4 Canum Venaticorum

Nowadays, 4 Canum Venaticorum has become a highly relevant topic in modern society. Its impact covers multiple areas, from politics to technology, including culture and the economy. More and more people are influenced by 4 Canum Venaticorum and its influence continues to expand at a dizzying rate. In this article, we will explore the various facets of 4 Canum Venaticorum and its impact on our daily lives. From its origins to its current evolution, including its possible repercussions in the future, we will comprehensively address the importance of understanding and analyzing 4 Canum Venaticorum in the current context.

4 Canum Venaticorum

A light curve for AI Canes Venaticorum, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Canes Venatici
Right ascension 12h 23m 47.01149s[2]
Declination +42° 32′ 33.8670″[2]
Apparent magnitude (V) +6.04[3] 5.89 to 6.15[4]
Characteristics
Spectral type F3 IV[5] or F0 III[6]
B−V color index 0.366±0.005[7]
Variable type δ Sct[8]
Astrometry
Radial velocity (Rv)−0.3±2.9[3] km/s
Proper motion (μ) RA: −79.651[2] mas/yr
Dec.: +13.203[2] mas/yr
Parallax (π)7.6829±0.0960 mas[2]
Distance425 ± 5 ly
(130 ± 2 pc)
Absolute magnitude (MV)+0.75[9]
Orbit[3]
Period (P)124.44±0.03 d
Eccentricity (e)0.311±0.003
Periastron epoch (T)2454605±10.3 JD
Argument of periastron (ω)
(secondary)		70.2±0.7°
Semi-amplitude (K1)
(primary)		13.24±0.05 km/s
Details[3]
4 CVn A
Mass1.0–2.0 M☉
Radius3.7–4.1 R☉
Luminosity295+3.6
−3.2 L☉
Surface gravity (log g)3.30±0.35 cgs
Temperature6,875±120 K
Metallicity −0.05±0.15 dex
Rotational velocity (v sin i)109±3 km/s
Other designations
4 CVn, AI Canum Venaticorum, BD+43°2218, FK5 2993, GC 16899, HD 107904, HIP 60467, HR 4715, SAO 44155[10]
Database references
SIMBADdata

4 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, located around 425 light years away.[2] It has the variable star designation AI Canum Venaticorum; 4 Canum Venaticorum is its Flamsteed designation. Its brightness varies from magnitude +5.89 to +6.15 with a period of 2.8 hours,[4] which places it around the lower limit of visibility to the naked eye. This was found to be a binary by Schmid et al. in 2014, based on periodic, non-sinusoidal changes in its radial velocity. It is a single-lined spectroscopic binary with an orbital period of 124.4 days and an eccentricity of 0.31.[3]

The primary component is an evolved F-type star with a stellar classification of F3 IV[5] or F0 III,[6] matching a subgiant or giant star, respectively. Roberta M. Humphreys first showed that the star's brightness varies, in 1966.[11] It is a variable of the Delta Scuti class, displaying both radial and non-radial pulsations.[8] The variable nature of this star was discovered by D. H. P. Jones and C. Margaret Haslam in 1966 at the suggestion of Olin J. Eggen,[12] and it has become one of the best studied stars in its class. The radial pulsations have shown little if any variations between 1974 and 2012. However, the non-radial pulsations vary continuously in frequency over periods spanning decades.[8] It is spinning rapidly with a rotation of at least one third of its critical velocity.[3]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e f 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. ^ a b c d e f Schmid, V. S.; et al. (October 2014), "Discovery of binarity, spectroscopic frequency analysis, and mode identification of the δ Scuti star 4 CVn", Astronomy & Astrophysics, 570: 17, arXiv:1407.4257, Bibcode:2014A&A...570A..33S, doi:10.1051/0004-6361/201423669, S2CID 36767234, A33.
  4. ^ a b 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.
  5. ^ a b Morgan, W. W.; Abt, H. A. (February 1972), "The spectral classification of the F stars of intermediate luminosity", Astronomical Journal, 77: 35–37, Bibcode:1972AJ.....77...35M, doi:10.1086/111242
  6. ^ a b Appenzeller, Immo (April 1967), "MK Spectral Types for 185 Bright Stars", Publications of the Astronomical Society of the Pacific, 79 (467): 102, Bibcode:1967PASP...79..102A, doi:10.1086/128449.
  7. ^ 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.
  8. ^ a b c Breger, M.; et al. (March 2017), "Nonradial and radial period changes of the δ Scuti star 4 CVn. II. Systematic behavior over 40 years", Astronomy & Astrophysics, 599: 8, arXiv:1612.06827, Bibcode:2017A&A...599A.116B, doi:10.1051/0004-6361/201629797, S2CID 55127114, A116.
  9. ^ Eggen, Olin J. (July 1998), "The Age Range of Hyades Stars", The Astronomical Journal, 116 (1): 284–292, Bibcode:1998AJ....116..284E, doi:10.1086/300413.
  10. ^ "4 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-25.
  11. ^ Humphreys, Roberta M. (February 1967). "Photoelectric Observations of 4 Canum Venaticorum". Publications of the Astronomical Society of the Pacific. 79 (466): 78–80. Bibcode:1967PASP...79...78H. doi:10.1086/128444. Retrieved 6 January 2025.
  12. ^ Jones, D. H. P.; Haslam, C. M. (February 1966), "A new delta Scuti variable", The Observatory, 86: 34, Bibcode:1966Obs....86...34J.