BU Canis Minoris

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BU Canis Minoris
BUCMiLightCurve.png
A light curve for BU Canis Minoris, plotted from TESS data [1]
Observation data
Epoch J2000        Equinox J2000
Constellation Canis Minor
Right ascension 07h 58m 05.89734s [2]
Declination 07° 12′ 48.7030″ [2]
Apparent magnitude  (V)6.42 [3]
Characteristics
Spectral type A0V [4]
B−V color index −0.031±0.008 [3]
Astrometry
Radial velocity (Rv)+34.0±6.5 [3]  km/s
Proper motion (μ)RA: −9.407 [2]   mas/yr
Dec.: −11.835 [2]   mas/yr
Parallax (π)4.0663 ± 0.0568 [2]   mas
Distance 800 ± 10  ly
(246 ± 3  pc)
Absolute magnitude  (MV)−0.38 [3]
Details [5]
BU CMi Aa
Mass 3.40 ± 0.10  M☉
Radius 2.51 ± 0.05  R☉
Surface gravity (log g)4.088 ± 0.010  cgs
Temperature 10130 ± 80  K
BU CMi Ab
Mass 3.11 ± 0.10  M☉
Radius 1.80 ± 0.05  R☉
Surface gravity (log g)4.338 ± 0.010  cgs
Temperature 9740 ± 80  K
BU CMi Ba
Mass 3.29 ± 0.10  M☉
Radius 2.31 ± 0.05  R☉
Surface gravity (log g)4.148 ± 0.010  cgs
Temperature 10180 ± 80  K
BU CMi Bb
Mass 3.29 ± 0.10  M☉
Radius 2.04 ± 0.05  R☉
Surface gravity (log g)4.259 ± 0.010  cgs
Temperature 9890 ± 80  K
Other designations
BU CMi, BD+07°1879, HD  65241, HIP  38945, HR  3103, SAO  116179 [6]
Database references
SIMBAD data

BU Canis Minoris is a quadruple star system in the equatorial constellation of Canis Minor. It has the Henry Draper Catalogue designation of HD 65241, while BU Canis Minoris is its variable star designation. The system is a challenge to view with the naked eye, having a peak apparent visual magnitude of 6.42. [3] It is located at a distance of approximately 700  light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of about +34 km/s. [3]

In 2021, BU Canis Majoris was found to be composed to two eclipsing binaries, totalling four stars. Both pairs are double-lined spectroscopic binary systems that form Algol-like eclipsing binaries. [5] The orbits of both systems are somewhat eccentric. [5] The brightness of the system decreases from 6.44 down to 6.53 during the primary eclipse. [7] It has a stellar classification of A0V, [4] which matches an A-type main-sequence star that is generating energy through hydrogen fusion at its core. In reality, however, all four stars are nearly equal in properties, and have masses from 3.1 to 3.4 solar masses. [5] The system is about 200 million years old. [5]

Related Research Articles

Beta Canis Minoris Star in the constellation Canis Minor

Beta Canis Minoris, also named Gomeisa, is a star in the constellation of Canis Minor. In the night sky it is notable for its proximity to the prominent star Procyon.

WW Aurigae Binary star in the constellation Auriga

WW Aurigae is an eclipsing binary star system in the northern constellation of Auriga. It has a combined maximum apparent visual magnitude of 5.86, which is bright enough to be dimly visible to the naked eye. Based upon an annual parallax shift of 11.0 mas, it is located 297 light years from the Earth. The system is moving further away with a heliocentric radial velocity of −9 km/s, having come to within 212.5 ly some 3.12 million years ago.

70 Cancri is a star in the zodiac constellation of Cancer, located around 580 light years from the Sun. It is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of 6.7. The star is moving closer to the Earth with a heliocentric radial velocity of -21 km/s, and is expected to come to within 44 light-years in around nine million years. It is an A-type main-sequence star with a stellar classification of A1V. The object has a radius of about 2.7 R☉ and is radiating 76 times the Sun's luminosity from its photosphere at an effective temperature of 8,887 K.

Delta<sup>1</sup> Canis Minoris Star in the constellation Canis Minor

Delta1 Canis Minoris, Latinized from δ1 Canis Minoris, is a solitary, yellow-white hued star in the constellation Canis Minor. It is faintly visible to the naked eye with an apparent visual magnitude of +5.25. Based upon an annual parallax shift of 4.29 mas as seen from Earth, this star is located roughly 760 light years from the Sun.

Delta<sup>2</sup> Canis Minoris Star in the constellation Canis Minor

Delta2 Canis Minoris is a main-sequence star in the constellation Canis Minor, about 141 ly away.

Eta Canis Minoris Star in the constellation Canis Minor

Eta Canis Minoris is a binary star system in the equatorial constellation of Canis Minor. It is approximately 318 light-years from Earth.

1 Canis Minoris is a single star in the equatorial constellation of Canis Minor, located about 287 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.37. The radial velocity of this object is poorly constrained at −1.0±4.2 km/s.

11 Canis Minoris is a single star in the equatorial constellation of Canis Minor, located around 313 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.25. This object is moving away from the Earth with a heliocentric radial velocity of +28 km/s, having come to within 157 light-years some 2.35 million years ago.

42 Cassiopeiae is a possible binary star system in the northern circumpolar constellation of Cassiopeia. It is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of +5.18. The system is located approximately 291 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +7 km/s.

ET Andromedae Star in the constellation Andromeda

ET Andromedae is a binary star system star in the northern constellation of Andromeda. It has an apparent visual magnitude of 6.48, placing it at the nominal limit for visibility with the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.42 mas, which yields a value of 602 light years.

IU Aurigae Triple star system in the constellation Auriga

IU Aurigae is a triple star system in the constellation Auriga, consisting of an eclipsing binary pair orbiting a third component with a period of 335 years. This system is too faint to be viewed with the naked eye, having a peak apparent visual magnitude of 8.19. The eclipsing pair form a Beta Lyrae-type semidetached binary of two Bp stars with a period of 1.81147435 days. During the primary eclipse, the visual magnitude of the system drops to 8.89, while for the secondary it decreases to 8.74. The third component is a massive object with 17–18 M☉, and may actually be a binary – which would make this a quadruple star system.

3 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 360 light years away from the Sun. 3 Vulpeculae is its Flamsteed designation. It has been nicknamed "the Observer's Nightmare" by some astronomers because it is difficult to study as its orbital period is close to a year and it is pulsating with a period close to a day. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.18.

NR Canis Majoris Binary star system in the constellation Canis Major

NR Canis Majoris is a binary star system in the southern constellation of Canis Major, located to the east of Sirius and Gamma Canis Majoris near the constellation border with Puppis. It has a yellow-white hue and is dimly visible to the naked eye with a combined apparent visual magnitude that fluctuates around 5.60. It is located at a distance of approximately 297 light years from the Sun based on parallax. The system is drifting closer to the Sun with a radial velocity of −29 km/s, and in about three million years it is predicted to approach within 14.1+4.7
−4.0 ly. At that time, the star will become the brightest in the night sky, potentially reaching magnitude −0.88.

BC Canis Minoris Star in the constellation Canis Minor

BC Canis Minoris is a variable star in the equatorial constellation of Canis Minor. It has a reddish hue and is just barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.30. The distance to this object is approximately 520 light years based on parallax, but it is drifting closer with a radial velocity of −67 km/s.

AZ Canis Minoris Star in the constellation Canis Minor

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. 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. No evidence has been found for a companion to this star, although in the past it has been reported as a binary star system.

14 Lacertae is a binary star system in the northern constellation Lacerta, located around 1,600 light years away. It has the variable star designation V360 Lacertae; 14 Lacertae is the Flamsteed designation. The system is barely visible to the naked eye in good seeing conditions, having a peak apparent visual magnitude of 5.91. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.

4 Cygni is a binary star system in the northern constellation of Cygnus. It is a faintly visible to the naked eye with an apparent visual magnitude of 5.17. The distance to 4 Cygni, as determined from its annual parallax shift of 5.8 mas, is about 560 light years.

AE Pictoris is an eclipsing binary star system in the southern constellation of Pictor. This dim, blue-white hued point of light is just barely visible to the naked eye; it has an apparent visual magnitude of 6.09, which drops to magnitude 6.14 during an eclipse. The system is located around 1,430 light years away from the Sun based on parallax, and it is receding with a radial velocity of 34 km/s.

TU Corvi is a yellow-white hued star in the southern constellation of Corvus. It is a dimly visible to the naked eye with an apparent visual magnitude of 6.20. The distance to this star can be estimated from its annual parallax shift of 13.59 mas, yielding a range of about 240 light years. Based upon measured changes in its proper motion, it may be a close binary system.

VW Leo Minoris is a tight quadruple star system, located in the constellation of Leo Minor. With a peak combined apparent visual magnitude of 8.07, it is too faint to be seen with the naked eye. Parallax measurements give a distance estimate of approximately 360 light years from the Sun, and it is drifting further away with a radial velocity of +5 km/s.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 5 6 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. 1 2 3 4 5 6 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. 1 2 Cowley, A.; Cowley, C.; Jaschek, M.; Jaschek, C. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819
  5. 1 2 3 4 5 Volkov, I. M.; Kravtsova, A. S.; Chochol, D. (2021). "BU CMi as a Quadruple Doubly Eclipsing System". Astronomy Reports. 65 (9): 826–838. arXiv: 2107.09116 . Bibcode:2021ARep...65..826V. doi:10.1134/S1063772921090080. S2CID   236133942.
  6. ↑ "BU CMi". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-12-11.
  7. ↑ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
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