NGC 2244: Difference between revisions

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The age of this cluster has been estimated to be less than 5 million years. The brightest star in the cluster is [[12 Monocerotis]], a foreground K-class [[giant star|giant]]. The two brightest members of the cluster are [[HD 46223]] of spectral class [[O-type main-sequence star|O4V]], 400,000 times brighter than the Sun, and approximately 50 times more massive, and [[HD 46150]], whose spectral type is O5V, has a luminosity 450,000 time larger than that of our star, and is up to 60 times more massive, but it may actually be a [[double star]].<ref name=Martins2012>A quantitative study of O stars in NGC 2244 and the Monoceros OB2 association, Martins, F.; Mahy, L.; Hillier, D. J.; Rauw, G., ''Astronomy and Astrophysics'' '''538''', pp. A39, {{bibcode|2012A&A...538A..39M}}, {{doi|10.1051/0004-6361/201117458}}.</ref>
The age of this cluster has been estimated to be less than 5 million years. The brightest star in the cluster is [[12 Monocerotis]], a foreground K-class [[giant star|giant]]. The two brightest members of the cluster are [[HD 46223]] of spectral class [[O-type main-sequence star|O4V]], 400,000 times brighter than the Sun, and approximately 50 times more massive, and [[HD 46150]], whose spectral type is O5V, has a luminosity 450,000 time larger than that of our star, and is up to 60 times more massive, but it may actually be a [[double star]].<ref name=Martins2012>A quantitative study of O stars in NGC 2244 and the Monoceros OB2 association, Martins, F.; Mahy, L.; Hillier, D. J.; Rauw, G., ''Astronomy and Astrophysics'' '''538''', pp. A39, {{bibcode|2012A&A...538A..39M}}, {{doi|10.1051/0004-6361/201117458}}.</ref>


A study from 2023 found that [[Brown dwarf|brown dwarfs]] in NGC 2244 form closer to OB-stars than to other stars.<ref name=":0">{{Cite journal |last=Almendros-Abad |first=V. |last2=Mužić |first2=K. |last3=Bouy |first3=H. |last4=Bayo |first4=A. |last5=Scholz |first5=A. |last6=Peña Ramírez |first6=K. |last7=Moitinho |first7=A. |last8=Kubiak |first8=K. |last9=Schöedel |first9=R. |last10=Barač |first10=R. |last11=Brčić |first11=P. |last12=Ascenso |first12=J. |last13=Jayawardhana |first13=R. |date=2023-05-01 |title=Spectroscopic substellar initial mass function of NGC 2244 |url=https://ui.adsabs.harvard.edu/abs/2023arXiv230507158A}}</ref> This could be explained by the [[photoevaporation]] of the outer layers of [[Pre-stellar core|prestellar cores]] that otherwise would form low-mass stars or intermediate mass stars.<ref>{{Cite journal |last=Whitworth |first=A. P. |last2=Zinnecker |first2=H. |date=2004-11-01 |title=The formation of free-floating brown dwarves and planetary-mass objects by photo-erosion of prestellar cores |url=https://ui.adsabs.harvard.edu/abs/2004A&A...427..299W |journal=Astronomy and Astrophysics |volume=427 |pages=299–306 |doi=10.1051/0004-6361:20041131 |issn=0004-6361}}</ref> The study also found a low disk fraction for low-mass objects of 39±9% for objects later than [[K-type main-sequence star|K0]].<ref name=":0" /> One cluster member was discovered in the past to show signs of an eroding disk, reminiscent of a [[proplyd]].<ref>{{Cite journal |last=Balog |first=Zoltan |last2=Rieke |first2=G. H. |last3=Su |first3=Kate Y. L. |last4=Muzerolle |first4=James |last5=Young |first5=Erick T. |date=2006-10-01 |title=Spitzer MIPS 24 μm Detection of Photoevaporating Protoplanetary Disks |url=https://ui.adsabs.harvard.edu/abs/2006ApJ...650L..83B |journal=The Astrophysical Journal |volume=650 |pages=L83–L86 |doi=10.1086/508707 |issn=0004-637X}}</ref>
A study from 2023 found that [[Brown dwarf|brown dwarfs]] in NGC 2244 form closer to OB-stars than to other stars.<ref name="Almendros-Abad">{{Cite journal |last=Almendros-Abad |first=V. |last2=Mužić |first2=K. |last3=Bouy |first3=H. |last4=Bayo |first4=A. |last5=Scholz |first5=A. |last6=Peña Ramírez |first6=K. |last7=Moitinho |first7=A. |last8=Kubiak |first8=K. |last9=Schöedel |first9=R. |last10=Barač |first10=R. |last11=Brčić |first11=P. |last12=Ascenso |first12=J. |last13=Jayawardhana |first13=R. |date=2023-05-01 |title=Spectroscopic substellar initial mass function of NGC 2244 |url=https://ui.adsabs.harvard.edu/abs/2023arXiv230507158A}}</ref> This could be explained by the [[photoevaporation]] of the outer layers of [[Pre-stellar core|prestellar cores]] that otherwise would form low-mass stars or intermediate mass stars.<ref>{{Cite journal |last=Whitworth |first=A. P. |last2=Zinnecker |first2=H. |date=2004-11-01 |title=The formation of free-floating brown dwarves and planetary-mass objects by photo-erosion of prestellar cores |url=https://ui.adsabs.harvard.edu/abs/2004A&A...427..299W |journal=Astronomy and Astrophysics |volume=427 |pages=299–306 |doi=10.1051/0004-6361:20041131 |issn=0004-6361}}</ref> The study also found a low disk fraction for low-mass objects of 39±9% for objects later than [[K-type main-sequence star|K0]].<ref name="Almendros-Abad" /> One cluster member was discovered in the past to show signs of an eroding disk, reminiscent of a [[proplyd]].<ref>{{Cite journal |last=Balog |first=Zoltan |last2=Rieke |first2=G. H. |last3=Su |first3=Kate Y. L. |last4=Muzerolle |first4=James |last5=Young |first5=Erick T. |date=2006-10-01 |title=Spitzer MIPS 24 μm Detection of Photoevaporating Protoplanetary Disks |url=https://ui.adsabs.harvard.edu/abs/2006ApJ...650L..83B |journal=The Astrophysical Journal |volume=650 |pages=L83–L86 |doi=10.1086/508707 |issn=0004-637X}}</ref>


==References==
==References==

Revision as of 14:21, 15 May 2023

Monoceros
See also: Open cluster, List of open clusters
An infrared Spitzer Space Telescope (SIRT) image of NGC 2244.
Credit: SIRT/NASA

NGC 2244 (also known as Caldwell 50 or the Satellite Cluster) is an

Monoceros. This cluster has several O-type stars, super hot stars that generate large amounts of radiation and stellar wind
.

The age of this cluster has been estimated to be less than 5 million years. The brightest star in the cluster is

HD 46150, whose spectral type is O5V, has a luminosity 450,000 time larger than that of our star, and is up to 60 times more massive, but it may actually be a double star.[5]

A study from 2023 found that brown dwarfs in NGC 2244 form closer to OB-stars than to other stars.[6] This could be explained by the photoevaporation of the outer layers of prestellar cores that otherwise would form low-mass stars or intermediate mass stars.[7] The study also found a low disk fraction for low-mass objects of 39±9% for objects later than K0.[6] One cluster member was discovered in the past to show signs of an eroding disk, reminiscent of a proplyd.[8]

References

  1. ^ a b c "NGC 2244". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2007-04-20.
  2. ^ distance × sin( angular diameter / 2 )
  3. ^ "The Rosette Nebula In Hubble Palette". Sky & Telescope. Retrieved 2020-06-23.
  4. ^ "Notes on the NGC objects, particularly those missing, misidentified, or otherwise unusual (ngcnotes.all)". Historically-aware NGC/IC Positions and Notes. Retrieved 2019-08-11.
  5. doi:10.1051/0004-6361/201117458
    .
  6. ^ a b Almendros-Abad, V.; Mužić, K.; Bouy, H.; Bayo, A.; Scholz, A.; Peña Ramírez, K.; Moitinho, A.; Kubiak, K.; Schöedel, R.; Barač, R.; Brčić, P.; Ascenso, J.; Jayawardhana, R. (2023-05-01). "Spectroscopic substellar initial mass function of NGC 2244". {{cite journal}}: Cite journal requires |journal= (help)
  7. ISSN 0004-6361
    .
  8. ISSN 0004-637X
    .

External links
Retrieved from "https://en.wikipedia.org/w/index.php?title=NGC_2244&oldid=1154918589"