Modeling Solar Energetic Particle Transport near a Wavy Heliospheric Current Sheet

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http://hdl.handle.net/10138/312252

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Battarbee , M , Dalla , S & Marsh , M S 2018 , ' Modeling Solar Energetic Particle Transport near a Wavy Heliospheric Current Sheet ' , Astrophysical Journal , vol. 854 , no. 1 , 23 . https://doi.org/10.3847/1538-4357/aaa3fa

Title: Modeling Solar Energetic Particle Transport near a Wavy Heliospheric Current Sheet
Author: Battarbee, Markus; Dalla, Silvia; Marsh, Mike S.
Contributor: University of Helsinki, Particle Physics and Astrophysics
Date: 2018-02-10
Language: eng
Number of pages: 14
Belongs to series: Astrophysical Journal
ISSN: 0004-637X
URI: http://hdl.handle.net/10138/312252
Abstract: Understanding the transport of solar energetic particles (SEPs) from acceleration sites at the Sun into interplanetary space and to the Earth is an important question for forecasting space weather. The interplanetary magnetic field (IMF), with two distinct polarities and a complex structure, governs energetic particle transport and drifts. We analyze for the first time the effect of a wavy heliospheric current sheet (HCS) on the propagation of SEPs. We inject protons close to the Sun and propagate them by integrating fully 3D trajectories within the inner heliosphere in the presence of weak scattering. We model the HCS position using fits based on neutral lines of magnetic field source surface maps (SSMs). We map 1 au proton crossings, which show efficient transport in longitude via HCS, depending on the location of the injection region with respect to the HCS. For HCS tilt angles around 30 degrees-40 degrees, we find significant qualitative differences between A+ and A- configurations of the IMF, with stronger fluences along the HCS in the former case but with a distribution of particles across a wider range of longitudes and latitudes in the latter. We show how a wavy current sheet leads to longitudinally periodic enhancements in particle fluence. We show that for an A+ IMF configuration, a wavy HCS allows for more proton deceleration than a flat HCS. We find that A- IMF configurations result in larger average fluences than A+ IMF configurations, due to a radial drift component at the current sheet.
Subject: methods: numerical
Sun: activity
Sun: heliosphere
Sun: magnetic fields
Sun: particle emission
GALACTIC COSMIC-RAYS
MAGNETIC-FIELDS
1 AU
ACCELERATION
DRIFTS
115 Astronomy, Space science
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