The authors show that intensity gradients from thick velocity channel maps trace magnetic fields, shocks, and self-gravitating regions in diffuse interstellar gas, though with lower accuracy than velocity gradients.
On the formation of density filaments in the turbulent interstellar medium
1 Pith paper cite this work. Polarity classification is still indexing.
1
Pith paper citing it
abstract
This study is motivated by recent observations on ubiquitous interstellar density filaments and guided by modern theories of compressible magnetohydrodynamic (MHD) turbulence. The interstellar turbulence shapes the observed density structures. As the fundamental dynamics of compressible MHD turbulence, perpendicular turbulent mixing of density fluctuations entails elongated density structures aligned with the local magnetic field, accounting for low-density parallel filaments seen in diffuse atomic and molecular gas. The elongation of low-density parallel filaments depends on the turbulence anisotropy. When taking into account the partial ionization, we find that the minimum width of parallel filaments in the cold neutral medium and molecular clouds is determined by the neutral-ion decoupling scale perpendicular to magnetic field. In highly supersonic MHD turbulence in molecular clouds, both low-density parallel filaments due to anisotropic turbulent mixing and high-density filaments due to shock compression exist.
fields
astro-ph.GA 1years
2019 1verdicts
CONDITIONAL 1representative citing papers
citing papers explorer
-
Intensity Gradients Technique: Synergy with Velocity Gradients and Polarization Studies
The authors show that intensity gradients from thick velocity channel maps trace magnetic fields, shocks, and self-gravitating regions in diffuse interstellar gas, though with lower accuracy than velocity gradients.