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  mas [2]
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]

BU Canis Majoris was discovered to be a variable star when the Hipparcos data was analyzed. It was given its variable star designation in 1999. [7]

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. [8] 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

<span class="mw-page-title-main">Beta Canis Minoris</span> 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.

<span class="mw-page-title-main">Lambda Ursae Minoris</span> AGB star in the constellation Ursa Minor

Lambda Ursae Minoris is a star in the constellation Ursa Minor. It is an M-type red giant with an apparent magnitude of +6.38, making it very faintly visible to the naked eye under the best observing conditions. It is approximately 880 light years from Earth.

<span class="mw-page-title-main">WW Aurigae</span> 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 11.1 mas, it is located 293 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.

<span class="mw-page-title-main">10 Canis Majoris</span> Star in the constellation Canis Major

10 Canis Majoris is a single variable star in the southern constellation of Canis Major, located roughly 1,980 light years away from the Sun. It has the variable star designation FT Canis Majoris; 10 Canis Majoris is the Flamsteed designation. This body is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.23. It is moving away from the Earth with a heliocentric radial velocity of +34 km/s.

<span class="mw-page-title-main">12 Canis Majoris</span> Variable star in the constellation Canis Major

12 Canis Majoris is a variable star located about 707 light years away from the Sun in the southern constellation of Canis Major. It has the variable star designation HK Canis Majoris; 12 Canis Majoris is the Flamsteed designation. This body is just barely visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of +6.07. It is moving away from the Earth with a heliocentric radial velocity of +16 km/s. This is the brightest star in the vicinity of the open cluster NGC 2287, although it is probably not a member based on its proper motion.

<span class="mw-page-title-main">26 Canis Majoris</span> Star in the constellation Canis Major

26 Canis Majoris is a variable star in the southern constellation of Canis Major, located around 1,010 light years away from the Sun. It has the variable star designation MM Canis Majoris; 26 Canis Majoris is the Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of 5.89. It is moving further from the Earth with a heliocentric radial velocity of +22 km/s.

<span class="mw-page-title-main">27 Canis Majoris</span> Binary star system in the constellation Canis Major

27 Canis Majoris is a binary star system in the northern constellation of Canis Major, located approximately 1,700 light years away from the Sun. It has the variable star designation EW Canis Majoris; 27 Canis Majoris is the Flamsteed designation. This system is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of +4.65. It is moving away from the Earth with a heliocentric radial velocity of 16 km/s.

<span class="mw-page-title-main">UW Canis Majoris</span> Beta Lyrae variable star in the constellation Canis Major

UW Canis Majoris is a star in the constellation Canis Major. It is classified as a Beta Lyrae eclipsing contact binary and given the variable star designation UW Canis Majoris. Its brightness varies from magnitude +4.84 to +5.33 with a period of 4.39 days. Bode had initially labelled it as Tau2 Canis Majoris, but this designation had been dropped by Gould and subsequent authors. It is visible to the naked eye of a person under good observing conditions.

<span class="mw-page-title-main">Eta Canis Minoris</span> Binary star system 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.

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.

<span class="mw-page-title-main">V448 Carinae</span> Star in the constellation Carina

V448 Carinae is a single star in the constellation Carina. It has the Bayer designation O Carinae, while V448 Carinae is the variable star designation. This object has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 5.60. It is located at a distance of approximately 680 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +26 km/s.

<span class="mw-page-title-main">DL Crucis</span> Star in the constellation Crux

DL Crucis is a variable star in the constellation Crux.

<span class="mw-page-title-main">NR Canis Majoris</span> 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.

<span class="mw-page-title-main">15 Camelopardalis</span> Star in the constellation Camelopardalis

15 Camelopardalis is a triple star system in the northern circumpolar constellation of Camelopardalis. It has the variable star designation DV Camelopardalis; 15 Camelopardalis is the Flamsteed designation. This is just visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of 6.13. It is a probable (99%) member of the Cas-Tau OB association.

<span class="mw-page-title-main">LS Canis Majoris</span> Binary star system in the constellation Canis Major

LS Canis Majoris is an eclipsing binary star located around 1,510 light years from Earth in the constellation Canis Major. Its apparent magnitude ranges from 5.63 to 5.79, so it is faintly visible to the naked eye. The orbital period of binary pair and the period of light variation is 70.048 days.

<span class="mw-page-title-main">Omicron Puppis</span> Variable Star in the constellation Puppis

Omicron Puppis (ο Puppis) is candidate binary star system in the southern constellation of Puppis. It is visible to the naked eye, having a combined apparent visual magnitude of +4.48. Based upon an annual parallax shift of 2.30 mas as seen from Earth, it is located roughly 1,400 light years from the Sun.

<span class="mw-page-title-main">BC Canis Minoris</span> 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.

<span class="mw-page-title-main">14 Lacertae</span> Binary star in the constellation Lacerta

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.

<span class="mw-page-title-main">65 Ursae Majoris</span> Star system in the constellation Ursa Major

65 Ursae Majoris, abbreviated as 65 UMa, is a star system in the constellation of Ursa Major. With a combined apparent magnitude of about 6.5, it is at the limit of human eyesight and is just barely visible to the naked eye in ideal conditions. It is about 760 light years away from Earth.

<span class="mw-page-title-main">BG Canis Minoris</span> Variable star in the constellation of Canis Minor

BG Canis Minoris is a binary star system in the equatorial constellation of Canis Minor, abbreviated BG CMi. With an apparent visual magnitude that fluctuates around 14.5, it is much too faint to be visible to the naked eye. Parallax measurements provide a distance estimate of approximately 2,910 light years from the Sun.

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. ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (January 1999). "The 74th Special Name-list of Variable Stars" (PDF). Information Bulletin on Variable Stars. 4659: 1–77. Bibcode:1999IBVS.4659....1K . Retrieved 3 January 2025.
  8. ↑ 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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