Science Working Groups
Various team members toasting to PUNCH at the first science meeting June 3-5, 2020
Click on a working group title to view group members, or collapse all sections | open all sections.
WG1A: How does the young solar wind flow and evolve on global scales?
Explanation of this topic|
Scientist |
Role |
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WG co-leader; Image analysis of polar flows |
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WG co-leader; Ball-tracking and motion extraction |
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Monitor solar wind diagnostics; DSCOVR liaison |
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Tomography; solar wind structure analysis |
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Heliospheric modeling; in-situ analysis |
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Solar wind theory; Interpretation of solar wind data |
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3D wind speed interpretation |
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Wind origin & structure; in-situ liaison |
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Optical flow and motion extraction |
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Working group coordination |
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Wind origins; SoLO joint science |
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Tomography; Solar wind structure analysis |
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Tomography; solar wind structure analysis |
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Heliospheric modeling (ENLIL) |
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Corona-wind relation; image analysis; PSP liason |
WG1B: Where and how do microstructures and turbulence form in the solar wind?
Explanation of this topic|
Scientist |
Role |
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WG leader; Turbulence and microstructure analysis |
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Breakup of solar plumes; Aditya liaison |
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Coordination with ground-based radio observing techniques (IPS and FR) |
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Turbulence transport modeling; turbulence simulation; in-situ analysis |
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Solar wind theory; Interpretation of solar wind turbulence data |
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Microstructure and turbulence analysis |
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3D location and polarization analysis |
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Wind origin & structure; in-situ liaison |
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Working Group Coordination |
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Analyze solar wind turbulence |
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Turbulence theory and interpretation; PSP/ISOIS liaison; in-situ comparison |
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Turbulence analysis |
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Coronagraphic image analysis; data product integration |
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Turbulence analysis |
WG1C: What are the evolving physical processes of the Alfven surface?
Explanation of this topic|
Scientist |
Role |
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WG leader; Solar wind theory; Interpretation of solar wind data |
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Solar wind structure; Coordination with radio observations |
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Solar wind and coronal modeling; turbulence analysis of Alfven surface |
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Coronal structure |
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Alfven surface measurement and interpretation |
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Working Group coordination |
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Image processing and flow forward modeling |
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Solar wind structure; Analysis of Alfven surface location and effects; PSP coordination |
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Modeling of solar wind structure |
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Corona-wind relation; image analysis; Analyze small-scale structures, plumes, and jets in the solar corona; PSP liason |
WG2A: How do coronal mass ejections (CMEs) propagate and evolve in the solar wind?
Explanation of this topic|
Scientist |
Role |
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WG co-leader; Study of CME structure and evolution in the solar wind |
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WG co-leader; Study of CME structure and evolution in the solar wind |
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CME tracking; Space weather applications |
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Heliospheric image interpretation; Coordination with ground-based radio observing techniques (IPS and FR) |
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Analysis of CME source regions, interplanetary evolution and space weather effects. |
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Coronagraphy; CME structure; lower coronal connection science; MLSO liaison |
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CME tracking |
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CME fine-scale interior structure |
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3D location and polarization analysis |
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Wind origin & structure; in-situ liaison |
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CME modeling; Working group coordination |
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CME image interpretation |
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CME modeling |
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Space weather applications |
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Forward modeling of space weather events |
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CME-heliosphere interactions; solar wind transients and tracking; comparison with in-situ measurements; synergies with SO/PSP |
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Coronagraphic image analysis; data product integration |
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CME structure; Image analysis |
WG2B: How do quasi-stationary corotating interaction regions (CIRs) form and evolve?
Explanation of this topic|
Scientist |
Role |
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WG leader; 3D location and polarization analysis |
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CIR tracking; Space weather applications science |
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Heliospheric image interpretation; Tomography; solar wind structure analysis |
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Analysis of CIR source regions, interplanetary evolution and space weather effects. |
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CIR small-scale morphology and 3D structure |
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Working group coordination |
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CIR image interpretation |
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Tomography; Solar wind structure interpretation |
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Tomography; solar wind structure analysis |
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Heliospheric modeling (ENLIL) |
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CIR analysis; Space weather applications |
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Forward modeling of space weather events |
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Dynamic solar wind analysis |
WG2C: How do shocks form and interact with the solar wind across spatial scales?
Explanation of this topic|
Scientist |
Role |
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WG co-leader; Shock structure; SEP acceleration |
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WG co-leader; Wind origin & structure; in-situ liaison |
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Analysis of CMEs and CIRs and their interplanetary evolution including their associated shock waves; Correlation of PUNCH remote sensing and in-situ observations. |
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Shock physics and CME; solar wind structure and turbulence; Coordination with radio observations |
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CME-shock interaction analysis |
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Shock cross-scale structure (“crinkles” and “jumps”) |
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Working Group coordination |
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Quantitative image analysis |
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Turbulence theory and interpretation; PSP/ISOIS liaison; in-situ comparison |
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Analysis of small-scale dynamics |
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Heliospheric modeling (ENLIL) |
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Shock analysis; Space weather applications |
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Analysis of solar wind variability and shocks in coronal and heliospheric imagery |
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Shock structure; image analysis |
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Analyze and interpret PUNCH data on solar wind variability |
