Protostellar collapse and fragmentation using an MHD gadget

Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been performed on this subject within the smoothed particle hydrodynamics method. This is largely due to the unsatisfactory treatment of non-vanishing...

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Published in	Monthly notices of the Royal Astronomical Society Vol. 412; no. 1; pp. 171 - 186
Main Authors	Bürzle, Florian, Clark, Paul C., Stasyszyn, Federico, Greif, Thomas, Dolag, Klaus, Klessen, Ralf S., Nielaba, Peter
Format	Journal Article
Language	English
Published	Oxford, UK Blackwell Publishing Ltd 01.03.2011 Wiley-Blackwell Oxford University Press
Subjects	Astronomy Earth, ocean, space Exact sciences and technology ISM: clouds ISM: magnetic fields Magnetic fields MHD Star & galaxy formation Stars & galaxies stars: formation MHD stars: formation ISM: clouds magnetic fields ISM: magnetic fields Collapse Induction equation Magnetohydrodynamics Digital simulation Smoothed particle hydrodynamics method Rotation axis Fragmentation Protostars Case study Regularization method Divergences MHD model Star formation Particle code High field Magnetic fields
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Abstract	Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been performed on this subject within the smoothed particle hydrodynamics method. This is largely due to the unsatisfactory treatment of non-vanishing divergence of the magnetic field. Recently smoothed particle magnetohydrodynamics (SPMHD) simulations based on Euler potentials have proven to be successful in treating MHD collapse and fragmentation problems, however these methods are known to have some intrinsic difficulties. We have performed SPMHD simulations based on a traditional approach evolving the magnetic field itself using the induction equation. To account for the numerical divergence, we have chosen an approach that subtracts the effects of numerical divergence from the force equation, and additionally we employ artificial magnetic dissipation as a regularization scheme. We apply this realization of SPMHD to a widely known setup, a variation of the 'Boss and Bodenheimer standard isothermal test case', to study the impact of the magnetic fields on collapse and fragmentation. In our simulations, we concentrate on setups, where the initial magnetic field is parallel to the rotation axis. We examine different field strengths and compare our results to other findings reported in the literature. We are able to confirm specific results found elsewhere, namely the delayed onset of star formation for strong fields, accompanied by the tendency to form only single stars. We also find that the 'magnetic cushioning effect', where the magnetic field is wound up to form a 'cushion' between the binary, aids binary fragmentation in a case where previously only formation of a single protostar was expected.
AbstractList	Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been performed on this subject within the smoothed particle hydrodynamics method. This is largely due to the unsatisfactory treatment of non-vanishing divergence of the magnetic field. Recently smoothed particle magnetohydrodynamics (SPMHD) simulations based on Euler potentials have proven to be successful in treating MHD collapse and fragmentation problems, however these methods are known to have some intrinsic difficulties. We have performed SPMHD simulations based on a traditional approach evolving the magnetic field itself using the induction equation. To account for the numerical divergence, we have chosen an approach that subtracts the effects of numerical divergence from the force equation, and additionally we employ artificial magnetic dissipation as a regularization scheme. We apply this realization of SPMHD to a widely known setup, a variation of the 'Boss and Bodenheimer standard isothermal test case', to study the impact of the magnetic fields on collapse and fragmentation. In our simulations, we concentrate on setups, where the initial magnetic field is parallel to the rotation axis. We examine different field strengths and compare our results to other findings reported in the literature. We are able to confirm specific results found elsewhere, namely the delayed onset of star formation for strong fields, accompanied by the tendency to form only single stars. We also find that the 'magnetic cushioning effect', where the magnetic field is wound up to form a 'cushion' between the binary, aids binary fragmentation in a case where previously only formation of a single protostar was expected. ABSTRACT Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been performed on this subject within the smoothed particle hydrodynamics method. This is largely due to the unsatisfactory treatment of non-vanishing divergence of the magnetic field. Recently smoothed particle magnetohydrodynamics (SPMHD) simulations based on Euler potentials have proven to be successful in treating MHD collapse and fragmentation problems, however these methods are known to have some intrinsic difficulties. We have performed SPMHD simulations based on a traditional approach evolving the magnetic field itself using the induction equation. To account for the numerical divergence, we have chosen an approach that subtracts the effects of numerical divergence from the force equation, and additionally we employ artificial magnetic dissipation as a regularization scheme. We apply this realization of SPMHD to a widely known setup, a variation of the 'Boss and Bodenheimer standard isothermal test case', to study the impact of the magnetic fields on collapse and fragmentation. In our simulations, we concentrate on setups, where the initial magnetic field is parallel to the rotation axis. We examine different field strengths and compare our results to other findings reported in the literature. We are able to confirm specific results found elsewhere, namely the delayed onset of star formation for strong fields, accompanied by the tendency to form only single stars. We also find that the 'magnetic cushioning effect', where the magnetic field is wound up to form a 'cushion' between the binary, aids binary fragmentation in a case where previously only formation of a single protostar was expected. [PUBLICATION ABSTRACT] ABSTRACT Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been performed on this subject within the smoothed particle hydrodynamics method. This is largely due to the unsatisfactory treatment of non‐vanishing divergence of the magnetic field. Recently smoothed particle magnetohydrodynamics (SPMHD) simulations based on Euler potentials have proven to be successful in treating MHD collapse and fragmentation problems, however these methods are known to have some intrinsic difficulties. We have performed SPMHD simulations based on a traditional approach evolving the magnetic field itself using the induction equation. To account for the numerical divergence, we have chosen an approach that subtracts the effects of numerical divergence from the force equation, and additionally we employ artificial magnetic dissipation as a regularization scheme. We apply this realization of SPMHD to a widely known setup, a variation of the ‘Boss and Bodenheimer standard isothermal test case’, to study the impact of the magnetic fields on collapse and fragmentation. In our simulations, we concentrate on setups, where the initial magnetic field is parallel to the rotation axis. We examine different field strengths and compare our results to other findings reported in the literature. We are able to confirm specific results found elsewhere, namely the delayed onset of star formation for strong fields, accompanied by the tendency to form only single stars. We also find that the ‘magnetic cushioning effect’, where the magnetic field is wound up to form a ‘cushion’ between the binary, aids binary fragmentation in a case where previously only formation of a single protostar was expected.
Author	Clark, Paul C. Nielaba, Peter Stasyszyn, Federico Bürzle, Florian Greif, Thomas Dolag, Klaus Klessen, Ralf S.
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Keywords	MHD stars: formation ISM: clouds magnetic fields ISM: magnetic fields Collapse Induction equation Magnetohydrodynamics Digital simulation Smoothed particle hydrodynamics method Rotation axis Fragmentation Protostars Case study Regularization method Divergences MHD model Star formation Particle code High field Magnetic fields
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Snippet	Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have been... ABSTRACT Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have... ABSTRACT Although the influence of magnetic fields is regarded as vital in the star formation process, only a few magnetohydrodynamics (MHD) simulations have...
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SubjectTerms	Astronomy Earth, ocean, space Exact sciences and technology ISM: clouds ISM: magnetic fields Magnetic fields MHD Star & galaxy formation Stars & galaxies stars: formation
Title	Protostellar collapse and fragmentation using an MHD gadget
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