Abstract Observations of the magnetic field B in very local interstellar medium (VLISM) were made by Voyager 1 (V1) northern hemisphere from 2012 to mid-2021 and 2 (V2) southern 2018 through 2020. Near 2019.4, V2 observed an abrupt increase associated with a pressure front near heliopause. During 2020, at jump that was preceded electron plasma oscillations cosmic rays, indicating it shock. The ...

We present a study of the kinetic energy dissipation in interstellar cloud collisions. The main aim is to understand the dependence of the elasticity (defined as the ratio of the final to the initial kinetic energy of the clouds) on the velocity and mass ratio of the colliding clouds, magnetic field strength, and gas metallicity for head-on collisions. The problem has been studied both analytic...

Heliospheric (HSP) radio emission detected by the Voyager spacecraft between 1.8 kHz and 3.6 kHz from the distant heliosphere is interpreted as emission generated close to and at the heliopause (HP), the interface between the ionised very local interstellar (LIC) gas and the supersonic solar wind (SW) stream. Radio emission is assumed to be triggered by secondary charge exchange ionisation of i...

The diffusion of uni-directional magnetic fields by two dimensional turbulent flows in a weakly ionized gas is studied. The fields here are orthogonal to the plane of fluid motion. This simple model arises in the context of the decay of the mean magnetic flux to mass ratio in the interstellar medium. When ions are strongly coupled to neutrals, the transport of a large–scale magnetic field is dr...

We consider the problem of magnetic-energy amplification by a turbulent flow of conducting fluid. This effect is known as the small-scale turbulent dynamo, and it is believed to be relevant in application to magnetic fields in astrophysical objects. It is, in fact, a generic property of random (in time and/or space) flows that they can amplify magnetic fluctuations at scales smaller than the sc...

Context. The magnetic field strength in interstellar clouds can be estimated indirectly from measurements of dust polarization by assuming that turbulent kinetic energy is comparable to the fluctuating energy, and using spread angles estimate latter. method developed Davis (1951, Phys. Rev., 81, 890) Chandrasekhar Fermi (1953, ApJ, 118, 1137) (DCF) assumes incompressible magnetohydrodynamic (MH...

The distribution of interstellar dust grains (ISDG) observed in the Solar System depends on the nature of the interstellar medium-solar wind interaction. The charge of the grains couples them to the interstellar magnetic field (ISMF) resulting in some fraction of grains being excluded from the heliosphere while grains on the larger end of the size distribution, with gyroradii comparable to the ...