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{{Starbox begin
| name = 4 Canum Venaticorum
}}{{Starbox observe
| epoch = J2000
| constell = Canes Venatici
| ra = {{RA|20|01|47.01149}}[1]
| dec = {{DEC|+64|49|33.8670}}[1]
| appmag_v = +6.04[3] {{nowrap|5.89 to 6.15}}[4]
}}{{Starbox character
| type =
| class = F3 IV[5] or F0 III[6]
| b-v = {{Val|0.366|0.005}}[7]
| u-b =
| variable = δ Sct[8]
}}{{Starbox astrometry
| radial_v = {{Val|−0.3|2.9}}[3]
| prop_mo_ra = −79.651[1]
| prop_mo_dec = +13.203[1]
| parallax = 7.6829
| p_error = 0.0960
| parallax_footnote = [1]
| absmag_v = +0.75[13]
}}{{Starbox orbit
| reference = [3]
| period_unitless = {{Val|124.44|0.03|u=days}}
| eccentricity = {{Val|0.311|0.003}}
| periastron = {{Val|2454605|10.3|ul=JD}}
| periarg = {{Val|70.2|0.7}}
| k1 = {{Val|13.24|0.05}}
}}{{Starbox detail
| source = [3]
| component1 = 4 CVn A
| mass = {{Val|1.0|–|2.0}}
| radius = {{Val|3.7|–|4.1}}
| luminosity = {{Val|295|3.6|3.2}}
| gravity = {{Val|3.30|0.35}}
| temperature = {{Val|6875|120|fmt=commas}}
| metal_fe = {{Val|−0.05|0.15}}
| rotational_velocity = {{Val|109|3}}
| age_gyr =
}}{{Starbox catalog
| names = {{odlist | V=AI Canum Venaticorum | F=4 CVn | BD=+43°2218 | FK5=2993 | HD=107904 | HIP=60467 | HR=4715 | SAO=44155 | GC=16899 }}
}}{{Starbox reference
| Simbad = 4+CVn
}}{{Starbox end}}4 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, located around 425 light years away.[1] 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. 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,[23] 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] References1. ^1 2 3 4 5 6 {{cite DR2|1535113503063938944}}
2. ^1 2 {{citation | last1=Samus | first1=N. N. | last2=Kazarovets | first2=E. V. | last3=Durlevich | first3=O. V. | last4=Kireeva | first4=N. N. | last5=Pastukhova | first5=E. N. | display-authors=1 | title=General Catalogue of Variable Stars | version=5.1 | journal=Astronomy Reports | year=2017 | volume=61 | issue=1 | pages=80–88 | bibcode=2017ARep...61...80S | postscript=. }}
3. ^1 {{citation | title=XHIP: An extended hipparcos compilation | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | journal=Astronomy Letters | volume=38 | issue=5 | pages=331 | year=2012 | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | arxiv=1108.4971 | postscript=. }}
4. ^1 {{citation | title=A new delta Scuti variable | last1=Jones | first1=D. H. P. | last2=Haslam | first2=C. M. | journal=The Observatory | volume=86 | pages=34–34 | date=February 1966 | bibcode=1966Obs....86...34J | postscript=. }}
5. ^1 2 3 {{citation | title=Nonradial and radial period changes of the δ Scuti star 4 CVn. II. Systematic behavior over 40 years | last1=Breger | first1=M. | last2=Montgomery | first2=M. H. | last3=Lenz | first3=P. | last4=Pamyatnykh | first4=A. A. | display-authors=1 | journal=Astronomy & Astrophysics | volume=599 | id=A116 | pages=8 | date=March 2017 | doi=10.1051/0004-6361/201629797 | bibcode=2017A&A...599A.116B | arxiv=1612.06827 | postscript=. }}
6. ^1 2 3 4 5 6 {{citation | title=Discovery of binarity, spectroscopic frequency analysis, and mode identification of the δ Scuti star 4 CVn | last1=Schmid | first1=V. S. | last2=Themeßl | first2=N. | last3=Breger | first3=M. | last4=Degroote | first4=P. | last5=Aerts | first5=C. | last6=Beck | first6=P. G. | last7=Tkachenko | first7=A. | last8=Van Reeth | first8=T. | last9=Bloemen | first9=S. | last10=Debosscher | first10=J. | last11=Castanheira | first11=B. G. | last12=McArthur | first12=B. E. | last13=Pápics | first13=P. I. | last14=Fritz | first14=V. | last15=Falcon | first15=R. E. | display-authors=1 | journal=Astronomy & Astrophysics | volume=570 | id=A33 | pages=17 | date=October 2014 | doi=10.1051/0004-6361/201423669 | bibcode=2014A&A...570A..33S | arxiv=1407.4257 | postscript=. }}
7. ^1 {{citation | title=The Age Range of Hyades Stars | last1=Eggen | first1=Olin J. | postscript=. | journal=The Astronomical Journal | volume=116 | issue=1 | pages=284–292 | date=July 1998 | doi=10.1086/300413 | bibcode=1998AJ....116..284E }}
8. ^1 2 {{citation | last1=Morgan | first1=W. W. | last2=Abt | first2=H. A. | title=The spectral classification of the F stars of intermediate luminosity | journal=Astronomical Journal | volume=77 | pages=35–37 | date=February 1972 | doi=10.1086/111242 | bibcode=1972AJ.....77...35M }}
9. ^1 2 {{citation | last1=Appenzeller | first1=Immo | postscript=. | title=MK Spectral Types for 185 Bright Stars | journal=Publications of the Astronomical Society of the Pacific | volume=79 | issue=467 | page=102 | date=April 1967 | doi=10.1086/128449 | bibcode=1967PASP...79..102A }}
}}{{Stars of Canes Venatici}} 11 : F-type subgiants|F-type giants|Delta Scuti variables|Spectroscopic binaries|Canes Venatici|Durchmusterung objects|Flamsteed objects|Henry Draper Catalogue objects|Hipparcos objects|HR objects|Objects with variable star designations |