BF Antliae

BF Antliae
	; A light curve for BF Antliae, plotted from TESS data
Observation data; Epoch J2000 Equinox J2000
Constellation	Antlia
Right ascension	09h 56m 54.09215s
Declination	−27° 28′ 30.5575″
Apparent magnitude (V)	6.32 (+0.01)
Characteristics
Spectral type	A4 V
B−V color index	0.173±0.008
Variable type	δ Sct
Astrometry
Radial velocity (Rv)	+18.2±0.8 km/s
Proper motion (μ)	RA: −72.627 mas/yr ; Dec.: +23.234 mas/yr
Parallax (π)	6.8977 ± 0.0578 mas
Distance	473 ± 4 ly ; (145 ± 1 pc)
Absolute magnitude (MV)	0.33
Details
Mass	2.41±0.05 M☉
Luminosity	66.8+11.7; −10.0 L☉
Temperature	7,745+53; −71 K
Rotational velocity (v sin i)	218.9±1.7 km/s
Other designations
	BF Ant, CD−26° 7551, HD 86301, HIP 48776, HR 3933, SAO 178216
Database references
SIMBAD	data

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]

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

^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
^ ^a ^b ^c ^d ^e ^f 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.
^ ^a ^b ^c ^d ^e ^f 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.
^ ^a ^b 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.
^ ^a ^b 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.
^ ^a ^b ^c 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.
^ ^a ^b 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.
^ "BF Ant". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 19, 2018.
^ 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.
^ 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.