Winnecke 4

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Winnecke 4
Winnecke 4.jpg
Winnecke 4 double star
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
A
Right ascension 12h 22m 12.5278s[1]
Declination +58° 4′ 58.539″[1]
Apparent magnitude (V)
B
Right ascension 12h 22m 18.9989s[1]
Declination +58° 5′ 10.364″[1]
Apparent magnitude (V)
Characteristics
A
Spectral type K0 III[2]
B
Spectral type G0 V[2]
Astrometry
A
Parallax (π)2.87 ± 0.24[1] mas
Distance1,140 ± 100 ly
(350 ± 30 pc)
Absolute magnitude (MV)+0.88[2]
B
Parallax (π)7.13 ± 0.24[1] mas
Distance460 ± 20 ly
(140 ± 5 pc)
Absolute magnitude (MV)+4.0[2]
Details
A
Mass1.1[2] M
B
Mass1.2[2] M
Other designations
M40, WNC 4, BD+56 1372, CCDM 12223+5805, WDS J12222+5805
A: HD 238107, SAO 28353
B: HD 238108, SAO 28355
Database references
SIMBADdata

Winnecke 4 (also known as Messier 40 or WNC 4) is a double star in the constellation Ursa Major.

WNC 4 was 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 double star instead. It was subsequently 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.[3] The nearby nebula observed by Hevelius may have been the nearby spiral galaxy NGC 4290. The galaxy, being 12th magnitude, may have been bright enough to notice for large telescopes at the time, but not quite bright enough for Messier.[citation needed]

In 1991 the separation between the components was measured at 51.7", an increase since Messier's time. Data gathered by astronomers Brian Skiff (2001) and Richard L. Nugent (2002) strongly suggested that this was merely an optical double star rather than a physically connected system.[2] In 2016, by using parallax measurements from the Gaia satellite, it was definitively proven that the two stars comprising the double star (HD 238107 and HD 238108) are entirely unrelated,[4] confirming the previous suggestion by Skiff and Nugent. Distances are 350±30 pc and 140±5 pc for the two objects. The further is just over twice as far as the nearer.[4]

References[edit]

  1. ^ a b c d e f Gaia Collaboration; Brown, A. G. A; Vallenari, A; Prusti, T; De Bruijne, J. H. J; Mignard, F; Drimmel, R; Babusiaux, C; Bailer-Jones, C. A. L; Bastian, U; Biermann, M; Evans, D. W; Eyer, L; Jansen, F; Jordi, C; Katz, D; Klioner, S. A; Lammers, U; Lindegren, L; Luri, X; O'Mullane, W; Panem, C; Pourbaix, D; Randich, S; Sartoretti, P; Siddiqui, H. I; Soubiran, C; Valette, V; Van Leeuwen, F; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics. 595: A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512.
  2. ^ a b c d e f g Nugent, Richard L (2002). "The Nature of the Double Star M40". Journal of the Royal Astronomical Society of Canada. 96: 63. Bibcode:2002JRASC..96...63N.
  3. ^ Robert Burnham (1978). Burnham's Celestial Handbook: An Observer's Guide to the Universe Beyond the Solar System. Courier Corporation. p. 1982. ISBN 978-0-486-23673-5.
  4. ^ a b Merrifield, M. R; Gray, M. E; Haran, B (2017). "Gaia Shows that Messier 40 is Definitely Not a Binary Star". The Observatory. 137: 23. arXiv:1612.00834. Bibcode:2017Obs...137...23M.

External links[edit]

Coordinates: Sky map 12h 22m 12.5s, 58° 04′ 59″