Astronomy:Beta Tucanae
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| Observation data {{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0 Equinox J2000.0 (ICRS)| Epoch J2000 [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}} | |
|---|---|
| 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[5] mas |
| Distance | 140 ± 1 ly (43.0 ± 0.5 pc) |
| β2 Tuc | |
| Parallax (π) | 19.5923 ± 0.9674[6] mas |
| Distance | 166 ± 8 ly (51 ± 3 pc) |
| Details | |
| β Tuc A | |
| Mass | 3.84[7] M☉ |
| Radius | 2.73[8] R☉ |
| Luminosity | 39[9] L☉ |
| Surface gravity (log g) | 4.37[9] cgs |
| Temperature | 10,726[9] K |
| Rotational velocity (v sin i) | 170[8] km/s |
| β Tuc B | |
| Mass | 0.40[7] M☉ |
| β Tuc Ca | |
| Mass | 2.0[10] M☉ |
| Radius | 1.6[10] R☉ |
| Temperature | 9,200[10] K |
| β Tuc Cb | |
| Mass | 1.45[10] M☉ |
| Radius | 1.4[10] R☉ |
| Temperature | 7,000[10] K |
| β Tuc D | |
| Mass | 1.45[10] M☉ |
| Radius | 1.4[10] R☉ |
| Temperature | 7,000[10] K |
| Other designations | |
| β1: HD 2884, HIP 2484, SAO 248201 | |
| β2: HD 2885, HIP 2487, SAO 248202 | |
| Database references | |
| 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.[11] The system is approximately 140 light years from Earth.
β1, 2 Tucanae
The two brightest stars, Beta1 Tucanae and Beta2 Tucanae, also referred to as Beta Tucanae A (or AB) and Beta Tucanae C (or CD), 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 are binaries. Beta Tucanae B is a magnitude +13.5 star which is a close companion to Beta1, being 2.4 arcseconds, or at least 100 AU away.[3] Beta Tucanae C is a close binary of components Ca and Cb, separated by 0.6 AU.[10] The 6th magnitude Beta Tucanae D, is another A-type star which is separated by approximately 0.38 arcseconds (16 AU) from Beta Tucanae C.[3]
| β1 A | |||||||||||||||||
| Sep = ~100 au | |||||||||||||||||
| β1 B | |||||||||||||||||
| Sep = ~1,200 au | |||||||||||||||||
| β2 Ca | |||||||||||||||||
| Sep = 0.59 au | |||||||||||||||||
| β2 Cb | |||||||||||||||||
| Sep = 22 au | |||||||||||||||||
| β2 D | |||||||||||||||||
| Sep = ~23,000 au | |||||||||||||||||
| β3 | |||||||||||||||||
Hierarchy of orbits in the β Tucanae system[10]
β3 Tucanae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Tucana |
| Right ascension | 00h 32m 43.905s[12] |
| Declination | −63° 01′ 53.40″[12] |
| Apparent magnitude (V) | +5.09[13] |
| Characteristics | |
| Spectral type | A0V[14] |
| Astrometry | |
| Radial velocity (Rv) | 3.60[12] km/s |
| Proper motion (μ) | RA: +86.541[12] mas/yr Dec.: −50.115[12] mas/yr |
| Parallax (π) | 21.6794 ± 0.0683[12] mas |
| Distance | 150.4 ± 0.5 ly (46.1 ± 0.1 pc) |
| Absolute magnitude (MV) | +1.8[15] |
| Details | |
| Mass | 2.0[12] M☉ |
| Radius | 1.7[12] R☉ |
| Luminosity | 19[12] L☉ |
| Surface gravity (log g) | 4.14[12] cgs |
| Temperature | 9,275[12] K |
| Metallicity [Fe/H] | 0.17[16] dex |
| Rotational velocity (v sin i) | 100[16] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Beta3 Tucanae is a suspected 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.
In 1926, Beta3 Tucanae was reported to be a binary, with two components of magnitudes 5.7 and 6.1 separated by 0.1″,[17] although more recent observations could not confirm this.[14][18] At the separation of 0.1″ they would be separated by at least 4 au.[19]
Beta3 Tucanae has an infrared excess, suggesting the presence a debris disk around the primary star.[19]
References
- ↑ 1.0 1.1 1.2 1.3 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 Hoffleit, Dorrit; Jaschek, Carlos (1991). The Bright star catalogue. Bibcode: 1991bsc..book.....H.
- ↑ 3.0 3.1 3.2 "Multiple Star Catalog". http://www.ctio.noao.edu/~atokovin/stars/stars.php?cat=HIP&number=2487. Retrieved 2019-02-19.
- ↑ 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. doi:10.1051/0004-6361/201219774. Bibcode: 2012A&A...546A..69M.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 7.0 7.1 Tokovinin, A. (September 2008). "Comparative statistics and origin of triple and quadruple stars". Monthly Notices of the Royal Astronomical Society 389 (2): 925–938. doi:10.1111/j.1365-2966.2008.13613.x. Bibcode: 2008MNRAS.389..925T.
- ↑ 8.0 8.1 Howe, K. S.; Clarke, C. J. (2009). "An analysis of v sin (I) correlations in early-type binaries". Monthly Notices of the Royal Astronomical Society 392 (1): 448. doi:10.1111/j.1365-2966.2008.14073.x. Bibcode: 2009MNRAS.392..448H.
- ↑ 9.0 9.1 9.2 Stassun, Keivan G. et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S.
- ↑ 10.00 10.01 10.02 10.03 10.04 10.05 10.06 10.07 10.08 10.09 10.10 Waisberg, Idel; Klein, Ygal; Katz, Boaz (May 2025). "Hidden Companions to Intermediate-mass Stars. Upgraded Multiplicity 5 → 6. XXVII. Discovery of a 1.45M⊙, 0.6 au Companion to Beta2 Tucanae C" (in en). Research Notes of the AAS 9 (5): 107. doi:10.3847/2515-5172/add412. ISSN 2515-5172. Bibcode: 2025RNAAS...9..107W.
- ↑ Kaler, Jim. "Beta Tucanae". Stars. University of Illinois. http://stars.astro.illinois.edu/sow/betatuc.html. Retrieved 2 May 2015.
- ↑ 12.00 12.01 12.02 12.03 12.04 12.05 12.06 12.07 12.08 12.09 12.10 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.
- ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". Vizier Online Data Catalog 2237. Bibcode: 2002yCat.2237....0D.
- ↑ 14.0 14.1 Tokovinin, Andrei (2018). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series 235 (1): 6. doi:10.3847/1538-4365/aaa1a5. Bibcode: 2018ApJS..235....6T.
- ↑ Bell, Cameron P. M.; Mamajek, Eric E.; Naylor, Tim (2015). "A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society 454 (1): 593. doi:10.1093/mnras/stv1981. Bibcode: 2015MNRAS.454..593B.
- ↑ 16.0 16.1 Iglesias, D.; Bayo, A.; Olofsson, J.; Wahhaj, Z.; Eiroa, C.; Montesinos, B.; Rebollido, I.; Smoker, J. et al. (2018). "Debris discs with multiple absorption features in metallic lines: Circumstellar or interstellar origin?". Monthly Notices of the Royal Astronomical Society 480 (1): 488. doi:10.1093/mnras/sty1724. Bibcode: 2018MNRAS.480..488I.
- ↑ Van Den Bos, W. H. (1926). "New Southern Double Stars, first list". Bulletin of the Astronomical Institutes of the Netherlands 3: 187. Bibcode: 1926BAN.....3..187V.
- ↑ Waisberg, Idel; Klein, Ygal; Katz, Boaz (2023). "Binarity and beyond in a stars - I. Survey description and first results of VLTI/GRAVITY observations of VAST targets with high Gaia-Hipparcos accelerations". Monthly Notices of the Royal Astronomical Society 521 (4): 5232. doi:10.1093/mnras/stad872. Bibcode: 2023MNRAS.521.5232W.
- ↑ 19.0 19.1 Donaldson, J. K.; Roberge, A.; Chen, C. H.; Augereau, J.-C.; Dent, W. R. F.; Eiroa, C.; Krivov, A. V.; Mathews, G. S. et al. (2012). "Herschelpacs Observations and Modeling of Debris Disks in the Tucana-Horologium Association". The Astrophysical Journal 753 (2): 147. doi:10.1088/0004-637X/753/2/147. Bibcode: 2012ApJ...753..147D.
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