Sub-Alfvenic Non-Ideal Magnetohydrodynamic Turbulence Simulations with Ambipolar Diffusion. III. Implications for Observations and Turbulent Enhancement

Li, Pak Shing; McKee, Christopher F.; Klein, Richard I.

doi:10.1088/0004-637x/744/1/73

Sub-Alfvenic Non-Ideal Magnetohydrodynamic Turbulence Simulations with Ambipolar Diffusion. III. Implications for Observations and Turbulent Enhancement

Journal Article · Wed Dec 14 00:00:00 EST 2011 · The Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637x/744/1/73· OSTI ID:2301829

Li, Pak Shing ^[1]; McKee, Christopher F. ^[1]; Klein, Richard I. ^[2]

Univ. of California, Berkeley, CA (United States)
Univ. of California, Berkeley, CA (United States); Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Ambipolar diffusion (AD) is believed to be a crucial process for redistributing magnetic flux in the dense molecular gas that occurs in regions of star formation. In this work, we carry out numerical simulations of this process in regions of low ionization using the heavy-ion approximation. The simulations are for regions of strong field (plasma β = 0.1) and mildly supersonic turbulence ($$\mathcal{M} = 3$$, corresponding to an Alfvén Mach number of 0.67). The velocity power spectrum of the neutral gas changes from an Iroshnikov–Kraichnan spectrum in the case of ideal MHD to a Burgers spectrum in the case of a shock-dominated hydrodynamic system. The magnetic power spectrum shows a similar behavior. We use a one-dimensional radiative transfer code to post-process our simulation results; the simulated emission from the CS J = 2–1 and H¹³CO⁺ J = 1–0 lines shows that the effects of AD are observable in principle. Linewidths of ions are observed to be less than those of neutrals, and we confirm previous suggestions that this is due to AD. We show that AD is unlikely to affect the Chandrasekhar–Fermi method for inferring field strengths unless the AD is stronger than generally observed. Finally, we present a study of the enhancement of AD by turbulence, finding that AD is accelerated by factor 2–4.5 for non-self-gravitating systems with the level of turbulence we consider.

View Accepted Manuscript (DOE)

Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Organization:: National Aeronautics and Space Administration (NASA); National Center of Supercomputing Application; National Science Foundation (NSF); USDOE National Nuclear Security Administration (NNSA)

Grant/Contract Number:: AC52-07NA27344

OSTI ID:: 2301829

Alternate ID(s):: OSTI ID: 22004311

Report Number(s):: LLNL--JRNL-502272; 518830

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 1 Vol. 744; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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