We investigate the effects of magnetic field configurations on ionization rate by cosmic rays in protoplanetary disks. First, we consider cosmic-ray propagation from interstellar medium (ISM) to disks and showed that density around disk should be 2 times lower than ISM value. Then, compute attenuation The fields are stretched azimuthal directions, need detour while propagating midplane. Our res...

The temperature structure of protoplanetary disks provides an important constraint on where in the rocky planets like our own form. Recent nonideal magnetohydrodynamical (MHD) simulations have shown that internal Joule heating associated with magnetically driven disk accretion is inefficient at midplane. A model based MHD predicts a around solar-mass young star, water snow line can move inside ...

Recent observations indicate that mm/cm-sized grains may exist in the embedded protostellar disks. How such large grow from micron size (or less) earliest phase of star formation remains relatively unexplored. In this study we take a first step to model grain growth environment, using two-dimensional (2D axisymmetric) radiation hydrodynamic and simulations. We show calculations can be greatly s...

Received ; accepted – 2 – ABSTRACT Supernova explosions, and winds and energetic photon fluxes from young star clusters drive outflows and supersonic turbulence in the interstellar medium in galaxy disks, and provide broad spectrum heating which generates a wide range of thermal phases in the gas. Star formation, the source of the energy inputs, is itself regulated by heating and phase exchange...

Activity of the nuclei of galaxies and stellar mass systems involving disk accretion to black holes is thought to be due to (1) a small-scale turbulent magnetic field in the disk (due to the magneto-rotational instability or MRI) which gives a large viscosity enhancing accretion, and (2) a large-scale magnetic field which gives rise to matter outflows and/or electromagnetic jets from the disk w...

Abstract Recently, a collision-induced magnetic reconnection (CMR) mechanism was proposed to explain dense filament formation in the Orion A giant molecular cloud. natural question is whether CMR works elsewhere Galaxy. As an initial attempt answer question, this paper investigates triggering of and production gas flat-rotating disk with modified Bisymmetric spiral (BSS) field. Cloud−cloud coll...

We carried out 3D dust+gas radiative hydrodynamic simulations of forming planets. investigated a parameter grid Neptune-, Saturn-, Jupiter-, and 5 Jupiter-mass planets at 5.2, 30, 50 AU distance from their star. found that the meridional circulation \citep{Szulagyi14,FC16} drives strong vertical flow for dust as well, hence is not settled in midplane, even mm-sized grains. The will deliver gas ...