Epsilon Tucanae

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Epsilon Tucanae
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Tucana
Right ascension 23h 59m 54.97761s [1]
Declination −65° 34′ 37.6804″ [1]
Apparent magnitude  (V)+4.50 [2]
Characteristics
Spectral type B8 V [3] or B9 IV [4]
U−B color index −0.28 [2]
B−V color index −0.08 [2]
Astrometry
Radial velocity (Rv)+8.8±2.8 [5]  km/s
Proper motion (μ)RA: +47.93 [1]   mas/yr
Dec.: −22.95 [1]   mas/yr
Parallax (π)8.74 ± 0.18  mas [1]
Distance 373 ± 8  ly
(114 ± 2  pc)
Absolute magnitude  (MV)−0.80 [6]
Details
Mass 4.00±0.20 [3]   M☉
Luminosity 389 [3]   L☉
Surface gravity (log g)3.9±0.1 [3]   cgs
Temperature 13,000±500 [3]   K
Rotation 0.79318(8) [7] d
Rotational velocity (v sin i)300±20 [3]  km/s
Age 123 [3]   Myr
Other designations
ε Tuc, CPD−66° 3819, FK5  903, HD  224686, HIP  118322, HR  9076, SAO  255619 [8]
Database references
SIMBAD data

Epsilon Tucanae (ε Tuc, ε Tucanae) is a solitary [9] star in the southern constellation of Tucana. With an apparent visual magnitude of +4.50, [2] it is faintly visible to the naked eye. Based upon an annual parallax shift of 8.74  mas as seen from Earth, it is located around 373  light years from the Sun.

Levenhagen and Leister (2008) classified this star as B8 V, [3] indicating a blue-white hued B-type main sequence star. However, Hiltner, Garrison, and Schild (1969) listed it with a classification of B9 IV, [4] suggesting it may be a more evolved subgiant star. It is a rapidly rotating Be star that is an estimated 78% of the way through its main sequence lifetime. [10] The projected rotational velocity is 300 km/s, [3] which is giving it an oblate shape with an equatorial bulge that is an estimated 36% larger than the polar radius. [11] It has a weak magnetic field with a strength of 74±24  G . [12]

It is the last star in the Hipparcos catalogue, HIP 118322, from the Hipparcos (1989–1993) astrometry satellite.

Related Research Articles

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Zeta Sculptoris, Latinized from ζ Sculptoris, is a multiple star system in the constellation Sculptor. It is faintly visible to the naked eye with an apparent magnitude of 5.04. The annual parallax shift is 6.49 mas, which yields a distance estimate of about 500 light years from the Sun. It is moving further away with a radial velocity of +8.6 km/s. Zeta Sculptoris is near the Blanco 1 cluster as viewed from Earth, although parallax measurements indicate it to be substantially closer.

<span class="mw-page-title-main">Epsilon Trianguli</span> Binary star in the constellation Triangulum

Epsilon Trianguli, Latinized from ε Trianguli, is a binary star system in the northern constellation of Triangulum. Based upon measurement of its trigonometric parallax, it is approximately 390 light years from Earth.

Kappa Tucanae, Latinised from, κ Tucanae, is a quadruple star system in the southern constellation Tucana. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of either +4.25 or +4.86, depending on the source. The system is located approximately 68 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8 km/s.

Delta Tucanae is a common proper motion pair located in the southwestern corner of the southern constellation of Tucana. Based upon an annual parallax shift of 13.00 mas as seen from Earth, is approximately 250 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +4.48. As of 2013, the two components had an angular separation of 7.0 arc seconds along a position angle of 282°.

<span class="mw-page-title-main">Iota Tucanae</span> Star in the constellation Tucana

Iota Tucanae is a solitary star in the southern constellation of Tucana. Based upon an annual parallax shift of 10.72 mas as seen from Earth, it is located around 304 light years from the Sun. With an apparent visual magnitude of +5.33, it is faintly visible to the naked eye.

Rho Tucanae is a binary star system in the southern constellation of Tucana. It is visible to the naked eye with a combined apparent visual magnitude of +5.38. Based upon an annual parallax shift of 24.37 mas as seen from Earth, it is located 131 light years from the Sun.

Pi Tucanae is a double star in the southern constellation of Tucana. It is visible to the naked eye with a combined apparent visual magnitude of +5.49. Based upon an annual parallax shift of 10.25 mas as seen from Earth, it is located around 317 light years from the Sun.

<span class="mw-page-title-main">Kappa Volantis</span> Quadruple star system in the constellation Volans

Kappa Volantis, Latinized from κ Volantis, is a quadruple star system in the southern constellation of Volans. The primary component has an apparent visual magnitude of 5.37, while the secondary companion is magnitude 5.65; individually, both a bright enough to be faintly visible to the naked eye. Based upon parallax measurements, the stars appear to be around 420−430 light-years from the Sun.

<span class="mw-page-title-main">Kappa Canis Majoris</span> Star in the constellation Canis Major

Kappa Canis Majoris, Latinized from κ Canis Majoris, is a solitary, blue-white hued star in the constellation Canis Major. It is visible to the naked eye with an apparent visual magnitude of +3.87. Based upon an annual parallax shift of 7.70 mas as seen from Earth, this star is located about 660 light years from the Sun.

<span class="mw-page-title-main">10 Canis Majoris</span> Star in the constellation Canis Major

10 Canis Majoris is a single variable star in the southern constellation of Canis Major, located roughly 1,980 light years away from the Sun. It has the variable star designation FT Canis Majoris; 10 Canis Majoris is the Flamsteed designation. This body is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.23. It is moving away from the Earth with a heliocentric radial velocity of +34 km/s.

Mu Crucis, Latinized from μ Crucis, is the seventh-brightest star in the constellation Crux commonly known as the Southern Cross. μ Crucis is a wide double star of spectral class B stars, magnitude 4.0 and 5.2 respectively. They lie about 370 light-years away, and both stars are likely physically attached. The brighter component is known as μ1 Crucis or μ Crucis A, while the fainter is μ2 Crucis or μ Crucis B.

HD 79447 is a single star in the southern constellation of Carina. It has the Bayer designation i Carinae, while HD 79447 is the identifier from the Henry Draper catalogue. This star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude of +3.96. It is located at a distance of approximately 540 light years from the Sun based on parallax, and has an absolute magnitude of −2.14. The star drifting further away with a radial velocity of +18 km/s. It is a candidate member of the Lower Centaurus–Crux group of the Sco OB2 association.

<span class="mw-page-title-main">Rho Centauri</span> Binary star system in the constellation Centaurus

Rho Centauri, Latinized from ρ Centauri, is a binary star system in the southern constellation of Centaurus. It is visible to the naked eye as a blue-white hued point of light with a combined apparent visual magnitude of +3.97. The system is located approximately 276 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +15 km/s. It is a proper motion member of the Lower Centaurus–Crux sub-group in the Scorpius–Centaurus OB association, the nearest such association of co-moving massive stars to the Sun.

HD 124639 is a Be star in the southern constellation of Apus. It has an apparent visual magnitude of 6.42, which makes it a challenge to view with the naked eye even under the best viewing conditions. Based upon an annual parallax shift of 3.41 mas as seen from Earth, it is 956 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction of 0.17 due to interstellar dust. The star is moving further away with a heliocentric radial velocity of +27 km/s.

μ Mensae, Latinized as Mu Mensae, is a solitary, blue-white hued star in the southern constellation of Mensa. With an apparent visual magnitude of 5.54, it is just bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 6.8405 mas as seen from GAIA, this star is located roughly 477 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.09 due to interstellar dust.

Kappa Eridani, Latinized from κ Eridani, is a solitary star in the constellation Eridanus. With an apparent visual magnitude of 4.25, it is bright enough to be visible to the naked eye on a dark night. Based upon an annual parallax shift of 0.00642 arc seconds, it is roughly 510 light years distant from the Sun.

Kappa1 Lupi is a solitary star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 3.86, and forms a double star with Kappa2 Lupi. Based upon an annual parallax shift of 18.12 mas as seen from Earth, it is located about 180 light years from the Sun. Both Kappa1 Lupi and its neighbor Kappa2 Lupi are members of the Hyades Stream, which is a moving group that is coincident with the proper motions of the Hyades cluster.

<span class="mw-page-title-main">KT Lupi</span> Visual binary star system in the constellation of Lupus

KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of 2.19″±0.03″. Based upon an annual parallax shift of 7.6 mas as seen from Earth's orbit, it is located 430 light-years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +6.5 km/s. It is a member of the Lower Centaurus–Crux sub-group of the Scorpius–Centaurus association.

<span class="mw-page-title-main">N Scorpii</span> Star in the constellation of Scorpius

N Scorpii, also known as HD 148703, is a solitary, bluish-white hued star located in the southern constellation Scorpius. It has an apparent magnitude of 4.23, making it readily visible to the naked eye. N Scorpii was initially given the Bayer designation Alpha Normae by Lacaille but it was later moved from Norma to Scorpius. N Scorpii is currently located 550 light years away based on parallax measurements from the Hipparcos satellite and is part of the Upper Scorpius–Centaurus region of the Scorpius–Centaurus association.

<span class="mw-page-title-main">DS Tucanae</span> Binary star system in the constellation of Tucana

DS Tucanae is a binary star system 144 light years away in the constellation of Tucana. It has an apparent visual magnitude of 8.5, and is a RS Canum Venaticorum variable. The system is notable for being young as a member of the 45 Myr old Tucana-Horologium moving group and for the primary star hosting the confirmed exoplanet DS Tucanae Ab, discovered by THYME, using TESS.

References

  1. 1 2 3 4 5 van Leeuwen, F. (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 3 4 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  3. 1 2 3 4 5 6 7 8 9 Levenhagen, R. S.; Leister, N. V. (2006), "Spectroscopic Analysis of Southern B and Be Stars", Monthly Notices of the Royal Astronomical Society , 371 (1): 252–62, arXiv: astro-ph/0606149 , Bibcode:2006MNRAS.371..252L, doi:10.1111/j.1365-2966.2006.10655.x, S2CID   16492030.
  4. 1 2 Hiltner, W. A.; et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal, 157: 313, Bibcode:1969ApJ...157..313H, doi: 10.1086/150069 .
  5. ↑ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv: 1606.08053 , Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID   119231169.
  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. ↑ Barraza, L. F.; Gomes, R. L.; Messias, Y. S.; Leão, I. C.; Almeida, L. A.; Janot-Pacheco, E.; Brito, A. C.; Brito, F. A. C.; Santana, J. V.; Gonçalves, N. S.; Das Chagas, M. L.; Teixeira, M. A.; De Medeiros, J. R.; Canto Martins, B. L. (2022). "Rotation Signature of TESS B-type Stars. A Comprehensive Analysis". The Astrophysical Journal. 924 (2): 117. arXiv: 2202.01022 . Bibcode:2022ApJ...924..117B. doi: 10.3847/1538-4357/ac3335 . S2CID   246030494.
  8. ↑ "eps Tuc -- Be Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg , retrieved 2017-04-22.
  9. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society , 389 (2): 869–879, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID   14878976.
  10. ↑ Zorec, J.; et al. (October 2005), "On the evolutionary status of Be stars. I. Field Be stars near the Sun", Astronomy and Astrophysics, 441 (1): 235–248, arXiv: astro-ph/0509119 , Bibcode:2005A&A...441..235Z, doi:10.1051/0004-6361:20053051, S2CID   17592657.
  11. ↑ Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv: 1204.2572 , Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID   119273474.
  12. ↑ Hubrig, S.; et al. (July 2009), "Magnetic survey of emission line B-type stars with FORS 1 at the VLT", Astronomische Nachrichten, 330 (7): 708, arXiv: 0907.0882 , Bibcode:2009AN....330..708H, doi:10.1002/asna.200911236, S2CID   13620067.
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