Prediction of the Sun’s Corona for the Total Solar Eclipse on 2019 July 2

Dash, Soumyaranjan; Bhowmik, Prantika; Nandy, Dibyendu

doi:10.3847/2515-5172/ab2ae3

Cited by 4 publications

(2 citation statements)

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“…Here, we utilize the Nandy et al (2018) prediction methodology-a combination of the PSSFT and PFSS models-to predict the large-scale coronal magnetic structure of the 2019 July 2 total solar eclipse. A short research note with the predicted coronal magnetic structure is communicated in Dash et al (2019). This work contains description of the methodology with detailed in-depth analysis of the coronal magnetic field structure and topology including the possibility of a pseudostreamer appearing in the future.…”

Section: Introductionmentioning

confidence: 99%

Prediction of the Sun’s Coronal Magnetic Field and Forward-modeled Polarization Characteristics for the 2019 July 2 Total Solar Eclipse

Dash

Bhowmik

Athira

et al. 2020

ApJ

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On 2019 July 2 a total solar eclipse—visible across parts of the Southern Pacific Ocean, Chile, and Argentina—enabled observations of the Sun’s corona. The structure and emission characteristics of the corona are determined by underlying magnetic fields, which also govern coronal heating and solar eruptive events. However, coronal magnetic field measurements remain an outstanding challenge. Coronal magnetic field models serve an important purpose in this context. Earlier work has demonstrated that the large-scale coronal structure is governed by surface flux evolution and memory buildup, which allows for its prediction on solar rotational timescales. Utilizing this idea and based upon a 51 day forward run of a predictive solar surface flux transport model and a potential field source surface model, we predict the coronal structure of the 2019 July 2 solar eclipse. We also forward model the polarization characteristics of the coronal emission. Our prediction of two large-scale streamer structures and their locations on the east and west limbs of the Sun match eclipse observations reasonably well. We demonstrate that the Sun’s polar fields strongly influence the modeled corona, concluding that accurate polar field observations are critical. This study is relevant for coronal magnetometry initiatives envisaged with the Daniel K. Inouye Solar Telescope, Coronal Multichannel Polarimeter and upcoming space-based instruments such as Solar Orbiter, Solar Ultraviolet Imaging Telescope and the Variable Emission Line Coronagraph on board the Indian Space Research Organisation’s Aditya-L1 space mission.

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Section: Introductionmentioning

confidence: 99%

Prediction of the Sun’s Coronal Magnetic Field and Forward-modeled Polarization Characteristics for the 2019 July 2 Total Solar Eclipse

Dash

Bhowmik

Athira

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Here we utilize the Nandy et al (2018) prediction methodology -a combination of the PSSFT and PFSS models -to predict the large-scale coronal magnetic structure of the 2019 July 2 total solar eclipse. A short research note with the predicted coronal magnetic structure is communicated in Dash et al (2019). This work contains description of the methodology with detailed in-depth analysis of the coronal magnetic field structure and topology including the possibility of a pseudo-streamer appearing in the future.…”

Section: Introductionmentioning

confidence: 99%

The 2019 July 2 Total Solar Eclipse: Prediction of the Coronal Magnetic Field Structure and Polarization Characteristics

Dash,

Bhowmik,

et al. 2019

Preprint

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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

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