Messier 34
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| Messier 34 | |
|---|---|
| Lua error in package.lua at line 80: module 'Module:InfoboxImage/data' not found. Open cluster Messier 34 in Perseus | |
| Observation data (J2000.0 epoch) | |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Distance | 1,500 light years (470 pc[2]) |
| Apparent magnitude (V) | 5.5[3] |
| Apparent dimensions (V) | 35.0′[3] |
| Physical characteristics | |
| Radius | 7 ly |
| Estimated age | 200–250 million years[2] |
| Other designations | NGC 1039, Cr 31, OCl 382, C 0238+425[1] |
| Associations | |
| Constellation | Perseus[3] |
Messier 34 (also known as M34, NGC 1039, or the Spiral Cluster) is a large and relatively near open cluster in Perseus. It was probably discovered by Giovanni Batista Hodierna before 1654[4] and included by Charles Messier in his catalog of comet-like objects in 1764. Messier described it as, "A cluster of small stars a little below the parallel of γ (Andromedae). In an ordinary telescope of 3 feet one can distinguish the stars."[3]
Based on the distance modulus of 8.38, it is about 470 parsecs (1,500 ly) away.[2] For stars ranging from 0.12 to 1 solar mass (M☉), the cluster has about 400.[5] It spans about 35′ on the sky which translates to a true radius of 7.5 light years at such distance.[6] The cluster is just visible to the naked eye in very dark conditions, well away from city lights. It is possible to see it in binoculars when light pollution is low.[3]
The age of this cluster lies between the ages of the Pleiades open cluster at 100 million years and the Hyades open cluster at 800 million years. Specifically, comparison between noted stellar spectra and the values predicted by stellar evolutionary models suggest 200–250 million years.[2] This is roughly the age at which stars with half a solar mass enter the main sequence. By comparison, stars like the Sun enter the main sequence after 30 million years.[5]
The average proportion of elements with higher atomic numbers than helium is termed the metallicity by astronomers. This is expressed by the logarithm of the ratio of iron to hydrogen, compared to the same proportion in the Sun. For M34, the metallicity has a value of [Fe/H] = +0.07 ± 0.04. This is equivalent to a 17% higher proportion of iron compared to the Sun. Other elements show a similar abundance, save for nickel which is underabundant.[7]
At least 19 members are white dwarfs. These are stellar remnants of progenitor stars of up to eight solar masses (M☉) that have evolved through the main sequence and are no longer have thermonuclear fusion to generate energy. Seventeen of these are of spectral type DA or DAZ, while one is a type DB and the last is a type DC.[8]
See also
References
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- ^ a b c
Page Module:Citation/CS1/styles.css has no content."M 34". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-09-03.
{{cite web}}: Invalid|mode=Script error: No such module "Citation mode".(help) - ^ a b c d Page Module:Citation/CS1/styles.css has no content.Jones, B. F.; Prosser, Charles F. (1996). "Membership of Stars in NGC 1039 (M34)". Astronomical Journal. 111: 1193. Bibcode:1996AJ....111.1193J. doi:10.1086/117865.
- ^ a b c d e Page Module:Citation/CS1/styles.css has no content.Jones, Kenneth Glyn (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge University Press. p. 139. ISBN 978-0-521-37079-0.
- ^ Page Module:Citation/CS1/styles.css has no content."Messier 34". SEDS Messier Catalog. Retrieved 23 July 2024.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Irwin, Jonathan; et al. (2006). "The Monitor project: rotation of low-mass stars in the open cluster M34". Monthly Notices of the Royal Astronomical Society. 370 (2): 954–974. arXiv:astro-ph/0605617. Bibcode:2006MNRAS.370..954I. doi:10.1111/j.1365-2966.2006.10521.x. S2CID 10454602.
- ^ Page Module:Citation/CS1/styles.css has no content.freestarcharts.com. "Messier 34 - M34 - Open Cluster | freestarcharts.com". freestarcharts.com. Retrieved 2018-10-25.
- ^ Page Module:Citation/CS1/styles.css has no content.Schuler, Simon C.; et al. (2003). "Spectroscopic Abundances of Solar-Type Dwarfs in the Open Cluster M34 (NGC 1039)". Astronomical Journal. 125 (4): 2085–2097. Bibcode:2003AJ....125.2085S. doi:10.1086/373927.
- ^ Page Module:Citation/CS1/styles.css has no content.Rubin, Kate H. R.; Williams, Kurtis A.; Bolte, M.; Koester, Detlev (2008). "The White Dwarf Population in NGC 1039 (M34) and the White Dwarf Initial-Final Mass Relation". Astronomical Journal. 135 (6): 2163–2176. arXiv:0805.3156. Bibcode:2008AJ....135.2163R. doi:10.1088/0004-6256/135/6/2163. S2CID 1481865.
External links
- Page Template:Sister-inline/styles.css has no content.Script error: No such module "Sister project logo". Media related to Script error: No such module "Commons link". at Wikimedia Commons
- Messier 34, SEDS Messier pages
- Messier 34 – Image by Donald P. Waid
- Page Module:Citation/CS1/styles.css has no content.Gretton, Roy; Gray, Meghan; Szymanek, Nik. "M34 – Open Cluster". Deep Sky Videos. Brady Haran.
- Template:WikiSky
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