magnitude of 5.4 and is estimated to be 408 light years away. However, it is receding with a heliocentric radial velocity of 32.2 km/s.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
  3. ↑ Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819
  4. 1 2 Kukarkin, B. V.; et al. (1971), General Catalogue of Variable Stars (3rd ed.), Bibcode:1971GCVS3.C......0K.
  5. ↑ Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington, D. C.: Carnegie Institute of Washington., Bibcode:1953GCRV..C......0W.
  6. 1 2 3 Ducati, J. R.; et al. (January 2011), "The mass ratio and initial mass functions in spectroscopic binaries", Astronomy and Astrophysics, 525: 9, Bibcode:2011A&A...525A..26D, doi: 10.1051/0004-6361/200913895 , A26.
  7. 1 2 Shulyak, D.; et al. (September 2014), "Interferometry of chemically peculiar stars: theoretical predictions versus modern observing facilities", Monthly Notices of the Royal Astronomical Society, 443 (2): 1629–1642, arXiv: 1406.6093 , Bibcode:2014MNRAS.443.1629S, doi:10.1093/mnras/stu1259.
  8. 1 2 McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv: 1208.2037 , Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID   118665352.
  9. 1 2 3 4 5 Bolcal, C.; et al. (December 1987), "A model atmosphere analysis of HD 25823", Astrophysics and Space Science, 139 (2): 295–304, Bibcode:1987Ap&SS.139..295B, doi:10.1007/BF00644358, S2CID   121253643.
  10. ↑ Freire Ferrero, R.; et al. (February 2012), "High Ionization Species in the Nearby Interstellar Medium from an Exhaustive Analysis of the IUE INES Database", The Astronomical Journal, 143 (2): 38, Bibcode:2012AJ....143...28F, doi: 10.1088/0004-6256/143/2/28 , 28.
  11. ↑ Gontcharov, G. A. (2012), "Dependence of kinematics on the age of stars in the solar neighborhood", Astronomy Letters, 38 (12): 771–782, arXiv: 1606.08814 , Bibcode:2012AstL...38..771G, doi:10.1134/S1063773712120031, S2CID   118345778.
  12. ↑ "41 Tau", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2015-11-09.
  13. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  14. 1 2 Artru, M.-C.; Freire-Ferrero, R. (September 1988), "Line variations in the ultra-violet spectrum of the Ap-Si star HD 25823", Astronomy and Astrophysics, 203 (1): 111–116, Bibcode:1988A&A...203..111A.
  15. ↑ "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.
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