A Statistical Study to Determine the Origin of Long-duration Gamma-Ray Flares
Abstract
Two scenarios have been proposed to account for sustained ≥30 MeV gamma-ray emission in solar flares: (1) prolonged particle acceleration/trapping involving large-scale magnetic loops at the flare site, and (2) precipitation of high-energy (>300 MeV) protons accelerated at coronal/interplanetary shock waves. To determine which of these scenarios is more likely, we examine the associated soft X-ray flares, coronal mass ejections (CMEs), and solar energetic proton events for (a) the long-duration gamma-ray flares (LDGRFs) observed by the Large Area Telescope on Fermi, and (b) delayed and/or spatially extended high-energy gamma-ray flares observed by the Gamma-ray Spectrometer on the Solar Maximum Mission, the Gamma-1 telescope on the Gamma satellite, and the Energetic Gamma-Ray Experiment Telescope on the Compton Gamma-Ray Observatory. For the Fermi data set of 11 LDGRFs with >100 MeV emission lasting for ≥~2 hr, we search for associations and reverse associations between LDGRFs, X-ray flares, CMEs, and SEPs, i.e., beginning with the gamma-ray flares and also, in turn, with X-class soft X-ray flares, fast (≥1500 km s-1) and wide CMEs, and intense (peak flux ≥2.67 × 10-3 protons cm-2 s-1 sr-1, with peak to background ratio >1.38) >300 MeV SEPs at 1 au. While LDGRFs tend to be associated withmore »
- Authors:
-
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Univ. of Colorado, Boulder, CO (United States). Ann and H.J. Smead Aerospace Engineering Sciences
- SLAC National Accelerator Lab. and Stanford Univ., Menlo Park, CA (United States). W.W. Hansen Experimental Physics Lab., Kavli Inst. for Particle Astrophysics and Cosmology and Dept. of Physics
- National Inst. of Nuclear Physics (INFN), Pisa (Italy)
- Publication Date:
- Research Org.:
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE; National Science Foundation (NSF); Atmospheric and Environmental Research (AER), Lexington, MA (United States)
- OSTI Identifier:
- 1473799
- Report Number(s):
- LA-UR-17-27146
Journal ID: ISSN 1538-4357
- Grant/Contract Number:
- AC52-06NA25396
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 864; Journal Issue: 1; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; 58 GEOSCIENCES; Heliospheric and Magnetospheric Physics; solar flares
Citation Formats
Winter, Lisa Marie, Bernstein, Valerie, Omodei, Nicola, and Pesce-Rollins, Melissa. A Statistical Study to Determine the Origin of Long-duration Gamma-Ray Flares. United States: N. p., 2018.
Web. doi:10.3847/1538-4357/aad3c0.
Winter, Lisa Marie, Bernstein, Valerie, Omodei, Nicola, & Pesce-Rollins, Melissa. A Statistical Study to Determine the Origin of Long-duration Gamma-Ray Flares. United States. https://doi.org/10.3847/1538-4357/aad3c0
Winter, Lisa Marie, Bernstein, Valerie, Omodei, Nicola, and Pesce-Rollins, Melissa. Wed .
"A Statistical Study to Determine the Origin of Long-duration Gamma-Ray Flares". United States. https://doi.org/10.3847/1538-4357/aad3c0. https://www.osti.gov/servlets/purl/1473799.
@article{osti_1473799,
title = {A Statistical Study to Determine the Origin of Long-duration Gamma-Ray Flares},
author = {Winter, Lisa Marie and Bernstein, Valerie and Omodei, Nicola and Pesce-Rollins, Melissa},
abstractNote = {Two scenarios have been proposed to account for sustained ≥30 MeV gamma-ray emission in solar flares: (1) prolonged particle acceleration/trapping involving large-scale magnetic loops at the flare site, and (2) precipitation of high-energy (>300 MeV) protons accelerated at coronal/interplanetary shock waves. To determine which of these scenarios is more likely, we examine the associated soft X-ray flares, coronal mass ejections (CMEs), and solar energetic proton events for (a) the long-duration gamma-ray flares (LDGRFs) observed by the Large Area Telescope on Fermi, and (b) delayed and/or spatially extended high-energy gamma-ray flares observed by the Gamma-ray Spectrometer on the Solar Maximum Mission, the Gamma-1 telescope on the Gamma satellite, and the Energetic Gamma-Ray Experiment Telescope on the Compton Gamma-Ray Observatory. For the Fermi data set of 11 LDGRFs with >100 MeV emission lasting for ≥~2 hr, we search for associations and reverse associations between LDGRFs, X-ray flares, CMEs, and SEPs, i.e., beginning with the gamma-ray flares and also, in turn, with X-class soft X-ray flares, fast (≥1500 km s-1) and wide CMEs, and intense (peak flux ≥2.67 × 10-3 protons cm-2 s-1 sr-1, with peak to background ratio >1.38) >300 MeV SEPs at 1 au. While LDGRFs tend to be associated with bright X-class flares, we find that only one-third of the X-class flares during the time of Fermi monitoring coincide with an LDGRF. However, nearly all fast, wide CMEs are associated with an LDGRF. These preliminary association analyses favor the proton precipitation scenario, however there is a prominent counter-example of a potentially magnetically well-connected solar eruption with >100 MeV emission for ~10 hr for which the near-Earth >300 MeV proton intensity did not rise above background.},
doi = {10.3847/1538-4357/aad3c0},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 864,
place = {United States},
year = {Wed Aug 29 00:00:00 EDT 2018},
month = {Wed Aug 29 00:00:00 EDT 2018}
}
Web of Science
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