We investigate the contribution of shocks amplified magnetic field in turbulent fluids to reentrant particle effect. More specifically we focused our attention on the reentrant particles influence to the solar modulation of energetic particles, in the heliosphere, in particular with amplified fields close to the termination shock. A simple I D model of heliosphere is used for a first approximation of modulation in such a case. The parameters of simulations are mean free paths of particles in heliosphere and in interstellar magnetic field. Mean free paths are scaled to multiplication of particle gyroradius. In Hel iosphere we use Paker's field amplified close to the termination shock and in interstellar space we test a set of possible values of magnetic field. © 2010 by World Scientific Publishing Co. Pte. Ltd.
Bobik, P., Kudela, K., Boschini, M., Grandi, D., Gervasi, M., Rancoita, P., et al. (2010). Reentrant Heliospheric Particles in case of Shocks Amplified Magnetic Fields. In Astroparticle Particle and Space Physics, Detectors and Medical Physics Applications (pp.751-754). World Scientific Publishing Co. Pte Ltd [10.1142/9789814307529_0119].
Reentrant Heliospheric Particles in case of Shocks Amplified Magnetic Fields
Grandi, D;GERVASI, MASSIMO;
2010
Abstract
We investigate the contribution of shocks amplified magnetic field in turbulent fluids to reentrant particle effect. More specifically we focused our attention on the reentrant particles influence to the solar modulation of energetic particles, in the heliosphere, in particular with amplified fields close to the termination shock. A simple I D model of heliosphere is used for a first approximation of modulation in such a case. The parameters of simulations are mean free paths of particles in heliosphere and in interstellar magnetic field. Mean free paths are scaled to multiplication of particle gyroradius. In Hel iosphere we use Paker's field amplified close to the termination shock and in interstellar space we test a set of possible values of magnetic field. © 2010 by World Scientific Publishing Co. Pte. Ltd.
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