Ryan French

Ryan French
National Solar Observatory

PhD

About

11
Publications
270
Reads
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40
Citations
Citations since 2016
11 Research Items
40 Citations
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2016201720182019202020212022051015
2016201720182019202020212022051015
Introduction
Solar Physicist at the National Solar Observatory (NSO). Previously an STFC-funded PhD student at the UCL Mullard Space Science Laboratory and Newkirk Fellow at the NCAR High Altitude Observatory.
Education
September 2018 - March 2022
University College London
Field of study
  • Solar Physics
September 2014 - June 2018
University College London
Field of study
  • Natural Sciences

Publications

Publications (11)
Article
Full-text available
We examine spectropolarimetric data from the Coronal Multi-channel Polarimeter (CoMP) instrument, acquired during the evolution of the 2017 September 10 X8.2 solar flare on the western solar limb. CoMP captured linearly polarized light from two emission lines of Fe xiii at 1074.7 and 1079.8 nm, from 1.03 to 1.5 solar radii. We focus here on the hot...
Article
In this multi-instrument paper, we search for evidence of sustained magnetic reconnection far beyond the impulsive phase of the X8.2-class solar flare on 2017 September 10. Using Hinode/EIS, CoMP, SDO/AIA, K-Cor, Hinode/XRT, RHESSI, and IRIS, we study the late-stage evolution of the flare dynamics and topology, comparing signatures of reconnection...
Article
The presence of current sheet instabilities, such as the tearing mode instability, are needed to account for the observed rate of energy release in solar flares. Insights into these current sheet dynamics can be revealed by the behavior of flare ribbon substructure, as magnetic reconnection accelerates particles down newly reconnected field lines i...
Article
Ryan French looks back at a momentous event, both in the history of solar physics, and his own career.
Thesis
Solar flares are one of the most energetic events in the solar system, created by the explosive conversion of magnetic free energy into particle acceleration, plasma heating and EM radiation through the process of magnetic reconnection. It is believed that in solar flares, magnetic reconnection occurs within a current sheet between converging oppos...
Preprint
Full-text available
The presence of current sheet instabilities, such as the tearing mode instability, are needed to account for the observed rate of energy release in solar flares. Insights into these current sheet dynamics can be revealed by the behaviour of flare ribbon substructure, as magnetic reconnection accelerates particles down newly reconnected field lines...
Article
Solar wind models predict that the mass flux carried away from the Sun in the solar wind should be extremely sensitive to the temperature in the corona, where the solar wind is accelerated. We perform a direct test of this prediction in coronal holes and active regions using a combination of in situ and remote sensing observations. For coronal hole...
Article
Full-text available
Ryan French and colleagues discuss their Hinode/EIS outreach work and the resulting resources available for A-level classes.
Preprint
Solar wind models predict that the mass flux carried away from the Sun in the solar wind should be extremely sensitive to the temperature in the corona, where the solar wind is accelerated. We perform a direct test of this prediction in coronal holes and active regions, using a combination of in-situ and remote sensing observations. For coronal hol...
Preprint
Full-text available
In this multi-instrument paper, we search for evidence of sustained magnetic reconnection far beyond the impulsive phase of the X8.2-class solar flare on 2017 September 10. Using Hinode/EIS, CoMP, SDO/AIA, K-Cor, Hinode/XRT, RHESSI, and IRIS, we study the late-stage evolution of the flare dynamics and topology, comparing signatures of reconnection...
Preprint
Full-text available
We examine spectropolarimetric data from the CoMP instrument, acquired during the evolution of the September 10th 2017 X8.2 solar flare on the western solar limb. CoMP captured linearly polarized light from two emission lines of Fe XIII at 1074.7 and 1079.8 nm, from 1.03 to 1.5 solar radii. We focus here on the hot plasma-sheet lying above the brig...

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