Winnecke 4

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Winnecke 4
M40 (Winnecke 4) (noao-m40).jpg
Winnecke 4 double star
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Ursa Major
A
Right ascension 12h 22m 12.5272s [1]
Declination +58° 4′ 58.549″ [1]
Apparent magnitude  (V)9.64 [2]
B
Right ascension 12h 22m 18.9992s [3]
Declination +58° 5′ 10.366″ [3]
Apparent magnitude  (V)10.11 [2]
Characteristics
A
Spectral type K0 III [4]
B
Spectral type G0 V [4]
Astrometry
A
Parallax (π)3.2191 ± 0.0118  mas [1]
Distance 1,013 ± 4  ly
(311 ± 1  pc)
Absolute magnitude  (MV)+0.88 [4]
B
Parallax (π)6.9328 ± 0.0155  mas [3]
Distance 470 ± 1  ly
(144.2 ± 0.3  pc)
Absolute magnitude  (MV)+4.0 [4]
Details
A
Mass 1.15 [5]   M☉
Radius 4.48 [6]   R☉
Luminosity 13 [6]   L☉
Surface gravity (log g)3.16 [5]   cgs
Temperature 4,957 [5]   K
Metallicity [Fe/H]−0.164 [7]   dex
Age 4.1 [7]   Gyr
B
Mass 1.00 [5]   M☉
Radius 1.1 [8]   R☉
Luminosity1.56 [8]   L☉
Surface gravity (log g)4.36 [5]   cgs
Temperature 6,146 [5]   K
Metallicity [Fe/H]−0.26 [5]   dex
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
SIMBAD data
A
B

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.

Contents

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. [9]

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. [4] The A star that seems the brighter is over twice as far as B. [10] Parallax measurements from the Gaia satellite show the two stars, HD 238107 and HD 238108, are at distances of 311 ± 1 parsec (1,013 ± 4 light-years ) and 144.2 ± 0.3 parsecs (470 ± 1 light-year ) respectively. HD 238108 is itself a genuine binary star, with an 18th magnitude white dwarf companion 5 arcseconds away and a parallax distance of 146.8 ± 2.3 parsecs (479 ± 8 light-years ).[ citation needed ]

See also

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References

  1. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361.
  3. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. 1 2 3 4 5 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.
  5. 1 2 3 4 5 6 7 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; de Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi: 10.1051/0004-6361/201935765 . ISSN   0004-6361.
  6. 1 2 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.
  7. 1 2 Sit, Tawny; Ness, M. K. (2020). "The Age Distribution of Stars in the Milky Way Bulge". The Astrophysical Journal. 900 (1): 4. arXiv: 2006.01158 . Bibcode:2020ApJ...900....4S. doi: 10.3847/1538-4357/ab9ff6 . S2CID   219179385.
  8. 1 2 Stassun, Keivan G.; et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv: 1905.10694 . Bibcode:2019AJ....158..138S. doi: 10.3847/1538-3881/ab3467 . hdl: 1721.1/124721 . ISSN   0004-6256. S2CID   166227927.
  9. ↑ 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.
  10. ↑ 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.
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