Zooming in on Individual Star Formation: Low- and High-Mass Stars
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Zooming in on Individual Star Formation: Low- and High-Mass Stars Anna L. Rosen1 · Stella S.R. Offner2 · Sarah I. Sadavoy3 · Asmita Bhandare4 · Enrique Vázquez-Semadeni5 · Adam Ginsburg6
Received: 31 January 2020 / Accepted: 11 May 2020 © Springer Nature B.V. 2020
Abstract Star formation is a multi-scale, multi-physics problem ranging from the size scale of molecular clouds (∼10s pc) down to the size scales of dense prestellar cores (∼0.1 pc) that are the birth sites of stars. Several physical processes like turbulence, magnetic fields and stellar feedback, such as radiation pressure and outflows, are more or less important for different stellar masses and size scales. During the last decade a variety of technological and computing advances have transformed our understanding of star formation through the use of multi-wavelength observations, large scale observational surveys, and multi-physics multi-dimensional numerical simulations. Additionally, the use of synthetic observations of simulations have provided a useful tool to interpret observational data and evaluate the importance of various physical processes on different scales in star formation. Here, we review these recent advancements in both high- (M 8 M ) and low-mass star formation. Keywords Star formation · ISM · High-mass stars · Low-mass stars · Stellar feedback · Numerical methods · Synthetic observations
Star Formation Edited by Andrei Bykov, Corinne Charbonnel, Patrick Hennebelle, Alexandre Marcowith, Georges Meynet, Maurizio Falanga and Rudolf von Steiger
B A.L. Rosen
[email protected]
1
Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA
2
The University of Texas at Austin, Austin, TX 78712, USA
3
Queen’s University, Kingston, ON, K7L 3N6, Canada
4
Max-Planck-Institut fur Astronomie, Konigstuhl 17, 69177 Heidelberg, Germany
5
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, México
6
University of Florida, Gainesville, FL 32611, USA
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A.L. Rosen et al.
1 Introduction Star formation is a multi-scale process that occurs in large (L ∼10 pc), dense (n 103 cm−3 ), and cold (T ∼ 10 K) giant molecular clouds (GMCs) that have a predominantly hierarchical structure with increasing densities toward smaller scales that are the birth sites of stars. Stars span a large range of masses from ∼0.08 M marking the maximum mass of brown dwarfs (i.e., the minimum mass required for core deuterium burning) to ∼200 M , the maximum stellar mass either set by stellar feedback – the injection of energy and momentum by young stars into the interstellar medium (ISM) – or instability i.e., exploding via a pulsational pairinstability supernova once a maximum mass is reached (Woosley 2017; Schneider et al. 2018). Typically, high-mass and low-mass stars are separated at the mass at which stellar death results in supernovae (SNe) explosions. For simplicity, we will refer to low-mass stars as stellar products that are of insufficient
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