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Title: Modeling jet and outflow feedback during star cluster formation

Abstract

Powerful jets and outflows are launched from the protostellar disks around newborn stars. These outflows carry enough mass and momentum to transform the structure of their parent molecular cloud and to potentially control star formation itself. Despite their importance, we have not been able to fully quantify the impact of jets and outflows during the formation of a star cluster. The main problem lies in limited computing power. We would have to resolve the magnetic jet-launching mechanism close to the protostar and at the same time follow the evolution of a parsec-size cloud for a million years. Current computer power and codes fall orders of magnitude short of achieving this. In order to overcome this problem, we implement a subgrid-scale (SGS) model for launching jets and outflows, which demonstrably converges and reproduces the mass, linear and angular momentum transfer, and the speed of real jets, with ∼1000 times lower resolution than would be required without the SGS model. We apply the new SGS model to turbulent, magnetized star cluster formation and show that jets and outflows (1) eject about one-fourth of their parent molecular clump in high-speed jets, quickly reaching distances of more than a parsec, (2) reduce the starmore » formation rate by about a factor of two, and (3) lead to the formation of ∼1.5 times as many stars compared to the no-outflow case. Most importantly, we find that jets and outflows reduce the average star mass by a factor of ∼ three and may thus be essential for understanding the characteristic mass of the stellar initial mass function.« less

Authors:
 [1];  [2];  [3];  [4]
  1. Monash Centre for Astrophysics, School of Mathematical Sciences, Monash University, VIC 3800 (Australia)
  2. Department of Computational Hydrosystems, Helmholtz Centre for Environmental Research-UFZ, Permoserstr. 15, D-04318 Leipzig (Germany)
  3. Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg (Germany)
  4. Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Strasse 2, D-69120 Heidelberg (Germany)
Publication Date:
OSTI Identifier:
22365490
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 790; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANGULAR MOMENTUM TRANSFER; COMPARATIVE EVALUATIONS; DISTANCE; LAUNCHING; LUMINOSITY; MAGNETOHYDRODYNAMICS; MASS; RESOLUTION; SIMULATION; STAR CLUSTERS; STAR EVOLUTION; STARS; TURBULENCE

Citation Formats

Federrath, Christoph, Schrön, Martin, Banerjee, Robi, and Klessen, Ralf S., E-mail: christoph.federrath@monash.edu. Modeling jet and outflow feedback during star cluster formation. United States: N. p., 2014. Web. doi:10.1088/0004-637X/790/2/128.
Federrath, Christoph, Schrön, Martin, Banerjee, Robi, & Klessen, Ralf S., E-mail: christoph.federrath@monash.edu. Modeling jet and outflow feedback during star cluster formation. United States. doi:10.1088/0004-637X/790/2/128.
Federrath, Christoph, Schrön, Martin, Banerjee, Robi, and Klessen, Ralf S., E-mail: christoph.federrath@monash.edu. Fri . "Modeling jet and outflow feedback during star cluster formation". United States. doi:10.1088/0004-637X/790/2/128.
@article{osti_22365490,
title = {Modeling jet and outflow feedback during star cluster formation},
author = {Federrath, Christoph and Schrön, Martin and Banerjee, Robi and Klessen, Ralf S., E-mail: christoph.federrath@monash.edu},
abstractNote = {Powerful jets and outflows are launched from the protostellar disks around newborn stars. These outflows carry enough mass and momentum to transform the structure of their parent molecular cloud and to potentially control star formation itself. Despite their importance, we have not been able to fully quantify the impact of jets and outflows during the formation of a star cluster. The main problem lies in limited computing power. We would have to resolve the magnetic jet-launching mechanism close to the protostar and at the same time follow the evolution of a parsec-size cloud for a million years. Current computer power and codes fall orders of magnitude short of achieving this. In order to overcome this problem, we implement a subgrid-scale (SGS) model for launching jets and outflows, which demonstrably converges and reproduces the mass, linear and angular momentum transfer, and the speed of real jets, with ∼1000 times lower resolution than would be required without the SGS model. We apply the new SGS model to turbulent, magnetized star cluster formation and show that jets and outflows (1) eject about one-fourth of their parent molecular clump in high-speed jets, quickly reaching distances of more than a parsec, (2) reduce the star formation rate by about a factor of two, and (3) lead to the formation of ∼1.5 times as many stars compared to the no-outflow case. Most importantly, we find that jets and outflows reduce the average star mass by a factor of ∼ three and may thus be essential for understanding the characteristic mass of the stellar initial mass function.},
doi = {10.1088/0004-637X/790/2/128},
journal = {Astrophysical Journal},
number = 2,
volume = 790,
place = {United States},
year = {Fri Aug 01 00:00:00 EDT 2014},
month = {Fri Aug 01 00:00:00 EDT 2014}
}