Jump to content

Super star cluster: Difference between revisions

From Wikipedia, the free encyclopedia
Content deleted Content added
Mgoumas (talk | contribs)
added pictures
Mgoumas (talk | contribs)
added more properties
Line 9: Line 9:
| pages = 207
| pages = 207
| bibcode = 2002IAUS..207..745G
| bibcode = 2002IAUS..207..745G
|arxiv = astro-ph/0109052 }}</ref> They typically contain a very large number of [[T Tauri Star|young]], [[OB star|massive stars]] that ionize a surrounding [[H II region]], similar to the [[Milky Way|Milky Way Galaxy]]'s so-called "Ultra dense H II regions (UDHIIs)".<ref name=kobulnicky99>{{cite journal
|arxiv = astro-ph/0109052 }}</ref> These clusters are referred to as "super" due to the fact that they are relatively much larger, more luminous, and contain more mass than other young star clusters.<ref name=":0">{{Cite journal|last=Johnson|first=Kelsey|year=|title=The Properties of Super Star Clusters In A Sample of Starburst Galaxies|url=https://pdfs.semanticscholar.org/998f/66fe062452fb32657a42a06c4818c2d5dd64.pdf|journal=|volume=|pages=|via=}}</ref> They typically contain a very large number of [[T Tauri Star|young]], [[OB star|massive stars]] that ionize a surrounding [[H II region]], similar to the [[Milky Way|Milky Way Galaxy]]'s so-called "Ultra dense H II regions (UDHIIs)".<ref name=kobulnicky99>{{cite journal
| last = Kobulnicky
| last = Kobulnicky
| first = Henry A.
| first = Henry A.
Line 33: Line 33:
|arxiv = astro-ph/0405125 }}</ref>
|arxiv = astro-ph/0405125 }}</ref>


The Typical characteristics of SSCs:
The unique characteristics of SSCs are their large [[electron]] [[Density|densities]] <math>n_e=10^3</math>–<math>10^6</math> cm<math>^{-3}</math> and [[pressure]]s <math>P/</math>[[Boltzmann's constant|<math>k_b</math>]]<math>=10^7</math>–<math>10^{10}</math> [[Kelvin|K]] cm<math>^{-3}</math>.<ref name=johnson04/>
* large [[electron]] [[Density|densities]] <math>n_e=10^3</math>–<math>10^6</math> cm<math>^{-3}</math>
* [[pressure]]s <math>P/</math>[[Boltzmann's constant|<math>k_b</math>]]<math>=10^7</math>–<math>10^{10}</math> [[Kelvin|K]] cm<math>^{-3}</math>.<ref name="johnson04" />
* Mass <math>\gtrsim</math> 5M<sub>☉</sub><ref name=":0" />
* Radius ≈ 5 pc ≈ <math>1.54^{19}</math> cm<ref name=":0" />
* Age ≈ 100Myr<ref name=":0" />


==List==
==List==
Line 54: Line 59:
|
|
| <ref>{{cite journal|doi=10.1088/0004-637X/780/1/36|title=Molecular Clouds Toward the Super Star Cluster Ngc 3603; Possible Evidence for a Cloud-Cloud Collision in Triggering the Cluster Formation|journal=The Astrophysical Journal|volume=780|pages=36|year=2014|last1=Fukui|first1=Y.|last2=Ohama|first2=A.|last3=Hanaoka|first3=N.|last4=Furukawa|first4=N.|last5=Torii|first5=K.|last6=Dawson|first6=J. R.|last7=Mizuno|first7=N.|last8=Hasegawa|first8=K.|last9=Fukuda|first9=T.|last10=Soga|first10=S.|last11=Moribe|first11=N.|last12=Kuroda|first12=Y.|last13=Hayakawa|first13=T.|last14=Kawamura|first14=A.|last15=Kuwahara|first15=T.|last16=Yamamoto|first16=H.|last17=Okuda|first17=T.|last18=Onishi|first18=T.|last19=Maezawa|first19=H.|last20=Mizuno|first20=A.|bibcode=2014ApJ...780...36F|arxiv = 1306.2090 }}</ref>
| <ref>{{cite journal|doi=10.1088/0004-637X/780/1/36|title=Molecular Clouds Toward the Super Star Cluster Ngc 3603; Possible Evidence for a Cloud-Cloud Collision in Triggering the Cluster Formation|journal=The Astrophysical Journal|volume=780|pages=36|year=2014|last1=Fukui|first1=Y.|last2=Ohama|first2=A.|last3=Hanaoka|first3=N.|last4=Furukawa|first4=N.|last5=Torii|first5=K.|last6=Dawson|first6=J. R.|last7=Mizuno|first7=N.|last8=Hasegawa|first8=K.|last9=Fukuda|first9=T.|last10=Soga|first10=S.|last11=Moribe|first11=N.|last12=Kuroda|first12=Y.|last13=Hayakawa|first13=T.|last14=Kawamura|first14=A.|last15=Kuwahara|first15=T.|last16=Yamamoto|first16=H.|last17=Okuda|first17=T.|last18=Onishi|first18=T.|last19=Maezawa|first19=H.|last20=Mizuno|first20=A.|bibcode=2014ApJ...780...36F|arxiv = 1306.2090 }}</ref>
|[[File:Stellar nursery NGC 3603.jpg|alt=SSC NGC 3603|center|thumb|SSC NGC 3603]]
|[[File:Stellar nursery NGC 3603.jpg|alt=\NGC 3603|center|thumb|NGC 3603]]
|-
|-
| [[R136]]
| [[R136]]
Line 60: Line 65:
| The prototype SSC
| The prototype SSC
| <ref>{{cite journal|doi=10.1086/305126|title=Star Formation in R136: A Cluster of O3 Stars Revealed by ''Hubble'' Space Telescope ''Spectroscopy''|journal=The Astrophysical Journal|volume=493|pages=180|year=1998|last1=Massey|first1=Philip|last2=Hunter|first2=Deidre A.|bibcode=1998ApJ...493..180M}}</ref>
| <ref>{{cite journal|doi=10.1086/305126|title=Star Formation in R136: A Cluster of O3 Stars Revealed by ''Hubble'' Space Telescope ''Spectroscopy''|journal=The Astrophysical Journal|volume=493|pages=180|year=1998|last1=Massey|first1=Philip|last2=Hunter|first2=Deidre A.|bibcode=1998ApJ...493..180M}}</ref>
|[[File:Grand star-forming region R136 in NGC 2070 (captured by the Hubble Space Telescope).jpg|alt=SSC R136 (Located in the Tarantula Nebula)|center|thumb|SSC R136 (Located in the Tarantula Nebula)]]
|[[File:Grand star-forming region R136 in NGC 2070 (captured by the Hubble Space Telescope).jpg|alt=R136 (Located in the Tarantula Nebula)|center|thumb|R136 (Located in the Tarantula Nebula)]]
|-
|-
| NGC 1569 A1 and A2
| NGC 1569 A1 and A2
Line 66: Line 71:
| Galaxy contains two SSCs
| Galaxy contains two SSCs
| <ref>{{cite journal|bibcode=2000AJ....120.2383H|title=The Star Clusters in the Starburst Irregular Galaxy NGC 1569|journal=The Astronomical Journal|volume=120|issue=5|pages=2383|author1=Hunter|first1=Deidre A.|last2=O'Connell|first2=Robert W.|last3=Gallagher|first3=J. S.|last4=Smecker-Hane|first4=Tammy A.|year=2000|doi=10.1086/316810|arxiv = astro-ph/0009280 }}</ref>
| <ref>{{cite journal|bibcode=2000AJ....120.2383H|title=The Star Clusters in the Starburst Irregular Galaxy NGC 1569|journal=The Astronomical Journal|volume=120|issue=5|pages=2383|author1=Hunter|first1=Deidre A.|last2=O'Connell|first2=Robert W.|last3=Gallagher|first3=J. S.|last4=Smecker-Hane|first4=Tammy A.|year=2000|doi=10.1086/316810|arxiv = astro-ph/0009280 }}</ref>
|[[File:Starburst in a Dwarf Irregular Galaxy.jpg|alt=NGC 1569|thumb|NGC 1569]]
|[[File:Starburst in a Dwarf Irregular Galaxy.jpg|alt=NGC 1569|thumb|NGC 1569|center]]
|}
|}
{{expand list|date=February 2011}}
{{expand list|date=February 2011}}

Revision as of 00:28, 27 February 2017

A super star cluster (SSC) is a very massive young open cluster that is thought to be the precursor of a globular cluster.[1] These clusters are referred to as "super" due to the fact that they are relatively much larger, more luminous, and contain more mass than other young star clusters.[2] They typically contain a very large number of young, massive stars that ionize a surrounding H II region, similar to the Milky Way Galaxy's so-called "Ultra dense H II regions (UDHIIs)".[3] An SSC's H II region is in turn surrounded by a cocoon of dust. In many cases, the stars and the H II regions will be invisible to optical observations due to high levels of extinction. As a result, the youngest SSCs are best observed in radio and infrared.[4]

The Typical characteristics of SSCs:

  • large electron densities cm
  • pressures K cm.[4]
  • Mass 5M[2]
  • Radius ≈ 5 pc ≈ cm[2]
  • Age ≈ 100Myr[2]

List

Name Galaxy Comments Notes Pictures
Westerlund 1 (Wd1) Milky Way Galaxy First SSC discovered in the Milky Way Galaxy. [5]
Westerlund 1
Westerlund 1
NGC 3603 Milky Way Galaxy [6]
\NGC 3603
NGC 3603
R136 Large Magellanic Cloud (LMC) The prototype SSC [7]
R136 (Located in the Tarantula Nebula)
R136 (Located in the Tarantula Nebula)
NGC 1569 A1 and A2 NGC 1569 Galaxy contains two SSCs [8]
NGC 1569
NGC 1569

References

  1. ^ Gallagher; Grebel (2002). "Extragalactic Star Clusters: Speculations on the Future". Extragalactic Star Clusters, IAU Symposium. 207: 207. arXiv:astro-ph/0109052. Bibcode:2002IAUS..207..745G. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
  2. ^ a b c d Johnson, Kelsey. "The Properties of Super Star Clusters In A Sample of Starburst Galaxies" (PDF). {{cite journal}}: Cite journal requires |journal= (help)
  3. ^ Kobulnicky, Henry A.; Johnson, Kelsey E. (1999). "Signatures of the Youngest Starbursts: Optically Thick Thermal Bremsstrahlung Radio Sources in Henize 2-10". ApJ. 527 (1): 154–166. arXiv:astro-ph/9907233. Bibcode:1999ApJ...527..154K. doi:10.1086/308075. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
  4. ^ a b Johnson (2004). "Extragalactic Ultracompact HII Regions: Probing the Birth Environments of Super Star Clusters". ASP Conference Series. 527: 322. arXiv:astro-ph/0405125. Bibcode:2004ASPC..322..339J.
  5. ^ Clark, J. S.; Negueruela, I.; Crowther, P. A.; Goodwin, S. P. (2005). "On the massive stellar population of the super star cluster Westerlund 1". Astronomy and Astrophysics. 434 (3): 949. arXiv:astro-ph/0504342. Bibcode:2005A&A...434..949C. doi:10.1051/0004-6361:20042413.
  6. ^ Fukui, Y.; Ohama, A.; Hanaoka, N.; Furukawa, N.; Torii, K.; Dawson, J. R.; Mizuno, N.; Hasegawa, K.; Fukuda, T.; Soga, S.; Moribe, N.; Kuroda, Y.; Hayakawa, T.; Kawamura, A.; Kuwahara, T.; Yamamoto, H.; Okuda, T.; Onishi, T.; Maezawa, H.; Mizuno, A. (2014). "Molecular Clouds Toward the Super Star Cluster Ngc 3603; Possible Evidence for a Cloud-Cloud Collision in Triggering the Cluster Formation". The Astrophysical Journal. 780: 36. arXiv:1306.2090. Bibcode:2014ApJ...780...36F. doi:10.1088/0004-637X/780/1/36.
  7. ^ Massey, Philip; Hunter, Deidre A. (1998). "Star Formation in R136: A Cluster of O3 Stars Revealed by Hubble Space Telescope Spectroscopy". The Astrophysical Journal. 493: 180. Bibcode:1998ApJ...493..180M. doi:10.1086/305126.
  8. ^ Hunter, Deidre A.; O'Connell, Robert W.; Gallagher, J. S.; Smecker-Hane, Tammy A. (2000). "The Star Clusters in the Starburst Irregular Galaxy NGC 1569". The Astronomical Journal. 120 (5): 2383. arXiv:astro-ph/0009280. Bibcode:2000AJ....120.2383H. doi:10.1086/316810.