University of Hertfordshire

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By the same authors

The Physics of Star Cluster Formation and Evolution

Research output: Contribution to journalArticlepeer-review

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The Physics of Star Cluster Formation and Evolution. / Krause, Martin G. H.; Offner, Stella S. R.; Charbonnel, Corinne; Gieles, Mark; Klessen, Ralf S.; Vazquez-Semadeni, Enrique; Ballesteros-Paredes, Javier; Girichidis, Philipp; Kruijssen, J. M. Diederik; Ward, Jacob L.; Zinnecker, Hans.

In: Space Science Reviews, Vol. 216, 64, 02.06.2020.

Research output: Contribution to journalArticlepeer-review

Harvard

Krause, MGH, Offner, SSR, Charbonnel, C, Gieles, M, Klessen, RS, Vazquez-Semadeni, E, Ballesteros-Paredes, J, Girichidis, P, Kruijssen, JMD, Ward, JL & Zinnecker, H 2020, 'The Physics of Star Cluster Formation and Evolution', Space Science Reviews, vol. 216, 64. https://doi.org/10.1007/s11214-020-00689-4

APA

Krause, M. G. H., Offner, S. S. R., Charbonnel, C., Gieles, M., Klessen, R. S., Vazquez-Semadeni, E., Ballesteros-Paredes, J., Girichidis, P., Kruijssen, J. M. D., Ward, J. L., & Zinnecker, H. (2020). The Physics of Star Cluster Formation and Evolution. Space Science Reviews, 216, [64]. https://doi.org/10.1007/s11214-020-00689-4

Vancouver

Krause MGH, Offner SSR, Charbonnel C, Gieles M, Klessen RS, Vazquez-Semadeni E et al. The Physics of Star Cluster Formation and Evolution. Space Science Reviews. 2020 Jun 2;216. 64. https://doi.org/10.1007/s11214-020-00689-4

Author

Krause, Martin G. H. ; Offner, Stella S. R. ; Charbonnel, Corinne ; Gieles, Mark ; Klessen, Ralf S. ; Vazquez-Semadeni, Enrique ; Ballesteros-Paredes, Javier ; Girichidis, Philipp ; Kruijssen, J. M. Diederik ; Ward, Jacob L. ; Zinnecker, Hans. / The Physics of Star Cluster Formation and Evolution. In: Space Science Reviews. 2020 ; Vol. 216.

Bibtex

@article{e46ed760d9424431abad5d728582b94f,
title = "The Physics of Star Cluster Formation and Evolution",
abstract = "Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work. ",
keywords = "astro-ph.GA, astro-ph.SR",
author = "Krause, {Martin G. H.} and Offner, {Stella S. R.} and Corinne Charbonnel and Mark Gieles and Klessen, {Ralf S.} and Enrique Vazquez-Semadeni and Javier Ballesteros-Paredes and Philipp Girichidis and Kruijssen, {J. M. Diederik} and Ward, {Jacob L.} and Hans Zinnecker",
note = "{\textcopyright} 2020 Springer-Verlag. The final publication is available at Springer via https://doi.org/10.1007/s11214-020-00689-4.",
year = "2020",
month = jun,
day = "2",
doi = "10.1007/s11214-020-00689-4",
language = "English",
volume = "216",
journal = "Space Science Reviews",
issn = "0038-6308",
publisher = "Springer Netherlands",

}

RIS

TY - JOUR

T1 - The Physics of Star Cluster Formation and Evolution

AU - Krause, Martin G. H.

AU - Offner, Stella S. R.

AU - Charbonnel, Corinne

AU - Gieles, Mark

AU - Klessen, Ralf S.

AU - Vazquez-Semadeni, Enrique

AU - Ballesteros-Paredes, Javier

AU - Girichidis, Philipp

AU - Kruijssen, J. M. Diederik

AU - Ward, Jacob L.

AU - Zinnecker, Hans

N1 - © 2020 Springer-Verlag. The final publication is available at Springer via https://doi.org/10.1007/s11214-020-00689-4.

PY - 2020/6/2

Y1 - 2020/6/2

N2 - Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.

AB - Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.

KW - astro-ph.GA

KW - astro-ph.SR

U2 - 10.1007/s11214-020-00689-4

DO - 10.1007/s11214-020-00689-4

M3 - Article

VL - 216

JO - Space Science Reviews

JF - Space Science Reviews

SN - 0038-6308

M1 - 64

ER -