Messier 14: Difference between revisions
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At a distance of about 30,000 [[light-year]]s, M14 contains several hundred thousand [[star]]s. At an [[apparent magnitude]] of +7.6 it can be easily observed with [[binoculars]]. Medium-sized [[telescope]]s will show some hint of the individual stars of which the brightest is of magnitude +14. |
At a distance of about 30,000 [[light-year]]s, M14 contains several hundred thousand [[star]]s. At an [[apparent magnitude]] of +7.6 it can be easily observed with [[binoculars]]. Medium-sized [[telescope]]s will show some hint of the individual stars of which the brightest is of magnitude +14. |
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The total [[luminosity]] of M14 is in the order of 400,000 times that of the [[Sun]] corresponding to an [[absolute magnitude]] of -9.12. The shape of the cluster is decidedly elongated. M14 is about 100 light-years across<ref>{{Cite web|url=https |
The total [[luminosity]] of M14 is in the order of 400,000 times that of the [[Sun]] corresponding to an [[absolute magnitude]] of -9.12. The shape of the cluster is decidedly elongated. M14 is about 100 light-years across<ref>{{Cite web|url=https://www.messier-objects.com/messier-14/|title=Messier 14 {{!}} Messier Objects|language=en-US|access-date=2020-04-14}}</ref>. |
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A total of 70 [[variable star]]s are known in M14, many of the [[W Virginis variable|W Virginis]] variety common in globular clusters. In 1938, a [[nova]] appeared, although this was not discovered until [[photographic plates]] from that time were studied in 1964. It is estimated that the nova reached a maximum brightness of magnitude +9.2, over five times brighter than the brightest 'normal' star in the cluster. |
A total of 70 [[variable star]]s are known in M14, many of the [[W Virginis variable|W Virginis]] variety common in globular clusters. In 1938, a [[nova]] appeared, although this was not discovered until [[photographic plates]] from that time were studied in 1964. It is estimated that the nova reached a maximum brightness of magnitude +9.2, over five times brighter than the brightest 'normal' star in the cluster. |
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Revision as of 15:19, 14 April 2020
| Messier 14 | |
|---|---|
 Messier 14, from 2MASS | |
| Observation data (J2000 epoch) | |
| Class | VIII[1] |
| Constellation | Ophiuchus |
| Right ascension | 17h 37m 36.15s[2] |
| Declination | –03° 14′ 45.3″[2] |
| Distance | 30.3 kly (9.3 kpc)[3] |
| Apparent magnitude (V) | +8.32[2] |
| Apparent dimensions (V) | 11.0′ |
| Physical characteristics | |
| Mass | 1.04×106[3] M☉ |
| Radius | 50 ly[4] |
| Metallicity | = –1.28[3] dex |
| Other designations | NGC 6402[2] |
![{\displaystyle {\begin{smallmatrix}\left[{\ce {Fe}}/{\ce {H}}\right]\end{smallmatrix}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/4c0821bd80891e071c08e7c7ee8e022baedf522c)
Messier 14 (also known as M14 or NGC 6402) is a globular cluster of stars in the constellation Ophiuchus. It was discovered by Charles Messier in 1764.
At a distance of about 30,000 light-years, M14 contains several hundred thousand stars. At an apparent magnitude of +7.6 it can be easily observed with binoculars. Medium-sized telescopes will show some hint of the individual stars of which the brightest is of magnitude +14.
The total luminosity of M14 is in the order of 400,000 times that of the Sun corresponding to an absolute magnitude of -9.12. The shape of the cluster is decidedly elongated. M14 is about 100 light-years across[5].
A total of 70 variable stars are known in M14, many of the W Virginis variety common in globular clusters. In 1938, a nova appeared, although this was not discovered until photographic plates from that time were studied in 1964. It is estimated that the nova reached a maximum brightness of magnitude +9.2, over five times brighter than the brightest 'normal' star in the cluster.
Slightly over 3° southwest of M14 lies the faint globular cluster NGC 6366.
Gallery
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Messier 14 with amateur telescope -
Map showing location of Messier 14
References
- ^ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin, 849 (849): 11–14, Bibcode:1927BHarO.849...11S.
- ^ a b c d "NGC 6402". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2006-11-15.
- ^ a b c 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.
- ^ distance × sin( diameter_angle / 2 ) = 50 ly radius
- ^ "Messier 14 | Messier Objects". Retrieved 2020-04-14.
External links
- SEDS Messier pages on M14
- M14, Galactic Globular Clusters Database page
- NASA Astronomy Picture of the Day: The Comet and the Star Cluster (11 April 2016) - one of the two being M14
- Messier 14 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
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