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27 April 2024 |
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Article overview
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Predicting the Structure of the Solar Corona and Inner Heliosphere during Parker Solar Probe's First Perihelion Pass | | Pete Riley
; Cooper Downs
; Jon A. Linker
; Zoran Mikic
; Roberto Lionello
; Ronald M. Caplan
; | | Date: |
26 Feb 2019 | | Abstract: | NASA’s Parker Solar Probe (Parker) spacecraft reached its first perihelion of
35.7 solar radii on November 5th, 2018. To aid in mission planning, and in
anticipation of the unprecedented measurements to be returned, in late October,
we developed a three-dimensional magnetohydrodynamic (MHD) solution for the
solar corona and inner heliosphere, driven by the then available observations
of the Sun’s photospheric magnetic field. Our model incorporates a
wave-turbulence-driven (WTD) model to heat the corona. Here, we present our
predictions for the structure of the solar corona and the likely {it in situ}
measurements that Parker will be returning over the next few months. We infer
that, in the days prior to 1st Encounter, Parker was immersed in wind emanating
from a positive-polarity equatorial coronal hole. During the encounter,
however, field lines from the spacecraft mapped to another, negative-polarity
equatorial coronal hole. Following the encounter, Parker was magnetically
connected to the large, positive-polarity northern polar coronal hole. When the
Parker data become available, these model results can be used to assist in
their calibration and interpretation, and, additionally, provide a global
context for interpreting the localized {it in situ} measurements. In
particular, we can identify what types of solar wind Parker encountered, what
the underlying magnetic structure was, and how complexities in the orbital
trajectory can be interpreted within a global, inertial frame. Ultimately, the
measurements returned by Parker can be used to constrain current theories for
heating the solar corona and accelerating the solar wind. | | Source: | arXiv, 1902.9673 | | Services: | Forum | Review | PDF | Favorites | |
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