NGC 4103

Last updated
NGC 4103
NGC 4103.png
Observation data (J2000 epoch)
Right ascension 12h 00m 39s [1]
Declination −61° 55′ 00″ [1]
Distance 5,320 ly (1,632 pc [2] )
Apparent magnitude  (V)7.4 [1]
Apparent dimensions (V)12' [3]
Physical characteristics
Mass1,180 [4]   M☉
Estimated age25 million years [2]
Other designations Collinder 252, Melotte 109
Associations
Constellation Crux
See also: Open cluster, List of open clusters

NGC 4103 is an open cluster in the constellation Crux. It was discovered by James Dunlop in 1826. It is located approximately 5,000 light years away from Earth, in the Carina-Sagittarius arm. [5]

Contents

Characteristics

Location within the constellation NGC 4103 map.png
Location within the constellation

NGC 4103 is a young open cluster. Its age has been determined to be 30 Myr by Sagar & Cannon (1997), [6] 20 ± 5 Myr by Sanner et al. (2001) [7] and 6 Myr by Piskunov et al. (2004). [8] The metallicity of NGC 4103 is subsolar (−0.47). [9] The tidal radius of the cluster is 12.1 - 15.9 parsecs (39 - 51 light years) and represents the average outer limit of NGC 4103, beyond which a star is unlikely to remain gravitationally bound to the cluster core. [4]

Members

There are 421 probable member stars within the angular radius of the cluster and 199 within the central part of the cluster. [3] No blue straggler has been detected in the cluster. [10] The cluster is not very richly populated and is dominated by moderately bright stars of 10th magnitude and fainter. [7] The hottest stars of the cluster are of spectral type B2. [11] No red giants have been found to be members of the cluster. [7] One member of the cluster is a Be star. [7] [12]

Among the members of the cluster is AI Crucis, a short-period semi-detached massive close binary star, with orbit period 1.41771 days. The orbital period of the binary is continuously increasing and this has been explained on the grounds of mass transfer from the less massive component to the more massive one and strong stellar wind from the hot component. It is estimated that 4.1 M☉ have been transferred from the hot component to the more massive. [13]

Related Research Articles

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<span class="mw-page-title-main">NGC 7160</span> Open cluster in the constellation Cepheus

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References

  1. 1 2 3 "NGC 4103". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2017-08-19.
  2. 1 2 WEBDA page for open cluster NGC 4103
  3. 1 2 Kharchenko, N. V.; Piskunov, A. E.; Schilbach, E.; Röser, S.; Scholz, R.-D. (3 October 2013). "Global survey of star clusters in the Milky Way". Astronomy & Astrophysics. 558: A53. arXiv: 1308.5822 . Bibcode:2013A&A...558A..53K. doi:10.1051/0004-6361/201322302. S2CID   118548517.
  4. 1 2 Piskunov, A. E.; Schilbach, E.; Kharchenko, N. V.; Röser, S.; Scholz, R.-D. (6 November 2007). "Tidal radii and masses of open clusters". Astronomy & Astrophysics. 477 (1): 165–172. Bibcode:2008A&A...477..165P. doi: 10.1051/0004-6361:20078525 .
  5. ↑ Carraro, Giovanni; Turner, David G.; Majaess, Daniel J.; Baume, Gustavo L.; Gamen, Roberto; Lera, José A. Molina (13 March 2017). "Extinction in the Star Cluster SAI 113 and Galactic Structure in Carina". The Astronomical Journal. 153 (4): 156. arXiv: 1701.08319 . Bibcode:2017AJ....153..156C. doi: 10.3847/1538-3881/aa5c3a . S2CID   119494346.
  6. ↑ Sagar, R.; Cannon, R. D. (15 April 1997). "Multicolour deep CCD photometric study of the moderately youngsouthern open star clusters NGC 3228, NGC 4103, NGC 5662 and NGC 6087". Astronomy and Astrophysics Supplement Series. 122 (1): 9–29. Bibcode:1997A&AS..122....9S. doi: 10.1051/aas:1997293 .
  7. 1 2 3 4 Sanner, J.; Brunzendorf, J.; Will, J.-M.; Geffert, M. (15 April 2001). "Photometric and kinematic studies of open star clusters". Astronomy & Astrophysics. 369 (2): 511–526. arXiv: astro-ph/0101541 . Bibcode:2001A&A...369..511S. doi:10.1051/0004-6361:20010196. S2CID   14693975.
  8. ↑ Piskunov, A. E.; Belikov, A. N.; Kharchenko, N. V.; Sagar, R.; Subramaniam, A. (April 2004). "On the determination of age and mass functions of stars in young open star clusters from the analysis of their luminosity functions". Monthly Notices of the Royal Astronomical Society. 349 (4): 1449–1463. arXiv: astro-ph/0401587 . Bibcode:2004MNRAS.349.1449P. doi:10.1111/j.1365-2966.2004.07620.x. S2CID   119434841.
  9. ↑ Paunzen, E.; Heiter, U.; Netopil, M.; Soubiran, C. (28 July 2010). "On the metallicity of open clusters". Astronomy and Astrophysics. 517: A32. arXiv: 1008.3476 . Bibcode:2010A&A...517A..32P. doi:10.1051/0004-6361/201014131. S2CID   119281965.
  10. ↑ Ahumada, J. A.; Lapasset, E. (20 November 2006). "New catalogue of blue stragglers in open clusters". Astronomy & Astrophysics. 463 (2): 789–797. Bibcode:2007A&A...463..789A. doi: 10.1051/0004-6361:20054590 .
  11. ↑ Wesselink, A. J. (1 October 1969). "Photometry of NGC 4103". Monthly Notices of the Royal Astronomical Society. 146 (3): 329–338. Bibcode:1969MNRAS.146..329W. doi: 10.1093/mnras/146.3.329 .
  12. ↑ Paunzen, E.; Netopil, M.; Maitzen, H. M.; Pavlovski, K.; Schnell, A.; Zejda, M. (3 April 2014). "Photoelectric search for peculiar stars in open clusters". Astronomy & Astrophysics. 564: A42. arXiv: 1403.3538 . Bibcode:2014A&A...564A..42P. doi:10.1051/0004-6361/201423521. S2CID   119174151.
  13. ↑ Zhao, Er-Gang; Qian, Sheng-Bang; Lajús, E. Fernández; Essen, Carolina von; Zhu, Li-Ying (May 2010). "Mass transfer and loss of the massive semi-detached binary AI Crucis". Research in Astronomy and Astrophysics. 10 (5): 438–444. Bibcode:2010RAA....10..438Z. doi: 10.1088/1674-4527/10/5/004 . hdl: 11336/9953 . S2CID   250683139.


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