Winnecke 4

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Template:Short description

Winnecke 4
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major[1]
A
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 9.64[3]
B
Right ascension Template:RA[4]
Declination Template:DEC[4]
Apparent magnitude (V) 10.11[3]
Characteristics
A
Spectral type K0 III[5]
B
Spectral type G0 V[5]
Astrometry
A
Parallax (π)3.2191±0.0118 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)+0.88[5]
B
Parallax (π)6.9328±0.0155 mas[4]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)+4.0[5]
Details
A
Mass1.15[6] Template:Solar mass
Radius4.48[7] Template:Solar radius
Luminosity13[7] Template:Solar luminosity
Surface gravity (log g)3.16[6] cgs
Temperature4,957[6] K
Metallicity [Fe/H]−0.164[8] dex
Age4.1[8] Gyr
B
Mass1.00[6] Template:Solar mass
Radius1.1[9] Template:Solar radius
Luminosity1.56[9] Template:Solar luminosity
Surface gravity (log g)4.36[6] cgs
Temperature6,146[6] K
Metallicity [Fe/H]−0.26[6] dex
Other designations
M40, WNC 4, Template:Odlist
A: Template:Odlist
B: Template:Odlist
Database references
SIMBADdata
A
B

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Winnecke 4 (also known as Messier 40 or WNC 4) is an optical double star consisting of two unrelated stars in a northerly zone of the sky, Ursa Major.

The pair were discovered by Charles Messier in 1764 while he was searching for a nebula that had been reported in the area by Johannes Hevelius. Not seeing any nebulae, Messier catalogued this apparent pair instead. The pair were rediscovered by Friedrich August Theodor Winnecke in 1863, and included in the Winnecke Catalogue of Double Stars as number 4. Burnham calls M40 "one of the few real mistakes in the Messier catalog," faulting Messier for including it when all he saw was a double star, not a nebula of any sort.[10]

In 1991 the separation between the components was measured at 51.7″, an increase since 1764. Data gathered by astronomers Brian Skiff (2001) and Richard L. Nugent (2002) strongly suggested the subject was merely an optical double star rather than a physically connected (binary) system.[5] The A star that seems the brighter is over twice as far as B.[11] Parallax measurements from the Gaia satellite show the two stars, HD 238107 and HD 238108, are at distances of Script error: No such module "convert". and Script error: No such module "convert". respectively. HD 238108 is itself a genuine binary star, with an 18th magnitude white dwarf companion 5 arcseconds away and a parallax distance of Script error: No such module "convert"..Script error: No such module "Unsubst".

See also

References

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  1. ↑ Template:Cite constellation
  2. ↑ a b c Template:Cite Gaia EDR3
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  4. ↑ a b c Template:Cite Gaia EDR3
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  7. ↑ a b Template:Cite Gaia DR2
  8. ↑ a b Script error: No such module "Citation/CS1".
  9. ↑ a b Script error: No such module "Citation/CS1".
  10. ↑ Script error: No such module "citation/CS1".
  11. ↑ Script error: No such module "Citation/CS1".

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External links

Template:Portal bar Template:Messier objects Template:Stars of Ursa Major Template:Sky

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