The interstellar magnetic field strength and density are observed to be correlated, but there is a large dispersion in this relation. In particular, the magnetic field is often observed to be weaker than expected. It is usually assumed that the field is frozen into the gas except at very high density and low ionization fraction, in which case ion-neutral drift, or ambipolar diffusion, leads to ...

Using an isothermal MHD code, we have performed three-dimensional, highresolution simulations of the Parker instability. The initial equilibrium system is composed of exponentially-decreasing isothermal gas and magnetic field (along the azimuthal direction) under a uniform gravity. The evolution of the instability can be divided into three phases: linear, nonlinear, and relaxed. During the line...

The G11.11-0.12 infrared-dark cloud has a filamentary appearance, both in extinction against the diffuse infrared emission of the Galactic plane and in emission at 850μm. We use a novel computational technique based on an advanced genetic algorithm to explore thoroughly 3 different models of self-gravitating, pressure truncated filaments and to constrain their parameters. Specifically, the mode...

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...

Abstract In a seminal paper, Parker showed the vertical stratification of interstellar medium (ISM) is unstable if magnetic fields and cosmic rays provide too large fraction pressure support. Cosmic ray acceleration linked to star formation, so Parker’s instability its nonlinear outcomes are type formation feedback. Numerical simulations have shown can significantly restructure ISM, thinning th...

Magnetic fields and turbulence are important components of the interstellar medium (ISM) star-forming galaxies. It is challenging to measure properties small-scale ISM magnetic (magnetic at scales smaller than driving scale). Using numerical simulations, we demonstrate how second-order rotation (RM, which depends on thermal electron density, $n_{\rm e}$, field, $b$) structure function can probe...

the second somatosensory area (sli) has been studied both by electrical evoked potentials24 and magnetoencephalography (meg)5 magnetic evoked fields of contralateral primary somatosensory and ipsilateral second somatosensory cortices of 12 normal subjects were recorded in response to median nerve electrical stimulation by means of a single magnetometer. we detected. in addition to the usual con...

introduction:  the  use  of  mobile  communication  systems  has  dramatically  increased  over  the  past  decade. although many studies have been performed to determine the effect of radio frequency (rf) but  less attention has been paid to the possible biological impact of exposure to extremely low frequency  (elf) components.   the objective of this study is two folds. one is to design the ...

background: nowadays, magnetic nanoparticles (mnps) have received much attention because of their enormous potentials in many fields such as magnetic fluid hyperthermia (mfh). the goal of hyperthermia is to increase the temperature of malignant cells to destroy them without any lethal effect on normal tissues. to investigate the effectiveness of cancer therapy by magnetic fluid hyperthermia, fe...

The “galactic shocks” (Fujimoto 1968; Roberts 1969) is investigated using a full three-dimensional hydrodynamic simulations, taking into account self-gravity of the ISM, radiative cooling, and star formation followed by energy feedback from supernovae. This is an essential progress from the previous numerical models, in which 2-D isothermal, non-self-gravitating gas is assumed. We find that the...