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Messier Index/M44

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The Beehive Cluster (also known as Praesepe (Latin for "manger"), M44, NGC 2632, or Cr 189) is an w:open cluster in the constellation Cancer. It is one of the nearest open clusters to the w:Solar System, and it contains a larger star population than most other nearby clusters. Under dark skies the Beehive Cluster looks like a nebulous object to the naked eye; thus it has been known since ancient times. The classical astronomer w:Ptolemy called it "the nebulous mass in the breast of Cancer," and it was among the first objects that w:Galileo studied with his telescope.[3]

Beehive Cluster
The Beehive Cluster is an w:open cluster in Cancer just visible to the naked eye.
Observation data (J2000.0 epoch)
ConstellationCancer
Right ascension08h 40.4m
Declination19° 41′
Distance577 ly (177 pc)
Apparent magnitude (V)3.1[1][2]
Apparent dimensions (V)95′
Other designationsM44, Praesepe, NGC 2632

The cluster's age and proper motion coincide with those of the Hyades open cluster, suggesting that both share a similar origin.[4][5] Both clusters also contain w:red giants and w:white dwarfs, which represent later stages of stellar evolution, along with w:main sequence stars of w:spectral classes A, F, G, K, and M.

Currently there is no consensus on the cluster's distance, with recent sources suggesting 160 to 187 w:parsecs (520-610 w:light years).[6][7][8] There is better agreement on its age, at about 600 million years.[9][7][5] This is equivalent to the age of the Hyades (~625 million years).[10] The bright central core of the cluster has a diameter of about 7 parsecs (22.8 light years).[9]

The Beehive is most easily observed when Cancer is high in the sky; in northern latitudes this occurs during the evening from February to May. At 95 arcminutes across, the cluster fits well in the field of view of a pair of binoculars or a telescope of low power.

History

Galileo was the first to observe the Beehive in a telescope, in 1609, and was able to resolve it into 40 stars. w:Charles Messier added it to his famous catalog in 1769 after precisely measuring its position in the sky. Along with the w:Orion Nebula and the Pleiades cluster, Messier's inclusion of the Beehive has been noted as curious, as most of Messier's objects were much fainter and more easily confused with comets. One possibility is that Messier simply wanted to have a larger catalog than his scientific rival Lacaille, whose 1755 catalog contained 42 objects, and so he added some bright, well-known objects to boost his list.[11]

Ancient Greeks and Romans saw this object as a manger from which two donkeys, the adjacent stars Asellus Borealis and Asellus Australis, are eating; these are the donkeys that w:Dionysos and w:Silenus rode into battle against the Titans.[12]

This perceived nebulous object is the main celestial object in the 23rd lunar mansion (Hsiu Kuei or Xiu Gui) of ancient Chinese astrology. Ancient Chinese skywatchers saw this as a ghost or demon riding in a carriage and likened its appearance to a "cloud of pollen blown from willow catkins."

Morphology and Composition

Like many w:star clusters of all kinds, Praesepe has experienced w:mass segregation.[13][9][7] This means that bright, massive stars are concentrated in the cluster's core, while dimmer, less massive stars populate its halo (sometimes called the "corona"). The cluster's core radius is estimated at 3.5 parsecs (11.4 light years); its half-mass radius is about 3.9 parsecs (12.7 light years); and its tidal radius is about 12 parsecs (39 light years).[9][7] However, the tidal radius also includes many stars that are merely "passing through" and not bona fide cluster members.

Altogether, the Praesepe cluster contains at least 1000 gravitationally bound stars, for a total mass of about 500-600 Solar masses.[9][7] A recent survey counts 1010 high-probability members, of which 68% are M dwarfs, 30% are Sun-like stars of spectral classes F, G, and K, and about 2% are bright stars of spectral class A.[7] Also present are five giant stars, four of which have spectral class K0 III and the fifth G0 III.[4][14][7]

So far, eleven w:white dwarfs have been identified, representing the final evolutionary phase of the cluster's most massive stars, which originally belonged to spectral type B.[5] w:Brown dwarfs, however, are extremely rare in this cluster,[15] probably because they have been lost by tidal stripping from the halo.[7]

The cluster has a visual brightness of magnitude 3.1. Its brightest stars are blue-white and of magnitude 6 to 6.5. w:42 Cancri is a confirmed member.

References

  1. ↑ (IAAC) OBJECT: M44 (Beehive cluster)
  2. ↑ Beehive Cluster - Encharta
  3. ↑ Messier 44: Observations and Descriptions, at http://www.maa.clell.de/Messier/Mdes/dm044.html.
  4. ↑ a b Klein-Wassink WJ. (1927) The proper motion and the distance of the Praesepe cluster. Publications of the Kapteyn Astronomical Laboratory Groningen, 41: 1-48.
  5. ↑ a b c Dobbie PD, Napiwotzki R, Burleigh MR, et al. (2006) New Praesepe white dwarfs and the initial mass-final mass relation. Monthly Notices of the Royal Astronomical Society, 369: 383-389.
  6. ↑ Pinfield DJ, Dobbie PD, Jameson F, Steele IA, Jones HRA, Katsiyannis AC. (2003) Brown dwarfs and low-mass stars in the Pleiades and Praesepe: Membership and binarity. Monthly Notices of the Royal Astronomical Society, 342: 1241-1259.
  7. ↑ a b c d e f g h Kraus AL, Hillenbrand LA. (2007) The stellar populations of Praesepe and Coma Berenices. Astronomical Journal, 134: 2340-2352.
  8. ↑ WEBDA at http://www.univie.ac.at/webda/.
  9. ↑ a b c d e Adams JD, Stauffer JR, Skrutskie MF, et al. (2002) Structure of the Praesepe Star Cluster. Astronomical Journal, 124: 1570-1584.
  10. ↑ Perryman M, Brown A, Lebreton Y, Gomez A, Turon C, Cayrel de Strobel G, Mermilliod J, Robichon N, Kovalevsky J, Crifo F. (1998) The Hyades: Distance, structure, dynamics, and age. Astronomy & Astrophysics, 331: 81-120.
  11. ↑ Frommert, Hartmut (1998). "Messier Questions & Answers". Retrieved March 1, 2005.
  12. ↑ M44, Students for the Exploration and Development of Space, February 6, 2005.
  13. ↑ Portegies Zwart SF, McMillan SL, Hut P, Makino J. (2001) Star cluster ecology IV. Dissection of an open star cluster: Photometry. Monthly Notices of the Royal Astronomical Society, 321: 199-226.
  14. ↑ Abt HA, Willmarth DW. (1999) Binaries in the Praesepe and Coma star clusters and their implications for binary evolution. Astrophysical Journal, 521: 682-690.
  15. ↑ Gonzalez-Garcia BM, Zapatero Osorio MR, Bejar VJS, Bihain G, Barrado y Navascues D, Caballero JA, Morales-Calderon M. (2006) A search for substellar members in the Praesepe and Sigma Orionis clusters. Astronomy & Astrophysics, 460: 799-810.
 

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