A5055664909- Solar and Space Plasma Dynamics
- Stellar, planetary, and galactic studies
- Ionosphere and magnetosphere dynamics
- Geomagnetism and Paleomagnetism Studies
- Astro and Planetary Science
- Solar Radiation and Photovoltaics
- Geophysics and Gravity Measurements
- Advanced Optical Sensing Technologies
- Geological and Geophysical Studies
- Fluid Dynamics and Turbulent Flows
- History and Developments in Astronomy
- Statistical and numerical algorithms
- Integrated Circuits and Semiconductor Failure Analysis
- Monetary Policy and Economic Impact
- Random lasers and scattering media
- Advanced Materials Characterization Techniques
- Electron and X-Ray Spectroscopy Techniques
- Spectroscopy and Laser Applications
Universities Space Research Association
2016-2019
Marshall Space Flight Center
2014-2016
Oak Ridge Associated Universities
2013-2016
University of Central Lancashire
2010-2014
Oak Ridge National Laboratory
1983
Abstract The third flight of the High-Resolution Coronal Imager (Hi-C 2.1) occurred on May 29, 2018; Sounding Rocket was launched from White Sands Missile Range in New Mexico. instrument has been modified its original configuration 1) to observe solar corona a passband that peaks near 172 Å, and uses new, custom-built low-noise camera. targeted Active Region 12712, captured 78 images at cadence 4.4 s (18:56:22 – 19:01:57 UT; 5 min 35 observing time). image spatial resolution varies due...
The Solar Dynamics Observatory (SDO) was launched in February 2010 and is now providing an unprecedented view of the solar activity at high spatial resolution cadence covering a broad range temperature layers atmosphere. We aim defining structure polar crown cavity describing its evolution during erupting process. use time series SDO/AIA observations 304\AA (50000 K) 171\AA (0.6 MK) to determine associated plasma as well different phases eruption. report on recorded 13 June located...
Fine-scale braiding of coronal magnetic loops by continuous footpoint motions may power heating via nanoflares, which are spontaneous fine-scale bursts internal reconnection. An initial nanoflare trigger an avalanche reconnection the braids, making a microflare or larger subflare. In contrast to this triggering subflares, we observe external subflares in braided field observed High-resolution Coronal Imager (Hi-C). We track development these using 12 s cadence images acquired SDO/AIA 1600,...
Plasma flows within prominences/filaments have been observed for many years and hold valuable clues concerning the mass energy balance these structures. Previous observations of primarily come from H-alpha cool EUV lines (e.g., 304A) where estimates size prominence threads has limited by resolution available instrumentation. Evidence `counter-steaming' previously inferred plasma but now, first time, directly imaged along fundamental filament million degree corona (at 193A). In this work we...
Observing the Sun at high time and spatial scales is a step towards understanding finest fundamental of heating events in solar corona. The Hi-C instrument has provided highest temporal resolution images corona EUV wavelength range to date. observed an active region on 11 July 2012, which exhibits several interesting features line 193\AA: one them existence short, small brightenings ``sparkling" edge region; we call these Bright Dots (EBDs). Individual EBDs have characteristic duration 25s...
In the Summer of 2012, High-resolution Coronal Imager (Hi-C) flew on board a NASA sounding rocket and collected highest spatial resolution images ever obtained solar corona. One goals Hi-C flight was to characterize substructure We therefore examine how intensity scales from AIA resolution. For each low-resolution pixel, we calculate standard deviation in contributing high-resolution pixel intensities compare that expected calculated noise. If these numbers are approximately equal, corona...
The light curves of solar coronal loops often peak first in channels associated with higher temperatures and then those lower. time delays between the different narrowband EUV have been measured for many individual recently every pixel an active region observation. Time exhibit a wide range values, maxima $>$ 5,000\,s. These large make up 3-26\% (depending on channel pair) pixels where significant, positive delay is measured. It has suggested that can be explained by impulsive heating. In...
Aims. We present complete Hinode Solar Optical Telescope (SOT), X-Ray (XRT)and EUV Imaging Spectrometer (EIS) observations of an X-ray bright point (XBP) observed on the 10, 11 October 2007 over its entire lifetime (~12 h). aim to show how measured plasma parameters XBP change time and also what kind similarities emission has a potential magnetic field model.