Local modulation and trapping of energetic particles by coherent magnetic structures

Tessein, Jeffrey A.; Ruffolo, D.; Matthaeus, W. H.; Wan, Minping

doi:10.1002/2016gl068045

Cited by 27 publications

(28 citation statements)

References 55 publications

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“…This indicates that there is a higher probability of finding high energetic particle count-rates near intense coherent structures. A similar result was found at 1 au using ACE data (Tessein et al 2016).…”

Section: Energetic Particles and Coherent Structuressupporting

confidence: 86%

“…One may note however that in this event the region of higher particle counts is approximately bounded on each side by elevated PVI (although still relatively low values). This is reminiscent of the suggestion made by Tessein et al (2016) that PVI events at edges of particle enhancements may sometimes be a signature of confinement (see also Seripienlert et al (2010). )…”

Section: Energetic Particles and Coherent Structuresmentioning

confidence: 55%

“…This suggests the possibility that energetic particles might be concentrated near magnetic flux tube boundaries, although other interpretations are also possible (see e.g., Kittinaradorn et al 2009;Seripienlert et al 2010;Tooprakai et al 2016;Malandraki et al 2019). This effect has also been reported at 1 au and may be associated either with transport effects, or even local acceleration processes (Tessein et al 2016;Khabarova et al 2015). An analysis focusing on a single day during which a dispersive SEP event occurred, suggests similar conclusions.…”

Section: A Dispersive Eventmentioning

confidence: 61%

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Observations of Energetic-particle Population Enhancements along Intermittent Structures near the Sun from the Parker Solar Probe

Bandyopadhyay

Matthaeus

Parashar

et al. 2020

ApJS

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Observations at 1 au have confirmed that enhancements in measured energetic particle fluxes are statistically associated with "rough" magnetic fields, i.e., fields having atypically large spatial derivatives or increments, as measured by the Partial Variance of Increments (PVI) method. One way to interpret this observation is as an association of the energetic particles with trapping or channeling within magnetic flux tubes, possibly near their boundaries. However, it remains unclear whether this association is a transport or local effect; i.e., the particles might have been energized at a distant location, perhaps by shocks or reconnection, or they might experience local energization or re-acceleration. The Parker Solar Probe (PSP), even in its first two orbits, offers a unique opportunity to study this statistical correlation closer to the corona. As a first step, we analyze the separate correlation properties of the energetic particles measured by the IS IS instruments during the first solar encounter. The distribution of time intervals between a specific type of event, i.e., the waiting time, can indicate the nature of the underlying process. We find that the IS IS observations show a power-law distribution of waiting

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Section: Energetic Particles and Coherent Structuressupporting

confidence: 86%

Section: Energetic Particles and Coherent Structuresmentioning

confidence: 55%

Section: A Dispersive Eventmentioning

confidence: 61%

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Observations of Energetic-particle Population Enhancements along Intermittent Structures near the Sun from the Parker Solar Probe

Bandyopadhyay

Matthaeus

Parashar

et al. 2020

ApJS

Self Cite

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“…They include significant variations in the magnetic field direction. In cases where the energy dissipation or particle acceleration effects are strongly skewed toward the environments with strong variations of the magnetic field direction (e.g., Chen et al 2015;Chasapis et al 2015;Tessein et al 2016), these effects will not be adequately captured by the reduced models.…”

Section: The Energy Dissipationmentioning

confidence: 99%

Influence of a large-scale field on energy dissipation in magnetohydrodynamic turbulence

Zhdankin¹,

Boldyrev

Mason

2017

Monthly Notices of the Royal Astronomical Society

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In magnetohydrodynamic (MHD) turbulence, the large-scale magnetic field sets a preferred local direction for the small-scale dynamics, altering the statistics of turbulence from the isotropic case. This happens even in the absence of a total magnetic flux, since MHD turbulence forms randomly oriented large-scale domains of strong magnetic field. It is therefore customary to study small-scale magnetic plasma turbulence by assuming a strong background magnetic field relative to the turbulent fluctuations. This is done, for example, in reduced models of plasmas, such as reduced MHD, reduced-dimension kinetic models, gyrokinetics, etc., which make theoretical calculations easier and numerical computations cheaper. Recently, however, it has become clear that the turbulent energy dissipation is concentrated in the regions of strong magnetic field variations. A significant fraction of the energy dissipation may be localized in very small volumes corresponding to the boundaries between strongly magnetized domains. In these regions the reduced models are not applicable. This has important implications for studies of particle heating and acceleration in magnetic plasma turbulence. The goal of this work is to systematically investigate the relationship between local magnetic field variations and magnetic energy dissipation, and to understand its implications for modeling energy dissipation in realistic turbulent plasmas.

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“…The magnetic structure of the solar wind is of interest for a number of reasons. The magnetic structure acts to duct energetic particles (McCracken & Ness, 1966;Tessein et al, 2016;Trenchi et al, 2013) and to scatter energetic particles (Qin & Li, 2008;Zimbardo et al, 2008), understanding particle transport and interpreting particle measurements requires some understanding of the properties of the heliospheric magnetic structure. The propagation of interplanetary shocks (Chashei & Shishov, 1995;Heinemann & Siscoe, 1974;Zank et al, 2003) and the acceleration of particles by shocks is dependent on the nature of the magnetic structure (Guo & Giacalone, 2010;Kocharov et al, 2013;Niemiec & Ostrowski, 2004;Sandroos & Vainio, 2006); an understanding of the properties of the heliospheric magnetic structure is needed to understand these shock processes.…”

Section: Introductionmentioning

confidence: 99%

On the Motion of the Heliospheric Magnetic Structure Through the Solar Wind Plasma

Borovsky

2020

JGR Space Physics

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A reference frame in the solar wind can often be found wherein the flow vector v is everywhere approximately parallel to the magnetic field vector B. This is the frame of the heliospheric magnetic structure moving relative to the plasma. Since v⊥ is very small in this reference frame, the magnetic structure appears to have little temporal evolution. The structure moves outward away from the Sun faster than the plasma flow. Even for highly Alfvénic plasma, the structure does not move at the Alfvén speed relative to the proton plasma, rather it moves at ~0.7 vA. This may be caused by the spread in the vector directions of the local magnetic field. The degree of inhomogeneity of the plasma is hypothesized to control the motion of the magnetic structure through the plasma. If so, non‐Alfvénicity may be owed to an inability of Alfvénic perturbations to coherently propagate from Alfvénic injections at the Sun. Schemes that mathematically advect magnetic and plasma structure from upstream solar wind monitors to the Earth may be improved by calculating and including the motion of the structure relative to the solar wind velocity vector.

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Local modulation and trapping of energetic particles by coherent magnetic structures

Cited by 27 publications

References 55 publications

Observations of Energetic-particle Population Enhancements along Intermittent Structures near the Sun from the Parker Solar Probe

Observations of Energetic-particle Population Enhancements along Intermittent Structures near the Sun from the Parker Solar Probe

Influence of a large-scale field on energy dissipation in magnetohydrodynamic turbulence

On the Motion of the Heliospheric Magnetic Structure Through the Solar Wind Plasma

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