Messier 30

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Messier 30
Messier 30 Hubble WikiSky.jpg
M30 by Hubble Space Telescope; 3.5′ view
Credit: NASA/STScI/WikiSky
Observation data (J2000 epoch)
Class V[1]
Constellation Capricornus
Right ascension 21h 40m 22.12s[2]
Declination –23° 10′ 47.5″[2]
Distance 29.4 ± 1.6 kly (9 ± 0.5 kpc)[3]
Apparent magnitude (V) +7.7[4]
Physical characteristics
Mass 1.6×105[5] M
Metallicity –2.27[6] dex
Estimated age 12.93 Gyr[7]
Other designations M30, NGC 7099, GCl 122[4]
See also: Globular cluster, List of globular clusters

Messier 30 (also known as M30 or NGC 7099) is a globular cluster of stars in the southern constellation of Capricornus. It was discovered by the French astronomer Charles Messier in 1764, who described it as a circular nebula without a star. In the New General Catalogue, compiled during the 1880s, it was described as a "remarkable globular, bright, large, slightly oval." This cluster can be easily viewed with a pair of 10×50 binoculars,[8] forming a patch of hazy light some 4 arcminutes wide that is slightly elongated along the east-west axis.[8] With a larger instrument, individual stars can be resolved and the cluster will cover an angle of up to 12 arcminutes across with a compressed core one arcminute wide.[9] It is best observed around August.[8]

M30 is located at a distance of about 29,400 light-years from Earth,[3] and is about 93 light-years across.[9] The estimated age is roughly 12.93 billion years[7] and it has a combined mass of about 160,000 times the mass of the Sun.[5] The cluster is following a retrograde orbit through the inner galactic halo, suggesting that it was acquired from a satellite galaxy rather than forming within the Milky Way.[7] It is currently located at a distance of about 22.2 kly (6.8 kpc) from the center of the galaxy, compared to an estimated 26 kly (8.0 kpc) for the Sun.[10]

The M30 cluster has passed through a dynamic process called core collapse and now has a concentration of mass at its core of about a million times the Sun's mass per cubic parsec. This makes it one of the highest density regions in the Milky Way galaxy. Stars in such close proximity will experience a high rate of interactions that can create binary star systems, as well as a type of star called a blue straggler that is formed by mass transfer.[3] A process of mass segregation may have caused the central region to gain a greater proportion of higher mass stars, creating a color gradient with increasing blueness toward the middle of the cluster.[11]

References[edit]

  1. ^ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin 849 (849): 11–14, Bibcode:1927BHarO.849...11S. 
  2. ^ a b Goldsbury, Ryan et al. (December 2010), "The ACS Survey of Galactic Globular Clusters. X. New Determinations of Centers for 65 Clusters", The Astronomical Journal 140 (6): 1830–1837, arXiv:1008.2755, Bibcode:2010AJ....140.1830G, doi:10.1088/0004-6256/140/6/1830. 
  3. ^ a b c Lugger, Phyllis M. et al. (March 2007), "Chandra X-Ray Sources in the Collapsed-Core Globular Cluster M30 (NGC 7099)", The Astrophysical Journal 657 (1): 286–301, arXiv:astro-ph/0606382, Bibcode:2007ApJ...657..286L, doi:10.1086/507572 
  4. ^ a b "NGC 7099", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2006-11-16 
  5. ^ a b Vande Putte, D.; Cropper, Mark (January 2009), "Detecting the effect of globular cluster impacts on the disc of the Milky Way", Monthly Notices of the Royal Astronomical Society 392 (1): 113–124, arXiv:0811.3106, Bibcode:2009MNRAS.392..113V, doi:10.1111/j.1365-2966.2008.14072.x 
  6. ^ Boyles, J. et al. (November 2011), "Young Radio Pulsars in Galactic Globular Clusters", The Astrophysical Journal 742 (1): 51, arXiv:1108.4402, Bibcode:2011ApJ...742...51B, doi:10.1088/0004-637X/742/1/51. 
  7. ^ a b c Forbes, Duncan A.; Bridges, Terry (May 2010), "Accreted versus in situ Milky Way globular clusters", Monthly Notices of the Royal Astronomical Society 404 (3): 1203–1214, arXiv:1001.4289, Bibcode:2010MNRAS.404.1203F, doi:10.1111/j.1365-2966.2010.16373.x 
  8. ^ a b c Bone, N. M. (August 2008), "Sky notes, 2008 August & September", Journal of the British Astronomical Association 118 (4): 231–232, Bibcode:2008JBAA..118..231B 
  9. ^ a b O'Meara, Stephen James (1998), The Messier objects, Deep-sky companions, Cambridge University Press, p. 108, ISBN 0-521-55332-6 
  10. ^ Dinescu, Dana I. et al. (January 1999), "Space Velocities of Southern Globular Clusters. II. New Results for 10 Clusters", The Astronomical Journal 117 (1): 277–285, Bibcode:1999AJ....117..277D, doi:10.1086/300699 
  11. ^ Howell, Justin H.; Guhathakurta, Puragra; Tan, Amy (March 2000), "Radial Color Gradient and Main-Sequence Mass Segregation in M30 (NGC 7099)", The Astronomical Journal 119 (3): 1259–1267, arXiv:astro-ph/9912002, Bibcode:2000AJ....119.1259H, doi:10.1086/301270 

External links[edit]

Coordinates: Sky map 21h 40m 22.03s, −23° 10′ 44.6″