Messier 67

Messier 67
Messier object 067.jpg
Messier 67 (2MASS near-infrared)
Observation data (J2000.0 epoch)
Constellation Cancer
Right ascension 08h 51.4m
Declination +11° 49′
Distance ~2.61-2.93 kly (800-900 pc[1][2][3][4])
Apparent magnitude (V) 6.1
Apparent dimensions (V) 30.0′
Physical characteristics
Radius 10 ly
Estimated age 3.2 to 5 billion years
Other designations NGC 2682
See also: Open cluster, List of open clusters

Messier 67 (also known as M67 or NGC 2682) is an open cluster in the constellation of Cancer. M67's Trumpler class is variously given as II 2 r, II 2 m, or II 3 r. It was discovered by Johann Gottfried Koehler in 1779. Age estimates for the cluster range between 3.2 and 5 billion years, with the most recent estimate (4 Gyr) implying stars in M67 are younger than the Sun. Distance estimates are likewise varied and typically range between 800-900 pc.[1][2][3][4] Recent estimates of 855, 840, and 815 pc were established via binary star modelling and infrared color-magnitude diagram fitting, accordingly.[2][3][4]

M67 is not the oldest known open cluster, but there are few Galactic clusters known to be older, and none of those are as close as M67. M67 is an important laboratory for studying stellar evolution, since the cluster is well populated, obscured by negligible amounts of sut, and all its stars are at the same distance and age, except for approximately 30 anomalous blue stragglers, whose origins are not fully understood.[5]

M67 is the nearest old open cluster, and thus has become a standard example for studying stellar evolution. It is probably the second best observed open cluster after the Hyades cluster, which is amongst the nearest open clusters and younger than M67.[6] M67 is one of the most-studied open clusters, yet estimates of its physical parameters such as age, mass, and number of stars of a given type, vary substantially. Richer et al.[7] estimate its age to be 4 Gyr, its mass to be 1080 solar masses, and the number of white dwarfs to be 150. Hurley et al.[8] estimate its current mass to be 1400 solar masses and its initial mass to be approximately 10 times as great.

M67 has more than 100 stars similar to the Sun, and countless red giants. The total star count has been estimated at well over 500.[9] The cluster contains no main sequence stars bluer than spectral type F, other than perhaps some of the blue stragglers, since the brighter stars of that age have already left the main sequence. In fact, when the stars of the cluster are plotted on the Hertzsprung-Russell diagram, there is a distinct "turn-off" representing the stars which have terminated hydrogen fusion in the core and are destined to become red giants. As the cluster ages, the turn-off moves progressively down the main sequence.

Hertzsprung-Russell diagram for two M67 and NGC 188, showing color-magnitude data for two of the best-studied old open clusters.

It appears that M67 does not contain an unbiased sample of stars. One cause of this is mass segregation, the process by which lighter stars (actually, systems) gain speed at the expense of more massive stars during close encounters, which causes the lighter stars to be at a greater average distance from the center of the cluster or to escape altogether[10]

References

  1. ^ a b Paunzen, E., Mermilliod, J.-C. "WEBDA: M67"
  2. ^ a b c Sarajedini, Ata; Dotter, Aaron; Kirkpatrick, Allison "Deep 2MASS Photometry of M67 and Calibration of the Main-Sequence J - KS Color Difference as an Age Indicator", AJ, 2009
  3. ^ a b c Yakut, K.; Zima, W.; Kalomeni, B.; van Winckel, H.; Waelkens, C.; De Cat, P.; Bauwens, E.; Vučković, M.; Saesen, S.; Le Guillou, L.; Parmaksızoğlu, M.; Uluç, K.; Khamitov, I.; Raskin, G.; Aerts, C."Close binary and other variable stars in the solar-age Galactic open cluster M 67", A&A, 2009
  4. ^ a b c Majaess, D.; Turner, D.; Lane, D.; Krajci, T. "Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars", JAAVSO, 2011
  5. ^ Xiao-Bin Zhang, Rong-Xian Zhang and Zhi-Ping Li (2005). "S1280 and S1284: Two Oscillating Blue Stragglers in the Open Cluster M67". Chinese Journal of Astronomy and Astrophysics 5 (6): 579–586. Bibcode 2005ChJAA...5..579Z. doi:10.1088/1009-9271/5/6/003. 
  6. ^ Kenneth A. Janes and Graeme H. Smith (1984). "The Giant Branch of the Old Open Cluster M67". Astronomical Journal 89 (4): 487–495. Bibcode 1984AJ.....89..487J. doi:10.1086/113539. 
  7. ^ Harvey B. Richer, Gregory G. Fahlman, Joanne Rosvick, Rodrigo Ibata (1998). Astrophysical Journal Letters. 504. pp. L91. arXiv:astro-ph/9806172. Bibcode 1998ApJ...504L..91R. doi:10.1086/311586. 
  8. ^ Jarrod R. Hurley, Onno R. Pols, Sverre J. Aarseth, Christopher A. Tout (2005). "A Complete N-body Model of the Old Open Cluster M67". Monthly Notices of the Royal Astronomical Society 363: 293–314. arXiv:astro-ph/0507239. Bibcode 2005MNRAS.363..293H. doi:10.1111/j.1365-2966.2005.09448.x. 
  9. ^ W. L. Sanders (1977). "Membership of the open cluster M67". Astronomy & Astrophysics Supplement Series 27: 89–116. Bibcode 1977A&AS...27...89S. 
  10. ^ Ch. Bonatto and E. Bica (2003). "Mass segregation in M67 with 2MASS". Astronomy and Astrophysics 405: 525. Bibcode 2003A&A...405..525B. doi:10.1051/0004-6361:20030205. http://www.aanda.org/articles/aa/pdf/2003/26/aah4157.pdf. 

External links

Coordinates: Sky map 08h 51.4m 00s, +11° 49′ 00″


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