BF Antliae

BF Antliae, or HD 86301, is a variable star in the southern constellation of Antlia. It has a baseline apparent visual magnitude of 6.32,[3] which indicates it lies near the lower limit of visibility for faint stars. The distance to BF Ant, as determined from its annual parallax shift of 6.9 mas,[2] is 473 light years. It is moving further away with a heliocentric radial velocity of +18 km/s.[5]

BF Antliae

A light curve for BF Antliae, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Antlia
Right ascension 09h 56m 54.09215s[2]
Declination −27° 28′ 30.5575″[2]
Apparent magnitude (V) 6.32 (+0.01)[3]
Characteristics
Spectral type A4 V[3]
B−V color index 0.173±0.008[4]
Variable type δ Sct[3]
Astrometry
Radial velocity (Rv)+18.2±0.8[5] km/s
Proper motion (μ) RA: −72.627[2] mas/yr
Dec.: +23.234[2] mas/yr
Parallax (π)6.8977 ± 0.0578 mas[2]
Distance473 ± 4 ly
(145 ± 1 pc)
Absolute magnitude (MV)0.33[4]
Details[6]
Mass2.41±0.05 M☉
Luminosity66.8+11.7
−10.0 L☉
Temperature7,745+53
−71 K
Rotational velocity (v sin i)218.9±1.7[7] km/s
Other designations
BF Ant, CD−26° 7551, HD 86301, HIP 48776, HR 3933, SAO 178216[8]
Database references
SIMBADdata

This is an A-type main-sequence star with a stellar classification of A4 V[3] that is at the end of its main sequence lifespan.[6] It is a Delta Scuti variable that varies by 0.01 of a magnitude.[3] These are short-period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study astroseismology.[9] Handler and Shobbrook (2002) noted that the star lies near the "hot luminous border of the δ Scuti instability strip", and it appears "multiperiodic with a time scale of 3.8–6 hours".[10]

BF Antliae is spinning rapidly with a projected rotational velocity of 219 km/s.[7] It has 2.41 times the mass of the Sun and is radiating 67 times the Sun's luminosity from its photosphere at an effective temperature of 7,745 K.[6]

References
  1. "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 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.
  3. Chang, S.-W.; et al. (2013), "Statistical Properties of Galactic δ Scuti Stars: Revisited", The Astronomical Journal, 145 (5): 10, arXiv:1303.1031, Bibcode:2013AJ....145..132C, doi:10.1088/0004-6256/145/5/132, S2CID 118900730, 132.
  4. 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.
  5. de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  6. Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789, A120.
  7. Díaz, C. G.; et al. (July 2011), "Accurate stellar rotational velocities using the Fourier transform of the cross correlation maximum", Astronomy & Astrophysics, 531: A143, arXiv:1012.4858, Bibcode:2011A&A...531A.143D, doi:10.1051/0004-6361/201016386, S2CID 119286673.
  8. "BF Ant". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 19, 2018.
  9. Templeton, Matthew (16 July 2010). "Delta Scuti and the Delta Scuti Variables". Variable Star of the Season. AAVSO (American Association of Variable Star Observers). Retrieved 5 September 2015.
  10. Handler, G.; Shobbrook, R. R. (June 2002), "On the relationship between the Delta Scuti and Gamma Doradus pulsators", Monthly Notices of the Royal Astronomical Society, 333 (2): 251–262, arXiv:astro-ph/0202152, Bibcode:2002MNRAS.333..251H, doi:10.1046/j.1365-8711.2002.05401.x, S2CID 119062757.
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