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]
| 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] |
| Distance | 425 ± 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 | |
| Mass | 1.0–2.0 M☉ |
| Radius | 3.7–4.1 R☉ |
| Luminosity | 295+3.6 −3.2 L☉ |
| Surface gravity (log g) | 3.30±0.35 cgs |
| Temperature | 6,875±120 K |
| Metallicity [Fe/H] | −0.05±0.15 dex |
| Rotational velocity (v sin i) | 109±3 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
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. 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,[11] 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
edit- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "4 CVn". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-25.
- ^ Jones, D. H. P.; Haslam, C. M. (February 1966), "A new delta Scuti variable", The Observatory, 86: 34, Bibcode:1966Obs....86...34J.