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Beta Tucanae

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β1, 2 Tucanae
Location of β Tucanae group.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Tucana
β1 Tuc (β Tuc AB)
Right ascension 00h 31m 32.6709s[1]
Declination −62° 57′ 29.587″[1]
Apparent magnitude (V) +4.37[2]
β2 Tuc (β Tuc CD)
Right ascension 00h 31m 33.4223s[1]
Declination −62° 57′ 56.134″[1]
Apparent magnitude (V) +4.54[2]
Characteristics
β1 Tuc
Spectral type B9V[3]
β2 Tuc
Spectral type A2V + A7V[4]
Astrometry
β1 Tuc
Parallax (π)23.2596 ± 0.2471 mas[5]
Distance140 ± 1 ly
(43.0 ± 0.5 pc)
β2 Tuc
Parallax (π)19.5923 ± 0.9674 mas[6]
Distance166 ± 8 ly
(51 ± 3 pc)
Details[7]
β Tuc A
Mass3.84 M☉
β Tuc B
Mass0.40 M☉
β Tuc C
Mass2.76 M☉
β Tuc D
Mass1.94 M☉
Other designations
β Tuc, CPD−63°50, GC 625, HR 126, CCDM 00316-6258
β1: HD 2884, HIP 2484, SAO 248201
β2: HD 2885, HIP 2487, SAO 248202
Database references
SIMBADdata
β1
β2

Beta Tucanae, Latinized from β Tucanae, is a group of six stars which appear to be at least loosely bound into a system in the constellation Tucana. Three of the stars are luminous and distinct enough to have been given their own Bayer designations, β1 Tucanae through β3 Tucanae.[8] The system is approximately 140 light years from Earth.

β1, 2 Tucanae

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Simulated image of the β Tucanae system

The two brightest stars, Beta1 Tucanae and Beta2 Tucanae, also referred to as Beta Tucanae A and Beta Tucanae C, are 27 arcseconds, or at least 1100 astronomical units (AU) apart. They are both main sequence dwarfs, Beta1 a blue-white B-type star with an apparent magnitude of +4.36, and Beta2 a white A-type star with an apparent magnitude of +4.53.

Both of these bright stars have at least one closer main sequence companion. Beta Tucanae B is a magnitude +13.5 M3-type star which is a close companion to Beta1, being 2.4 arcseconds, or at least 100 AU away. Beta2's companion, the 6th magnitude Beta Tucanae D, is another A-type star which is separated by approximately 0.38 arcseconds (16 AU) from Beta2.

β3 Tucanae

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β3 Tucanae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Tucana
Right ascension 00h 32m 43.8s
Declination −63° 01′ 52″
Apparent magnitude (V) combined: +5.07

AB: 5.8 + 6.0

Distance152 ± 3 ly
(46 ± 1 pc)
Spectral typeA0V+A2V
Other designations
CPD−63 52, GC 651, HD 3003, HIP 2578, HR 136, SAO 248208, CCDM 00327-6302

Beta3 Tucanae is a binary star which is separated from Beta1 and Beta2 Tucanae by 9 arcminutes on the sky, which puts the two systems at least 23 000 astronomical units (AU) or 0.37 light years apart. It is not clear how tightly Beta3 Tucanae is gravitationally bound to the rest of the β Tucanae system, but all the stars have similar distances from Earth and have the same proper motion on the sky, indicating they are gravitationally influencing each other to some degree.

Both components of the binary system are white A-type main sequence stars and they have apparent magnitudes of +5.8 and +6.0. They are separated by 0.1 arcseconds, or at least 4 astronomical units.

Beta3 Tucanae has an infrared excess, suggesting the presence a debris disk around the primary star. The distance of the other star to the debris disk is not known.[9]

β Tucanae system

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Beta1a's binary companion, Beta1b, orbits at a bit over three times Neptune's distance from the Sun. The Beta2 pair is located over ten times further away. The pair is separated by less than the distance from the Sun to Uranus. The Beta3 pair is much further out, at one-and-a-half times the distance of Proxima Centauri from the main Alpha Centauri pair. The Beta3 pair are separated by less distance than the Sun and Jupiter.

References

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  1. ^ a b c d 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. ^ a b Hoffleit, Dorrit; Jaschek, Carlos (1991). The Bright star catalogue. Bibcode:1991bsc..book.....H.
  3. ^ "Multiple Star Catalog". Archived from the original on 2019-02-20. Retrieved 2019-02-19.
  4. ^ Malkov, O. Yu; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (2012). "Dynamical masses of a selected sample of orbital binaries". Astronomy and Astrophysics. 546: A69. Bibcode:2012A&A...546A..69M. doi:10.1051/0004-6361/201219774.
  5. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  6. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  7. ^ Tokovinin, A. (September 2008). "Comparative statistics and origin of triple and quadruple stars". Monthly Notices of the Royal Astronomical Society. 389 (2): 925–938. arXiv:0806.3263. Bibcode:2008MNRAS.389..925T. doi:10.1111/j.1365-2966.2008.13613.x. S2CID 16452670.
  8. ^ Kaler, Jim. "Beta Tucanae". Stars. University of Illinois. Retrieved 2 May 2015.
  9. ^ Donaldson, J. K.; Roberge, A.; Chen, C. H.; Augereau, J.-C.; Dent, W. R. F.; Eiroa, C.; Krivov, A. V.; Mathews, G. S.; Meeus, G.; Ménard, F.; Riviere-Marichalar, P.; Sandell, G. (2012). "Herschelpacs Observations and Modeling of Debris Disks in the Tucana-Horologium Association". The Astrophysical Journal. 753 (2): 147. arXiv:1206.6358. Bibcode:2012ApJ...753..147D. doi:10.1088/0004-637X/753/2/147. hdl:10486/662289.
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