Astronomy:Tau1 Aquarii

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Short description: Star in the constellation Aquarius
For other star systems with this Bayer designation, see Astronomy:Tau Aquarii.
τ1 Aquarii
Location of τ1 Aquarii (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aquarius[1]
Right ascension  22h 47m 42.769s[2]
Declination −14° 03′ 23.14″[2]
Apparent magnitude (V) +5.66[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type B9 V[5]
U−B color index −0.25[6]
B−V color index −0.05[6]
Variable type Constant[7]
Astrometry
Radial velocity (Rv)+15[8] km/s
Proper motion (μ) RA: +30.413[2] mas/yr
Dec.: −9.053[2] mas/yr
Parallax (π)9.1322 ± 0.0557[2] mas
Distance357 ± 2 ly
(109.5 ± 0.7 pc)
Absolute magnitude (MV)+0.74[1]
Details
Mass2.8±0.1[9] M☉
Radius2.56[10] R☉
Luminosity87±2[9] L☉
Surface gravity (log g)4.06[10] cgs
Temperature10,560±70[9] K
Rotational velocity (v sin i)185[4] km/s
Age100+100
−50[9] Myr
Other designations
τ1 Aqr, 69 Aquarii, BD−14 6346, GC 31802, HD 215766, HIP 112542, HR 8673, SAO 165298, PPM 240758, ADS 16268, WDS J22477-1403A[11]
Database references
SIMBADdata

Tau1 Aquarii is a solitary[12] star in the equatorial constellation of Aquarius. Its name is a Bayer designation that is Latinized from τ1 Aquarii, and abbreviated Tau1 Aqr or τ1 Aqr. With an apparent visual magnitude of 5.66,[3] it is a faint naked eye target that requires dark suburban skies for viewing. Parallax measurements yield a distance estimate of approximately 357 light-years (109 parsecs) from the Sun.[2] The star is drifting further away with a radial velocity of +15 km/s.[8] It is a candidate member of the Pisces-Eridanus stellar stream.[13]

The stellar classification of τ1 Aquarii is B9 V;[5] at the borderline between a B- and A-type main sequence star. This is a candidate silicon star; a type of Ap star of class CP2 that shows a magnetic field.[14] It is around 100[15] million years old and is spinning rapidly with a projected rotational velocity of 185 km/s.[4] The star has 2.8 times the mass of the Sun and 2.56 times the Sun's radius. It is radiating 87 times the luminosity of the Sun from its photosphere at an effective temperature of 10,560 K.[9] When examined in the infrared band, it displays an excess emission that is a characteristic of stars with an orbiting debris disk. The model that best fits the data suggests there are two concentric circumstellar disks.[15]

References

  1. ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 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.
  3. ↑ 3.0 3.1 Corben, P. M.; Stoy, R. H. (1968), "Photoelectric Magnitudes and Colours for Bright Southern Stars", Monthly Notes of the Astronomical Society of Southern Africa 27: 11, Bibcode: 1968MNSSA..27...11C. 
  4. ↑ 4.0 4.1 4.2 Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z. 
  5. ↑ 5.0 5.1 Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1988mcts.book.....H. 
  6. ↑ 6.0 6.1 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series 34: 1–49, Bibcode: 1978A&AS...34....1N. 
  7. ↑ Paunzen, E. et al. (July 2021), "Magnetic chemically peculiar stars investigated by the Solar Mass Ejection Imager", Monthly Notices of the Royal Astronomical Society 504 (3): 3758–3772, doi:10.1093/mnras/stab1100, Bibcode: 2021MNRAS.504.3758P. 
  8. ↑ 8.0 8.1 Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Carnegie Institute Washington D.C. Publication (Carnegie Institution of Washington), Bibcode: 1953GCRV..C......0W. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 Pearce, Tim D.; Launhardt, Ralf; Ostermann, Robert; Kennedy, Grant M.; Gennaro, Mario; Booth, Mark; Krivov, Alexander V.; Cugno, Gabriele et al. (2022-03-01), "Planet populations inferred from debris discs. Insights from 178 debris systems in the ISPY, LEECH, and LIStEN planet-hunting surveys", Astronomy and Astrophysics 659: A135, doi:10.1051/0004-6361/202142720, ISSN 0004-6361, Bibcode: 2022A&A...659A.135P. 
  10. ↑ 10.0 10.1 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. 
  11. ↑ "* tau01 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+tau01+Aqr. 
  12. ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  13. ↑ Curtis, Jason L. et al. (August 2019), "TESS Reveals that the Nearby Pisces-Eridanus Stellar Stream is only 120 Myr Old", The Astronomical Journal 158 (2): 11, doi:10.3847/1538-3881/ab2899, 77, Bibcode: 2019AJ....158...77C. 
  14. ↑ Wraight, K. T. et al. (2012), "A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars★", Monthly Notices of the Royal Astronomical Society 420 (1): 757–772, doi:10.1111/j.1365-2966.2011.20090.x, Bibcode: 2012MNRAS.420..757W. 
  15. ↑ 15.0 15.1 Morales, Farisa Y. et al. (April 2011), "Common Warm Dust Temperatures Around Main-sequence Stars", The Astrophysical Journal Letters 730 (2): L29, doi:10.1088/2041-8205/730/2/L29, Bibcode: 2011ApJ...730L..29M, https://authors.library.caltech.edu/24736/1/Morales2011p15446Astrophys_J_Lett.pdf. 



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