The 2019 July 2 Total Solar Eclipse: Prediction of the Coronal Magnetic Field Structure and Polarization Characteristics. (arXiv:1906.10201v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dash_S/0/1/0/all/0/1">Soumyaranjan Dash</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhowmik_P/0/1/0/all/0/1">Prantika Bhowmik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+S_A/0/1/0/all/0/1">Athira B S</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghosh_N/0/1/0/all/0/1">Nirmalya Ghosh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nandy_D/0/1/0/all/0/1">Dibyendu Nandy</a>
On 2019 July 2 a total solar eclipse — visible across some parts of the
Southern Pacific Ocean, Chile and Argentina — will enable observations of the
Sun’s large-scale coronal structure. The structure of the Sun’s corona and
their emission characteristics are determined by underlying magnetic fields
which also govern coronal heating and solar eruptive events. However, coronal
magnetic field measurements remain an outstanding challenge. Computational
models of coronal magnetic fields serve an important purpose in this context.
Earlier work has demonstrated that the large-scale coronal field is governed by
slow surface flux evolution and memory build-up which allows for prediction of
the coronal structure on solar rotational timescales. Utilizing this idea and
based upon a 51 day forward run of a data-driven solar surface flux transport
model and a Potential Field Source Surface model, we predict the Sun’s coronal
structure for the 2019 July 2 solar eclipse. We also forward model the
polarization characteristics of the coronal emission from the predicted
magnetic fields. We predict two large-scale streamer structures and their
locations on the east and west limbs of the Sun and discuss the possibility of
development of a pseudo-streamer based on an analysis of field line topology.
This study is relevant for coronal magnetometry initiatives from ground-based
facilities such as the Daniel K. Inouye Solar Telescope and Coronal
Multichannel Polarimeter, and upcoming space-based instruments such as the
Solar Ultraviolet Imaging Telescope and the Variable Emission Line Coronagraph
onboard ISRO’s Aditya-L1 space mission.
On 2019 July 2 a total solar eclipse — visible across some parts of the
Southern Pacific Ocean, Chile and Argentina — will enable observations of the
Sun’s large-scale coronal structure. The structure of the Sun’s corona and
their emission characteristics are determined by underlying magnetic fields
which also govern coronal heating and solar eruptive events. However, coronal
magnetic field measurements remain an outstanding challenge. Computational
models of coronal magnetic fields serve an important purpose in this context.
Earlier work has demonstrated that the large-scale coronal field is governed by
slow surface flux evolution and memory build-up which allows for prediction of
the coronal structure on solar rotational timescales. Utilizing this idea and
based upon a 51 day forward run of a data-driven solar surface flux transport
model and a Potential Field Source Surface model, we predict the Sun’s coronal
structure for the 2019 July 2 solar eclipse. We also forward model the
polarization characteristics of the coronal emission from the predicted
magnetic fields. We predict two large-scale streamer structures and their
locations on the east and west limbs of the Sun and discuss the possibility of
development of a pseudo-streamer based on an analysis of field line topology.
This study is relevant for coronal magnetometry initiatives from ground-based
facilities such as the Daniel K. Inouye Solar Telescope and Coronal
Multichannel Polarimeter, and upcoming space-based instruments such as the
Solar Ultraviolet Imaging Telescope and the Variable Emission Line Coronagraph
onboard ISRO’s Aditya-L1 space mission.
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