NR Canis Majoris

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NR Canis Majoris
NRCMaLightCurve.png
A light curve for NR Canis Majoris, plotted from TESS data [1]
Observation data
Epoch J2000        Equinox J2000
Constellation Canis Major
Right ascension 07h 27m 07.99012s [2]
Declination −17° 51′ 53.5058″ [2]
Apparent magnitude  (V)5.60 [3] (5.66 + 9.23) [4]
Characteristics
Spectral type F2V [5]
B−V color index +0.314±0.002 [3]
Variable type δ Sct [6]
Astrometry
Radial velocity (Rv)−29.2±2.9 [3]  km/s
Proper motion (μ)RA: −2.420 [2]   mas/yr
Dec.: +1.388 [2]   mas/yr
Parallax (π)10.9688 ± 0.0917 [2]   mas
Distance 297 ± 2  ly
(91.2 ± 0.8  pc)
Absolute magnitude  (MV)0.78 [3]
Details
A
Mass 1.62 [7] or 2.18±0.04 [8]   M☉
Radius 3.90+0.18
−0.24 [2]   R☉
Luminosity 37.4±0.4 [2]   L☉
Surface gravity (log g)3.65 [7]   cgs
Temperature 7,227+238
−160 [2]   K
Rotational velocity (v sin i)185 [9]  km/s
Age 1.494 [7]   Gyr
Other designations
NR CMa, BD−17°1980, HD  58954, HIP  36186, HR  2853, SAO  152894, ADS  6093, CCDM J07271-1752AB, WDS J07271-1752 [10]
Database references
SIMBAD data

NR Canis Majoris is a binary star [11] 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. [3] It is located at a distance of approximately 297  light years from the Sun based on parallax. [2] The system is drifting closer to the Sun with a radial velocity of −29 km/s, [3] and in about three million years it is predicted to approach within 14.1+4.7
−4.0 ly. [12] At that time, the star will become the brightest in the night sky, potentially reaching magnitude −0.88. [13]

The magnitude 5.66 [4] primary component is an F-type main-sequence star with a stellar classification of F2V. [5] It is a Delta Scuti variable [6] that varies by a few hundredths of a magnitude over roughly 16 hours. [14] The star is an estimated 1.5 billion years old. [7] It has a high rate of spin with a projected rotational velocity of 185 km/s, which is giving the star an equatorial bulge that is estimated to be 8% larger than the polar radius. [9]

The secondary companion is magnitude 9.23 and lies at an angular separation of 1.3″ along a position angle of 39°, as of 2005. [4]

Related Research Articles

Kappa<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Kappa1 Sagittarii (κ1 Sagittarii) is a solitary, white-hued star in the zodiac constellation of Sagittarius. It has an apparent visual magnitude of +5.58, which is bright enough to be faintly visible to the naked eye. According to the Bortle scale, it can be viewed from dark suburban skies. Based upon an annual parallax shift of 15.12 mas as seen from Earth, this star is located around 223 light years from the Sun. It is advancing in the general direction of the Sun with a radial velocity of −11.6 km/s.

Nu Tauri Single star in the constellation Taurus

ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.

18 Aurigae is a star located 233 light years away from the Sun in the northern constellation of Auriga. The brightness of this object is near the limit of visibility to the naked eye under good viewing conditions, appearing as a dim, white-hued star with an apparent visual magnitude of 6.49. The star is moving away from the Sun with a heliocentric radial velocity of 7 km/s.

Theta Canis Majoris Star in the constellation Canis Major

Theta Canis Majoris is a solitary, orange-hued star near the northern edge of the constellation Canis Major, forming the nose of the "dog". The star is visible to the naked eye with an apparent visual magnitude of 4.08. Based upon an annual parallax shift of 12.51 mas as seen from Earth, it is located about 260 light years from the Sun. The star is moving away from us with a radial velocity of +96.2 km/s.

Nu1 Canis Majoris (ν1 Canis Majoris) is a binary star in the constellation Canis Major. It is visible to the naked eye with a combined apparent visual magnitude of 5.7. Based on parallax shift of 12.366 mas as seen from our orbit, this system is approximately 264 light years from the Sun.

Nu<sup>2</sup> Canis Majoris Star in the constellation Canis Major

Nu2 Canis Majoris (ν2 Canis Majoris) is a single star in the southern constellation of Canis Major.

10 Canis Majoris Variable star in the constellation Canis Major

10 Canis Majoris is a single variable star in the southern constellation of Canis Major, located roughly 1,800 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.

11 Canis Majoris is a single star in the southern constellation of Canis Major, the eleventh entry in John Flamsteed's catalogue of stars in that constellation. It has a blue-white hue and is visible to the naked eye with an apparent visual magnitude of 5.28. The distance to this star is approximately 1,010 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of around +15 km/s. It has an absolute magnitude of −1.63.

17 Canis Majoris is a single star in the southern constellation of Canis Major, located 610 light years away from the Sun. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.80. The object is moving closer to the Earth with a heliocentric radial velocity of −13 km/s.

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.

19 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, located approximately 238 light years from Sun based on its parallax. It is dimly visible to the naked eye as a white-hued star with an apparent visual magnitude of 5.77. The pair orbit each other with a period of 219.2 years and an eccentricity of 0.686. The system is moving closer to the Earth with a heliocentric radial velocity of −21 km/s.

HD 220105 is a star in the northern constellation of Andromeda, and a member of the Sirius supercluster. It lies near the lower limit of visibility to the naked eye at an apparent visual magnitude of 6.24, and can be a challenge to spot under normal viewing conditions. The star is located 239 light years away, based upon an annual parallax shift of 13.63 mas. It is moving closer to the Earth with a heliocentric radial velocity of −2 km/s.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 96 parsecs (310 ly) distant.

Mu Canis Majoris Star in the constellation Canis Major

Mu Canis Majoris is a binary star system in the southern constellation of Canis Major. The pair can be located a little to the southwest of the point midway between Gamma and Theta Canis Majoris, and the components can be split with a small telescope. The system is faintly visible to the naked eye with an apparent visual magnitude of 5.12. Based upon an annual parallax shift of just 2.62 mas as seen from Earth, this system is located roughly 1,200 light years from the Sun.

Delta Horologii is a binary star system in the constellation Horologium. It is visible to the naked eye with a combined apparent visual magnitude of 4.93. As of 2014, the pair had an angular separation of 0.20 arc seconds along a position angle of 24°. Based upon an annual parallax shift of 18.24 mas as seen from Earth, it is located 179 ± 4 light years from the Sun.

Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.

HD 79940 is a single star in the southern constellation of Vela. It has the Bayer designation of k Velorum; HD 79940 is the identifier from the Henry Draper Catalogue. This star has a yellow-white hue and is faintly visible to the naked eye as a point light source with an apparent visual magnitude of 4.63. It is located at a distance of approximately 158 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +6 km/s.

57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.90 mas provides a distance estimate of about 193 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).

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 7 8 9 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 3 Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 . Retrieved 2015-07-22.
  5. 1 2 Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. 4. Ann Arbor: Department of Astronomy, University of Michigan. Bibcode:1988mcts.book.....H.
  6. 1 2 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.
  7. 1 2 3 4 David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID   33401607.
  8. ↑ 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.
  9. 1 2 van Belle, Gerard T. (March 2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review. 20 (1): 51. arXiv: 1204.2572 . Bibcode:2012A&ARv..20...51V. doi:10.1007/s00159-012-0051-2. S2CID   119273474.
  10. ↑ "NR CMa". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 12 February 2017.
  11. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  12. ↑ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv: 1412.3648 . Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID   59039482. A35.
  13. ↑ Tomkin, Jocelyn (April 1998). "Once and Future Celestial Kings". Sky and Telescope. 95 (4): 59–63. Bibcode:1998S&T....95d..59T.
  14. ↑ Watson, Christopher (4 January 2010). "LS Canis Majoris". AAVSO Website. American Association of Variable Star Observers . Retrieved 12 July 2014.
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