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16th European Solar Physics Meeting

6–10 Sept 2021
Online
Europe/Rome timezone

Flux tubes and energetic particles in Parker Solar Probe orbit 5: magnetic helicity--PVI method and IS$\odot$IS observations

6 Sept 2021, 16:48
13m
Online

Online
Poster Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration Poster Session 2.5

Speaker

Francesco Pecora (Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA)

Description

Plasma turbulence can be viewed as a magnetic landscape populated by large- and small-scale coherent structures, consisting notionally of magnetic flux tubes and their boundaries. Such structures exist over a wide range of scales and exhibit diverse morphology and plasma properties. Interactions of particles with turbulence may involve temporary trapping in, as well as exclusion from, certain regions of space; generally controlled by the topology and connectivity of the magnetic field. In some cases, such as SEP ``dropouts'', the influence of the magnetic structure is dramatic; in other cases, it is more subtle, as in edge effects in SEP confinement. With Parker Solar Probe now closer to the sun than any previous mission, novel opportunities are available for examination of the relationship between magnetic flux structures and energetic particle populations.

We present a synergistic use of the magnetic helicity-partial variance of increments (PVI) technique paired with IS$\odot$IS observations of energetic particles (EPs). The filtered magnetic helicity detects large-scale helical flux tubes while the PVI identifies their boundaries, thus giving a multi-scale finer description of the structures. The correlation with EP fluxes show direct observational evidence of the modulation provided by flux tubes.

We find that helical flux tubes, accompanied by bounding large-PVI patches, act as hard boundaries that inhibit EP transport either confining populations within the helical field, or excluding them from entering it.

Primary authors

Francesco Pecora (Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA) Prof. S. Servidio (Dipartimento di Fisica, Universit\`a della Calabria, Arcavacata di Rende, 87036, IT) A. Greco (Dipartimento di Fisica, Universit\`a della Calabria, Arcavacata di Rende, 87036, IT) W. H. Matthaeus (Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA) D. J. McComas (Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA) J. Giacalone (Lunar \& Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA) C. J. Joyce (Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA) R. Bandyopadhyay (Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA) C. M. S. Cohen (California Institute of Technology, Pasadena, CA 91125, USA) R. A. Leske (California Institute of Technology, Pasadena, CA 91125, USA) M. E. Wiedenbeck (Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA) R. L. McNutt Jr. (Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA) M. E. Hill (Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA) D. G. Mitchell (Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA) E. R. Christian (NASA/Goddard Space Flight Center, Greenbeelt, MD 20771, USA) E. C. Roelof (Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA) N. A. Schwadron (University of New Hampshire, Durham, NH 03824, USA) S. D. Bale (Physics Department, University of California at Berkeley, Berkeley, CA 94720, USA)

Presentation materials

2021_ESPM_PECORA.pdf
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