AZ Canis Minoris

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AZ Canis Minoris

A blue band light curve for AZ Canis Minoris, adapted from Poretti et al. (1996)[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Canis Minor
Right ascension 07h 44m 07.63294s[2]
Declination +02° 24′ 19.5226″[2]
Apparent magnitude (V) 6.46[3] (6.44 to 6.51)[4]
Characteristics
Spectral type A5 IV[5]
B−V color index 0.211±0.008[3]
Variable type δ Sct[6]
Astrometry
Radial velocity (Rv)+14.9±0.9[3] km/s
Proper motion (μ) RA: −18.963[2] mas/yr
Dec.: −8.672[2] mas/yr
Parallax (π)6.5237 ± 0.1107 mas[2]
Distance500 ± 8 ly
(153 ± 3 pc)
Absolute magnitude (MV)1.01[3]
Details
Mass1.91[7] M☉
Radius3.83+0.20
−0.17[2] R☉
Luminosity48.4±1.0[2] L☉
Surface gravity (log g)3.6[8] cgs
Temperature7,783+138
−201[2] K
Metallicity [Fe/H]0.12[9] dex
Rotational velocity (v sin i)44[10] km/s
Age990[7] Myr
Other designations
AZ CMi, BD+02°1761, GC 10410, HD 62437, HIP 37705, HR 2989, SAO 115864[11]
Database references
SIMBADdata

AZ Canis Minoris is a variable star in the equatorial constellation of Canis Minor. It is just visible to the naked eye in good viewing conditions as a dim, white-hued star with an apparent visual magnitude of around 6.46.[3] The star is located around 500 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +15 km/s.[3] No evidence has been found for a companion to this star,[12] although in the past it has been reported as a binary star system.[13]

This star has a stellar classification of A5 IV,[5] matching an A-type subgiant star. The variable nature of this star was discovered in 1970 at Kitt Peak Observatory.[14] It is a monoperiodic Delta Scuti variable[8] with a cycle period of 2.29 hours and an amplitude of 0.060 in visual magnitude;[6] ranging from a peak magnitude of 6.44 down to 6.51.[4] AZ Canis Minoris is nearly a billion[7] years old with a projected rotational velocity of 44 km/s.[10] It has 1.9[7] times the mass of the Sun and 3.8[2] times the Sun's radius. The star is radiating 48[2] times as much luminosity as the Sun from its photosphere at an effective temperature of 7,783 K.[2]

References

  1. ^ Poretti, E.; Mantegazza, L.; Bossi, M. (August 1996). "The stability of the frequency content in the light curves of the δ Scuti stars HD16439=V663 Cassiopeiae, AZ Canis Minoris, HD 223480=BF Phoenicis". Astronomy & Astrophysics. 312: 912–918. Bibcode:1996A&A...312..912P. Retrieved 12 November 2021.
  2. ^ a b c d e f g h i j k 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.
  3. ^ a b c d e f 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.
  4. ^ a b "AZ CMi". International Variable Star Index. AAVSO. 4 January 2010. Retrieved 14 January 2013.
  5. ^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  6. ^ a b Rodríguez, E.; et al. (June 2000). "A revised catalogue of delta Sct stars". Astronomy and Astrophysics Supplement. 144 (3): 469–474. Bibcode:2000A&AS..144..469R. doi:10.1051/aas:2000221. hdl:10261/226673.
  7. ^ a b c d Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal. 150 (3): 88. arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID 118505114.
  8. ^ a b Poretti, E.; et al. (August 1996). "The stability of the frequency content in the light curves of the δ Scuti stars HD16439=V663 Cassiopeiae, AZ Canis Minoris, HD 223480=BF Phoenicis". Astronomy and Astrophysics. 312: 912−918. Bibcode:1996A&A...312..912P.
  9. ^ Netopil, Martin (August 2017). "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system". Monthly Notices of the Royal Astronomical Society. 469 (3): 3042–3055. arXiv:1705.00883. Bibcode:2017MNRAS.469.3042N. doi:10.1093/mnras/stx1077. S2CID 119034918.
  10. ^ a b Bush, Tabitha C.; Hintz, Eric G. (September 2008). "Rotational Velocity Determinations for 118 δ Scuti Variables". The Astronomical Journal. 136 (3): 1061–1066. Bibcode:2008AJ....136.1061B. doi:10.1088/0004-6256/136/3/1061.
  11. ^ "AZ CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-11.
  12. ^ Liakos, Alexios; Niarchos, Panagiotis (February 2017). "Catalogue and properties of δ Scuti stars in binaries". Monthly Notices of the Royal Astronomical Society. 465 (1): 1181–1200. arXiv:1611.00200. Bibcode:2017MNRAS.465.1181L. doi:10.1093/mnras/stw2756. S2CID 119284575.
  13. ^ Szatmary, Karoly (June 1990). "Pulsating Variable Stars in Binary Systems". The Journal of the American Association of Variable Star Observers. 19 (1): 52–56. Bibcode:1990JAVSO..19...52S.
  14. ^ Percy, J. R. (July 1970). "HR 2989: a New Delta Scuti Star". Information Bulletin on Variable Stars. 444: 1. Bibcode:1970IBVS..444....1P.
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