TY - JOUR
T1 - Dressing the Coronal Magnetic Extrapolations of Active Regions with a Parameterized Thermal Structure
AU - Nita, Gelu
AU - Viall, Nicholeen M.
AU - Klimchuk, James A.
AU - Loukitcheva, Maria A.
AU - Gary, Dale
AU - Kuznetsov, Alexey A.
AU - Fleishman, Gregory
N1 - Funding Information:
This work was supported in part by NSF grants AST-1615807, AGS-1250374, AGS-1262772, and ICER-1639683; NASA grants NNX14AC87G and 80NSSC18K0015 to the New Jersey Institute of Technology; and RFBR grants 15-02-03717, 15-02-03835, and 16-02-00749. NMV and JAK are supported by the NASA GI and NASA SR programs. We thank our collaborators Sergey Anfinogentov and Alexey Stupishin for useful discussions and providing open access to their codes, including the NLFFF reconstruction code, now used by the GX_Simulator package. We thank the SDO/AIA team for the use of the AIA data.
Funding Information:
This work was supported in part by NSF grants AST-1615807, AGS-1250374, AGS-1262772, and ICER-1639683; NASA grants NNX14AC87G and 80NSSC18K0015 to the New Jersey Institute of Technology; and RFBR grants 15-02-03717, 15-02-03835, and 16-02-00749. NMV and JAK are supported by the NASA GI and NASA SR programs.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/1/20
Y1 - 2018/1/20
N2 - The study of time-dependent solar active region (AR) morphology and its relation to eruptive events requires analysis of imaging data obtained in multiple wavelength domains with differing spatial and time resolution, ideally in combination with 3D physical models. To facilitate this goal, we have undertaken a major enhancement of our IDL-based simulation tool, GX-Simulator, previously developed for modeling microwave and X-ray emission from flaring loops, to allow it to simulate quiescent emission from solar ARs. The framework includes new tools for building the atmospheric model and enhanced routines for calculating emission that include new wavelengths. In this paper, we use our upgraded tool to model and analyze an AR and compare the synthetic emission maps with observations. We conclude that the modeled magneto-thermal structure is a reasonably good approximation of the real one.
AB - The study of time-dependent solar active region (AR) morphology and its relation to eruptive events requires analysis of imaging data obtained in multiple wavelength domains with differing spatial and time resolution, ideally in combination with 3D physical models. To facilitate this goal, we have undertaken a major enhancement of our IDL-based simulation tool, GX-Simulator, previously developed for modeling microwave and X-ray emission from flaring loops, to allow it to simulate quiescent emission from solar ARs. The framework includes new tools for building the atmospheric model and enhanced routines for calculating emission that include new wavelengths. In this paper, we use our upgraded tool to model and analyze an AR and compare the synthetic emission maps with observations. We conclude that the modeled magneto-thermal structure is a reasonably good approximation of the real one.
KW - Sun: flares
KW - Sun: magnetic fields
KW - Sun: radio radiation
KW - acceleration of particles
KW - diffusion
KW - turbulence
UR - http://www.scopus.com/inward/record.url?scp=85041140268&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85041140268&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aaa4bf
DO - 10.3847/1538-4357/aaa4bf
M3 - Article
AN - SCOPUS:85041140268
SN - 0004-637X
VL - 853
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 66
ER -