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Messier 67

February 26, 2024

Messier 67 (also known as M67 or NGC 2682) and sometimes called the King Cobra Cluster or the Golden Eye Cluster[5] is an open cluster in the southern, equatorial half of Cancer. It was discovered by Johann Gottfried Koehler in 1779. Estimates of its age range between 3.2 and 5 billion years. Distance estimates are likewise varied, but typically are 800–900 parsecs (2,600–2,900 ly).[1][2][3][4] Estimates of 855, 840, and 815 pc were established via binary star modelling and infrared color-magnitude diagram fitting.[2][3][4]

Messier 67
Open cluster Messier 67 in Cancer
Observation data (J2000.0 epoch)
Right ascension08h 51.3m
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
Radius10 ly[citation needed]
Estimated age3.2 to 5 billion years
Other designationsNGC 2682, Cr 204
Associations
ConstellationCancer
See also: Open cluster, List of open clusters

Description edit

M67 is not the oldest known open cluster, but there are few Milky Way clusters known to be older, and none of those is closer than M67. It is a paradigm study object in stellar evolution:[6]

  • it is well-populated
  • has negligible amounts of dust obscuration
  • all its stars are at the same distance and age, save for approximately 30 anomalous blue stragglers

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. estimate its age to be 4 billion years, its mass to be 1080 solar masses (M☉), and number its white dwarfs at 150.[7] Hurley et al. estimate its current mass to be 1,400 M☉ and its initial mass to be approximately 10 times as great.[8]

It has more than 100 stars similar to the Sun, and numerous red giants. The total star count has been estimated at well over 500.[9] The ages and prevalence of Sun-like stars had led some astronomers to theorize it as the possible parent cluster of the Sun.[10] However, computer simulations have suggested that this is highly unlikely.[11]

The cluster contains no main sequence stars bluer (hotter) 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 a cluster ages, the turn-off moves progressively down the main sequence to cooler stars.

It appears that M67 has a bias toward heavier stars. One cause of this is mass segregation, the process by which lighter stars gain speed at the expense of more massive stars during close encounters, which moves them to greater average distance from the center of the cluster or allows escape altogether.[12]

A March 2016 joint AIP/JHU study by Barnes et al. on rotational periods of 20 Sun-like stars, measured by the effects of moving starspots on light curves, suggests that these approximately 4 billion-year old stars spin in about 26 days – like the Sun, which has a period at the equator of 25.38 days.[13] Measurements were carried out as part of the extended K2 mission of Kepler space telescope. This reinforces the applicability of many key properties of the sun to stars of the same size and age, a fundamental principle of modern solar and stellar physics.[14] The authors abbreviate this as the "solar-stellar connection".[14]

Planets edit

A radial velocity survey of M67 has found exoplanets around four stars in the cluster: YBP 1194, YBP 1514, YBP 401, and Sand 978.[15][16][17] A fifth star, Sand 364, was also thought to have a planet, but a follow-up study did not find evidence for it and concluded that the radial velocity variations have a non-planetary origin, likely stellar variability.[18]

Gallery edit

  •  
    Messier 67 (SDSS, optical and near-infrared)
  •  
    Hertzsprung-Russell diagram for two open clusters, M67 and NGC 188, showing color-magnitude data
  • Artist's impression video showing a hot Jupiter exoplanet orbiting close to a star in Messier 67
  •  
    Artist's impression of a hot Jupiter exoplanet in the star cluster Messier 67

See also edit

References edit

  1. ^ a b Paunzen, E.; Mermilliod, J.-C. "WEBDA page for open cluster NGC 2682". WEBDA. Retrieved 2022-10-12.
  2. ^ a b c Sarajedini, Ata; Dotter, Aaron; Kirkpatrick, Allison (2009). "Deep 2MASS Photometry of M67 and Calibration of the Main-Sequence J - KS Color Difference as an Age Indicator". The Astrophysical Journal. 698 (2): 1872–1878. arXiv:0904.2907. Bibcode:2009ApJ...698.1872S. doi:10.1088/0004-637X/698/2/1872. S2CID 11654120.
  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. (2009). "Close binary and other variable stars in the solar-age Galactic open cluster M 67". Astronomy and Astrophysics. 503 (1): 165. arXiv:0906.4908. Bibcode:2009A&A...503..165Y. doi:10.1051/0004-6361/200911918. S2CID 1136371.
  4. ^ a b c Majaess, Daniel J.; Turner, David G.; Lane, David J.; Krajci, Tom (2011). "Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars". Journal of the American Association of Variable Star Observers (Jaavso). 39 (2): 219. arXiv:1102.1705. Bibcode:2011JAVSO..39..219M.
  5. ^ Martina McGovern. "M67 Open cluster". British Astronomical Association. Retrieved 2022-10-12.
  6. ^ Xiao-Bin Zhang; Rong-Xian Zhang & 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.
  7. ^ Harvey B. Richer; Gregory G. Fahlman; Joanne Rosvick; Rodrigo Ibata (1998). "The White Dwarf Cooling Age of M67". The Astrophysical Journal. 504 (2): L91. arXiv:astro-ph/9806172. Bibcode:1998ApJ...504L..91R. doi:10.1086/311586. S2CID 17309096.
  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 (1): 293–314. arXiv:astro-ph/0507239. Bibcode:2005MNRAS.363..293H. doi:10.1111/j.1365-2966.2005.09448.x. S2CID 17632739.
  9. ^ W. L. Sanders (1977). "Membership of the open cluster M67". Astronomy & Astrophysics Supplement Series. 27: 89–116. Bibcode:1977A&AS...27...89S.
  10. ^ . Daily Galaxy. 30 September 2014. Archived from the original on 10 May 2016. Retrieved 30 March 2016.
  11. ^ Pichardo, Bárbara; Moreno, Edmundo; Allen, Christine; Bedin, Luigi R.; Bellini, Andrea; Pasquini, Luca (February 2012). "The Sun was not born in M 67". The Astronomical Journal. 143 (3): 73. arXiv:1201.0987. Bibcode:2012AJ....143...73P. doi:10.1088/0004-6256/143/3/73. S2CID 119266159. article ID 73.
  12. ^ Ch. Bonatto & E. Bica (2003). "Mass segregation in M67 with 2MASS" (PDF). Astronomy and Astrophysics. 405 (2): 525. Bibcode:2003A&A...405..525B. doi:10.1051/0004-6361:20030205.
  13. ^ Sydney A. Barnes; Jörg Weingrill; Dario Fritzewski; Klaus G. Strassmeier; Imants Platais (2016). "Rotation periods for cool stars in the 4 Gyr-old open cluster M67, the solar-stellar connection, and the applicability of gyrochronology to at least solar age". The Astrophysical Journal. 823 (1): 16. arXiv:1603.09179. Bibcode:2016ApJ...823...16B. doi:10.3847/0004-637X/823/1/16. S2CID 89613927.
  14. ^ a b "Stars nearly as old as Sun found to have similar spin rates". Astronomy Now. 17 May 2016.
  15. ^ Brucalassi, A.; Pasquini, L.; et al. (January 2014). "Three planetary companions around M 67 stars". Astronomy & Astrophysics. 561: L9. arXiv:1401.4905. Bibcode:2014A&A...561L...9B. doi:10.1051/0004-6361/201322584.
  16. ^ Brucalassi, A.; Pasquini, L.; et al. (July 2016). "Search for giant planets in M67. III. Excess of hot Jupiters in dense open clusters". Astronomy & Astrophysics. 592: L1. arXiv:1606.05247. Bibcode:2016A&A...592L...1B. doi:10.1051/0004-6361/201527561.
  17. ^ Brucalassi, A.; Koppenhoefer, J.; et al. (July 2017). "Search for giant planets in M 67. IV. Survey results". Astronomy & Astrophysics. 603: A85. arXiv:1703.04296. Bibcode:2017A&A...603A..85B. doi:10.1051/0004-6361/201527562.
  18. ^ Zhou, Qijia; Latham, David W.; et al. (October 2023). "False Planets around Giant Stars: A Case Study of Sanders 364 in M67". The Astronomical Journal. 166 (4): 160. Bibcode:2023AJ....166..160Z. doi:10.3847/1538-3881/acf291.

External links edit

  •   Media related to Messier 67 at Wikimedia Commons
  • Messier 67, SEDS Messier pages
  • Merrifield, Mike. "M67 – Open Cluster". Deep Sky Videos. Brady Haran.
  • Messier 67 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images


February 26, 2024
messier, also, known, 2682, sometimes, called, king, cobra, cluster, golden, cluster, open, cluster, southern, equatorial, half, cancer, discovered, johann, gottfried, koehler, 1779, estimates, range, between, billion, years, distance, estimates, likewise, var. Messier 67 also known as M67 or NGC 2682 and sometimes called the King Cobra Cluster or the Golden Eye Cluster 5 is an open cluster in the southern equatorial half of Cancer It was discovered by Johann Gottfried Koehler in 1779 Estimates of its age range between 3 2 and 5 billion years Distance estimates are likewise varied but typically are 800 900 parsecs 2 600 2 900 ly 1 2 3 4 Estimates of 855 840 and 815 pc were established via binary star modelling and infrared color magnitude diagram fitting 2 3 4 Messier 67Open cluster Messier 67 in CancerObservation data J2000 0 epoch Right ascension08h 51 3mDeclination 11 49 Distance 2 61 2 93 kly 800 900 pc 1 2 3 4 Apparent magnitude V 6 1Apparent dimensions V 30 0 Physical characteristicsRadius10 ly citation needed Estimated age3 2 to 5 billion yearsOther designationsNGC 2682 Cr 204AssociationsConstellationCancerSee also Open cluster List of open clusters Contents 1 Description 2 Planets 3 Gallery 4 See also 5 References 6 External linksDescription editM67 is not the oldest known open cluster but there are few Milky Way clusters known to be older and none of those is closer than M67 It is a paradigm study object in stellar evolution 6 it is well populated has negligible amounts of dust obscuration all its stars are at the same distance and age save for approximately 30 anomalous blue stragglersM67 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 estimate its age to be 4 billion years its mass to be 1080 solar masses M and number its white dwarfs at 150 7 Hurley et al estimate its current mass to be 1 400 M and its initial mass to be approximately 10 times as great 8 It has more than 100 stars similar to the Sun and numerous red giants The total star count has been estimated at well over 500 9 The ages and prevalence of Sun like stars had led some astronomers to theorize it as the possible parent cluster of the Sun 10 However computer simulations have suggested that this is highly unlikely 11 The cluster contains no main sequence stars bluer hotter 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 a cluster ages the turn off moves progressively down the main sequence to cooler stars It appears that M67 has a bias toward heavier stars One cause of this is mass segregation the process by which lighter stars gain speed at the expense of more massive stars during close encounters which moves them to greater average distance from the center of the cluster or allows escape altogether 12 A March 2016 joint AIP JHU study by Barnes et al on rotational periods of 20 Sun like stars measured by the effects of moving starspots on light curves suggests that these approximately 4 billion year old stars spin in about 26 days like the Sun which has a period at the equator of 25 38 days 13 Measurements were carried out as part of the extended K2 mission of Kepler space telescope This reinforces the applicability of many key properties of the sun to stars of the same size and age a fundamental principle of modern solar and stellar physics 14 The authors abbreviate this as the solar stellar connection 14 Planets editA radial velocity survey of M67 has found exoplanets around four stars in the cluster YBP 1194 YBP 1514 YBP 401 and Sand 978 15 16 17 A fifth star Sand 364 was also thought to have a planet but a follow up study did not find evidence for it and concluded that the radial velocity variations have a non planetary origin likely stellar variability 18 Gallery edit nbsp Messier 67 SDSS optical and near infrared nbsp Hertzsprung Russell diagram for two open clusters M67 and NGC 188 showing color magnitude data source source source source source source source source Artist s impression video showing a hot Jupiter exoplanet orbiting close to a star in Messier 67 nbsp Artist s impression of a hot Jupiter exoplanet in the star cluster Messier 67See also editList of Messier objects List of open clusters Open cluster family Open cluster remnantReferences edit a b Paunzen E Mermilliod J C WEBDA page for open cluster NGC 2682 WEBDA Retrieved 2022 10 12 a b c Sarajedini Ata Dotter Aaron Kirkpatrick Allison 2009 Deep 2MASS Photometry of M67 and Calibration of the Main Sequence J KS Color Difference as an Age Indicator The Astrophysical Journal 698 2 1872 1878 arXiv 0904 2907 Bibcode 2009ApJ 698 1872S doi 10 1088 0004 637X 698 2 1872 S2CID 11654120 a b c Yakut K Zima W Kalomeni B Van Winckel H Waelkens C De Cat P Bauwens E Vuckovic M Saesen S Le Guillou L Parmaksizoglu M Uluc K Khamitov I Raskin G Aerts C 2009 Close binary and other variable stars in the solar age Galactic open cluster M 67 Astronomy and Astrophysics 503 1 165 arXiv 0906 4908 Bibcode 2009A amp A 503 165Y doi 10 1051 0004 6361 200911918 S2CID 1136371 a b c Majaess Daniel J Turner David G Lane David J Krajci Tom 2011 Deep Infrared ZAMS Fits to Benchmark Open Clusters Hosting delta Scuti Stars Journal of the American Association of Variable Star Observers Jaavso 39 2 219 arXiv 1102 1705 Bibcode 2011JAVSO 39 219M Martina McGovern M67 Open cluster British Astronomical Association Retrieved 2022 10 12 Xiao Bin Zhang Rong Xian Zhang amp 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 Harvey B Richer Gregory G Fahlman Joanne Rosvick Rodrigo Ibata 1998 The White Dwarf Cooling Age of M67 The Astrophysical Journal 504 2 L91 arXiv astro ph 9806172 Bibcode 1998ApJ 504L 91R doi 10 1086 311586 S2CID 17309096 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 1 293 314 arXiv astro ph 0507239 Bibcode 2005MNRAS 363 293H doi 10 1111 j 1365 2966 2005 09448 x S2CID 17632739 W L Sanders 1977 Membership of the open cluster M67 Astronomy amp Astrophysics Supplement Series 27 89 116 Bibcode 1977A amp AS 27 89S Did Our Solar System Originate in a Distant Star Cluster Daily Galaxy 30 September 2014 Archived from the original on 10 May 2016 Retrieved 30 March 2016 Pichardo Barbara Moreno Edmundo Allen Christine Bedin Luigi R Bellini Andrea Pasquini Luca February 2012 The Sun was not born in M 67 The Astronomical Journal 143 3 73 arXiv 1201 0987 Bibcode 2012AJ 143 73P doi 10 1088 0004 6256 143 3 73 S2CID 119266159 article ID 73 Ch Bonatto amp E Bica 2003 Mass segregation in M67 with 2MASS PDF Astronomy and Astrophysics 405 2 525 Bibcode 2003A amp A 405 525B doi 10 1051 0004 6361 20030205 Sydney A Barnes Jorg Weingrill Dario Fritzewski Klaus G Strassmeier Imants Platais 2016 Rotation periods for cool stars in the 4 Gyr old open cluster M67 the solar stellar connection and the applicability of gyrochronology to at least solar age The Astrophysical Journal 823 1 16 arXiv 1603 09179 Bibcode 2016ApJ 823 16B doi 10 3847 0004 637X 823 1 16 S2CID 89613927 a b Stars nearly as old as Sun found to have similar spin rates Astronomy Now 17 May 2016 Brucalassi A Pasquini L et al January 2014 Three planetary companions around M 67 stars Astronomy amp Astrophysics 561 L9 arXiv 1401 4905 Bibcode 2014A amp A 561L 9B doi 10 1051 0004 6361 201322584 Brucalassi A Pasquini L et al July 2016 Search for giant planets in M67 III Excess of hot Jupiters in dense open clusters Astronomy amp Astrophysics 592 L1 arXiv 1606 05247 Bibcode 2016A amp A 592L 1B doi 10 1051 0004 6361 201527561 Brucalassi A Koppenhoefer J et al July 2017 Search for giant planets in M 67 IV Survey results Astronomy amp Astrophysics 603 A85 arXiv 1703 04296 Bibcode 2017A amp A 603A 85B doi 10 1051 0004 6361 201527562 Zhou Qijia Latham David W et al October 2023 False Planets around Giant Stars A Case Study of Sanders 364 in M67 The Astronomical Journal 166 4 160 Bibcode 2023AJ 166 160Z doi 10 3847 1538 3881 acf291 External links edit nbsp Media related to Messier 67 at Wikimedia Commons Messier 67 SEDS Messier pages Merrifield Mike M67 Open Cluster Deep Sky Videos Brady Haran Messier 67 on WikiSky DSS2 SDSS GALEX IRAS Hydrogen a X Ray Astrophoto Sky Map Articles and images Portals nbsp Astronomy nbsp Stars nbsp Outer space Retrieved from https en wikipedia org w index php title Messier 67 amp oldid 1209956660, wikipedia, wiki, book, books, library,

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