24 Canum Venaticorum

Nowadays, 24 Canum Venaticorum has become a topic of great interest and relevance in today's society. With the constant advancement of technology and globalization, 24 Canum Venaticorum has acquired a fundamental role in our daily lives. From its impact on the economy and politics, to its influence on culture and entertainment, 24 Canum Venaticorum has managed to capture the attention of people of all ages and backgrounds. In this article we will explore in depth the various aspects related to 24 Canum Venaticorum, analyzing its importance, its implications and its evolution over time. What is the true impact of 24 Canum Venaticorum on our society? How has our way of seeing and living 24 Canum Venaticorum changed over the years? These are some of the questions that we will try to answer throughout this exhaustive analysis.

24 Canum Venaticorum
Observation data
Epoch J2000      Equinox J2000
Constellation Canes Venatici
Right ascension 13h 34m 27.25928s[1]
Declination +49° 00′ 57.5065″[1]
Apparent magnitude (V) +4.68[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A5V
B−V color index 0.132±0.005[2]
Astrometry
Radial velocity (Rv)−18.3±2.8[4] km/s
Proper motion (μ) RA: −128.38[1] mas/yr
Dec.: +28.05[1] mas/yr
Parallax (π)18.09±0.19 mas[1]
Distance180 ± 2 ly
(55.3 ± 0.6 pc)
Absolute magnitude (MV)0.85[5]
Details
Mass1.74[6] M☉
Radius1.90[7] R☉
Luminosity40.8+1.1
−1.0[3] L☉
Surface gravity (log g)3.97[6] cgs
Temperature8,285±282[6] K
Rotational velocity (v sin i)159[3] km/s
Age310[6] Myr
Other designations
24 CVn, BD+49°2227, FK5 3083, GC 18356, HD 118232, HIP 66234, HR 5112, SAO 44668[8]
Database references
SIMBADdata

24 Canum Venaticorum is a single[9] star in the northern constellation of Canes Venatici, located 277 light years away from the Sun.[1] This object is visible to the naked eye as a faint white-hued star with an apparent visual magnitude of +4.68.[2] It is moving closer to the Earth with a heliocentric radial velocity of −18 km/s.[4]

This is an A-type main-sequence star with a stellar classification of A4 V,[10] and it is a shell star with rotationally-broadened lines.[11] It is 310[6] million years old with a projected rotational velocity of 159 km/s.[3] This rate of spin is giving the star an oblate shape with an equatorial bulge that is 7% larger than the polar radius.[12] The star has 1.74[6] times the mass of the Sun and 1.9[7] times the Sun's radius. It is radiating 41[3] times the Sun's luminosity from its photosphere at an effective temperature of 8,285 K.[6]

24 Canum Venaticorum displays a significant infrared excess at wavelengths of 24μm and 70μm, indicating an orbiting circumstellar debris disk.[11] The signature matches a black body temperature of 464 K for an estimated orbital radius of 1.4 AU.[7]

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 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 d e Zorec, J.; et al. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  5. ^ Pizzolato, N.; et al. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P
  6. ^ a b c d e f g 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.
  7. ^ a b c Patel, Rahul I.; et al. (May 2014), "A Sensitive Identification of Warm Debris Disks in the Solar Neighborhood through Precise Calibration of Saturated WISE Photometry", The Astrophysical Journal Supplement Series, 212 (1): 23, arXiv:1403.3435, Bibcode:2014ApJS..212...10P, doi:10.1088/0067-0049/212/1/10, S2CID 119219094, 10.
  8. ^ "24 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-27.
  9. ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  10. ^ Mora, A.; et al. (2001), "EXPORT: Spectral classification and projected rotational velocities of Vega-type and pre-main sequence stars", Astronomy & Astrophysics, 378 (1): 116–131, Bibcode:2001A&A...378..116M, doi:10.1051/0004-6361:20011098.
  11. ^ a b Roberge, Aki; Weinberger, Alycia J. (March 2008), "Debris Disks around Nearby Stars with Circumstellar Gas", The Astrophysical Journal, 676 (1): 509–517, arXiv:0711.4561, Bibcode:2008ApJ...676..509R, doi:10.1086/527314, S2CID 18407657.
  12. ^ 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.