Mass and Magnetic distributions in Self Gravitating Super Alfvenic Turbulence with AMR

TL;DR

This paper analyzes the mass and magnetic field distributions in self-gravitating, super-Alfvénic turbulence using AMR MHD simulations, revealing power-law behaviors and agreement with observational data.

Contribution

It presents novel simulation results showing power-law distributions in density and magnetic fields, aligning with recent observations of prestellar cores.

Findings

Power-law tails in density and magnetic field PDFs.

Magnetic field strength scales with density as B∝ρ^0.48.

Mass distribution of cores matches observational data.

Abstract

In this work, we present the mass and magnetic distributions found in a recent Adaptive Mesh Refinement (AMR) MHD simulation of supersonic, \sa, self gravitating turbulence. Powerlaw tails are found in both volume density and magnetic field probability density functions, with $P(\rho) \propto \rho^{-1.67}$ and $P(B)\propto B^{-2.74}$. A power law is also found between magnetic field strength and density, with $B\propto \rho^{0.48}$, throughout the collapsing gas. The mass distribution of gravitationally bound cores is shown to be in excellent agreement with recent observation of prestellar cores. The mass to flux distribution of cores is also found to be in excellent agreement with recent Zeeman splitting measurements.