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25 Canum Venaticorum
Observation data
Epoch J2000       Equinox J2000
Constellation Canes Venatici
Right ascension 13h 37m 27.62782s [1]
Declination +36° 17′ 41.6337″ [1]
Apparent magnitude (V) +4.82 [2] (4.98 + 6.95) [3]
Characteristics
Spectral type A7 III + A8 V: [4]
Astrometry
Radial velocity (Rv)−10.4±2.1 [2] km/s
Proper motion (μ) RA: −95.54 [1]  mas/ yr
Dec.: +23.75 [1]  mas/ yr
Parallax (π)16.42 ± 0.53  mas [1]
Distance199 ± 6  ly
(61 ± 2  pc)
Absolute magnitude (MV)0.90 [2]
Orbit [5]
Period (P)228 yr
Semi-major axis (a)1.02″
Eccentricity (e)0.80
Inclination (i)147°
Longitude of the node (Ω)87°
Periastron epoch (T)1864.0
Argument of periastron (ω)
(secondary)		159°
Details
25 CVn A
Mass2.23 [6]  M☉
Surface gravity (log g)3.85 [7]  cgs
Temperature7,609±259 [7]  K
Rotational velocity (v sin i)235 [8] km/s
Age659 [7]  Myr
25 CVn B
Mass1.58 [6]  M☉
Other designations
25 CVn, BD+37° 2433, FK5 3083, GC 18421, HD 118623, HIP 66458, HR 5127, SAO 63648, ADS 8974, CCDM 13375+3617, WDS J13375+3618 [9]
Database references
SIMBAD data

25 Canum Venaticorum is a binary star [10] system in the northern constellation of Canes Venatici, approximately 199 [1] light years from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of +4.82 [2] The system is moving closer to the Earth with a heliocentric radial velocity of roughly −10 km/s. [2]

This is a wide binary system with an orbital period of 228 years and an eccentricity of 0.80. [5] As of 2001, they had a projected separation of 107.0  AU. [6] The magnitude 4.98 [3] primary, component A, has a stellar classification of A7 III, [4] which matches an A-type giant star. It is 659 [7] million years old with a projected rotational velocity of 235 km/s. This rate of spin is giving the star an oblate shape with an equatorial bulge that is an estimated 27% larger than the polar radius. [8] The companion, component B, is a magnitude 6.95 [3] A-type main-sequence star with a class of A8 V:. [4] The ':' suffix indicates some uncertainty in the classification of this star.

References

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID  18759600.
  2. ^ a b c d e 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.
  3. ^ a b c Mason, B. D.; et al. (December 2001), "The Washington Visual Double Star Catalog (WDS), Version 2019-01-21", The Astronomical Journal, 122 (6), U. S. Naval Observatory, Washington D.C.: 3466–3471, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920.
  4. ^ a b c Stephenson, C. B.; Sanwal, N. B. (June 1969), "The masses of stars above the main sequence", Astronomical Journal, 74: 689–704, Bibcode: 1969AJ.....74..689S, doi: 10.1086/110845.
  5. ^ a b Söderhjelm, Staffan (1999), "Visual binary orbits and masses POST HIPPARCOS", Astronomy and Astrophysics, 341: 121–140, Bibcode: 1999A&A...341..121S.
  6. ^ a b c De Rosa, R. J.; Patience, J.; Wilson, P. A.; Schneider, A.; Wiktorowicz, S. J.; Vigan, A.; Marois, C.; Song, I.; Macintosh, B.; Graham, J. R.; Doyon, R.; Bessell, M. S.; Thomas, S.; Lai, O. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society, 437 (2): 1216–1240, arXiv: 1311.7141, Bibcode: 2014MNRAS.437.1216D, doi: 10.1093/mnras/stt1932.
  7. ^ a b c d 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. ^ a b 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.
  9. ^ "25 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID  14878976.
Retrieved from " https://en.wikipedia.org/?title=25_Canum_Venaticorum&oldid=1169993490"
From Wikipedia, the free encyclopedia
25 Canum Venaticorum
Observation data
Epoch J2000       Equinox J2000
Constellation Canes Venatici
Right ascension 13h 37m 27.62782s [1]
Declination +36° 17′ 41.6337″ [1]
Apparent magnitude (V) +4.82 [2] (4.98 + 6.95) [3]
Characteristics
Spectral type A7 III + A8 V: [4]
Astrometry
Radial velocity (Rv)−10.4±2.1 [2] km/s
Proper motion (μ) RA: −95.54 [1]  mas/ yr
Dec.: +23.75 [1]  mas/ yr
Parallax (π)16.42 ± 0.53  mas [1]
Distance199 ± 6  ly
(61 ± 2  pc)
Absolute magnitude (MV)0.90 [2]
Orbit [5]
Period (P)228 yr
Semi-major axis (a)1.02″
Eccentricity (e)0.80
Inclination (i)147°
Longitude of the node (Ω)87°
Periastron epoch (T)1864.0
Argument of periastron (ω)
(secondary)		159°
Details
25 CVn A
Mass2.23 [6]  M☉
Surface gravity (log g)3.85 [7]  cgs
Temperature7,609±259 [7]  K
Rotational velocity (v sin i)235 [8] km/s
Age659 [7]  Myr
25 CVn B
Mass1.58 [6]  M☉
Other designations
25 CVn, BD+37° 2433, FK5 3083, GC 18421, HD 118623, HIP 66458, HR 5127, SAO 63648, ADS 8974, CCDM 13375+3617, WDS J13375+3618 [9]
Database references
SIMBAD data

25 Canum Venaticorum is a binary star [10] system in the northern constellation of Canes Venatici, approximately 199 [1] light years from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of +4.82 [2] The system is moving closer to the Earth with a heliocentric radial velocity of roughly −10 km/s. [2]

This is a wide binary system with an orbital period of 228 years and an eccentricity of 0.80. [5] As of 2001, they had a projected separation of 107.0  AU. [6] The magnitude 4.98 [3] primary, component A, has a stellar classification of A7 III, [4] which matches an A-type giant star. It is 659 [7] million years old with a projected rotational velocity of 235 km/s. This rate of spin is giving the star an oblate shape with an equatorial bulge that is an estimated 27% larger than the polar radius. [8] The companion, component B, is a magnitude 6.95 [3] A-type main-sequence star with a class of A8 V:. [4] The ':' suffix indicates some uncertainty in the classification of this star.

References

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID  18759600.
  2. ^ a b c d e 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.
  3. ^ a b c Mason, B. D.; et al. (December 2001), "The Washington Visual Double Star Catalog (WDS), Version 2019-01-21", The Astronomical Journal, 122 (6), U. S. Naval Observatory, Washington D.C.: 3466–3471, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920.
  4. ^ a b c Stephenson, C. B.; Sanwal, N. B. (June 1969), "The masses of stars above the main sequence", Astronomical Journal, 74: 689–704, Bibcode: 1969AJ.....74..689S, doi: 10.1086/110845.
  5. ^ a b Söderhjelm, Staffan (1999), "Visual binary orbits and masses POST HIPPARCOS", Astronomy and Astrophysics, 341: 121–140, Bibcode: 1999A&A...341..121S.
  6. ^ a b c De Rosa, R. J.; Patience, J.; Wilson, P. A.; Schneider, A.; Wiktorowicz, S. J.; Vigan, A.; Marois, C.; Song, I.; Macintosh, B.; Graham, J. R.; Doyon, R.; Bessell, M. S.; Thomas, S.; Lai, O. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society, 437 (2): 1216–1240, arXiv: 1311.7141, Bibcode: 2014MNRAS.437.1216D, doi: 10.1093/mnras/stt1932.
  7. ^ a b c d 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. ^ a b 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.
  9. ^ "25 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID  14878976.
Retrieved from " https://en.wikipedia.org/?title=25_Canum_Venaticorum&oldid=1169993490"

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