| NSF Org: |
AGS Division of Atmospheric and Geospace Sciences |
| Recipient: |
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| Initial Amendment Date: | July 12, 2024 |
| Latest Amendment Date: | July 12, 2024 |
| Award Number: | 2350366 |
| Award Instrument: | Standard Grant |
| Program Manager: |
Andreas Keiling
akeiling@nsf.gov (703)292-7834 AGS Division of Atmospheric and Geospace Sciences GEO Directorate for Geosciences |
| Start Date: | August 1, 2024 |
| End Date: | July 31, 2027 (Estimated) |
| Total Intended Award Amount: | $517,046.00 |
| Total Awarded Amount to Date: | $517,046.00 |
| Funds Obligated to Date: |
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| History of Investigator: |
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| Recipient Sponsored Research Office: |
1 SILBER WAY BOSTON MA US 02215-1703 (617)353-4365 |
| Sponsor Congressional District: |
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| Primary Place of Performance: |
1 SILBER WAY Boston MA US 02215-1703 |
| Primary Place of
Performance Congressional District: |
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| Unique Entity Identifier (UEI): |
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| Parent UEI: |
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| NSF Program(s): | SOLAR-TERRESTRIAL |
| Primary Program Source: |
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| Program Reference Code(s): | |
| Program Element Code(s): |
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| Award Agency Code: | 4900 |
| Fund Agency Code: | 4900 |
| Assistance Listing Number(s): | 47.050 |
ABSTRACT
The investigators will carry out theoretical analysis and computer simulations of solar observations to test the hypothesis that heating in the coolest parts of the Sun?s atmosphere is caused by small-scale (meter-sized) slow-moving plasma processes referred to as the Thermal Farley-Buneman Instability. This may also occur in the atmospheres of other stars and planets, including the Earth. The researchers will train graduate, undergraduate, and high school students in methods of computational plasma physics. The student groups will include women and people from historically excluded populations.
The team will constrain their models using data from the Interface Region Imaging Spectrograph (IRIS) on the NASA Solar Observation Satellite using the Mg II spectral lines in the NUV passband. They will use full-disk scans performed once month to capture a large variety of targets. They will also use Fe I 617.3 nm data with 1 arcsecond resolution obtained with the NASA Solar Dynamics Observatory?s Helioseismic and Magnetic Imager (SDO/HMI) instrument for measurements of the photospheric magnetic field. The work will include a series of multifluid and kinetic simulations to explore the nonlinear and thermal properties of the resulting turbulence and incorporate the electron heating into larger radiative magnetohydrodynamic codes. The models will also help understand observations from NSF?s new DKIST solar observatory.
This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.
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