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  mas [2]
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

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<span class="mw-page-title-main">Upsilon Ursae Majoris</span> Binary star in the constellation Ursa Major

Upsilon Ursae Majoris, Latinized from υ Ursae Majoris, is a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of +3.79. Based upon an annual parallax shift of 13.24 mas, it is located roughly 246 light-years from the Sun.

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

Iota Canis Majoris, Latinized from ι Canis Majoris, is a solitary variable supergiant star in the southern constellation of Canis Major. It is visible to the naked eye with an apparent visual magnitude that varies between +4.36 and +4.40. The distance to this star is approximately 2,500 light years based on spectroscopic measurements. It is drifting further away with a radial velocity of +42 km/s.

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

Kappa Canis Majoris, Latinized from κ Canis Majoris, is a solitary, blue-white hued star in the constellation Canis Major. It is visible to the naked eye with an apparent visual magnitude of +3.87. Based upon an annual parallax shift of 7.70 mas as seen from Earth, this star is located about 660 light years from the Sun.

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.

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Sigma Canis Majoris, also named Unurgunite, is a variable star in the southern constellation of Canis Major. It is approximately 1,290 light-years from the Sun and has an average apparent visual magnitude of +3.41.

<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.

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.

Delta<sup>3</sup> Canis Minoris Star in the constellation Canis Minor

Delta3 Canis Minoris, Latinized from δ3 Canis Minoris, is a solitary, white-hued star in the equatorial constellation of Canis Minor. Based upon a parallax of 4.46 mas as seen from Gaia spacecraft in its repeated orbits around the Sun, just beyond the Earth. This star is about 730 light years from the Solar System. At that distance, the visual magnitude of these stars is diminished by an extinction of more than 0.15 due to interstellar dust. With an apparent visual magnitude of +5.81, it is just bright enough to be faintly visible to the naked eye.

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.

<span class="mw-page-title-main">21 Vulpeculae</span> Star in the constellation Vulpecula

21 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. Its distance can be estimated from the annual parallax shift of 10.4302±0.0696 mas, yielding a separation of 313 light years. The star is faintly visible to the naked eye at night, having an apparent visual magnitude of 5.19. It is moving further away with a heliocentric radial velocity of about +7 km/s, having come within 243 ly (74.53 pc) around 4.2 million years ago.

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

<span class="mw-page-title-main">64 Eridani</span> Single, yellow-white hued star in the constellation Eridanus

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<span class="mw-page-title-main">QW Puppis</span> F3V star in the constellation Puppis

QW Puppis is a class F3V star in the constellation Puppis. Its apparent magnitude is 4.49 and it is approximately 69.5 light years away based on parallax.

<span class="mw-page-title-main">42 Persei</span> Binary star system in the constellation Perseus

42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around 93 parsecs (302 ly) distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.

<span class="mw-page-title-main">TU Corvi</span> Star in the constellation Corvus

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<span class="mw-page-title-main">BW Vulpeculae</span> Star in the constellation Vulpecula

BW Vulpeculae or BW Vul, is a variable star in the northern constellation of Vulpecula. It is near the lower limit of visibility to the naked eye with a typical apparent visual magnitude of 6.54. Based on an annual parallax shift of 1.15 mas, the distance to BW Vul is about 2,800 light years. It is moving closer to the Earth with a baseline heliocentric radial velocity of around −6 km/s.

<span class="mw-page-title-main">BF Antliae</span> Star in the constellation Antlia

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, 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, is 473 light years. It is moving further away with a heliocentric radial velocity of +18 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 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. Vol. 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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