Gelu M. Nita. New Jersey Institute of Technology

Transcription

1 Gelu M. Nita New Jersey Institute of Technology

2 Online documentation and solar-soft instalation instructions Official introduction of GX Simulator: Nita et al APJ 799https:// dl=0 Fast Gyrosynchrotron Codes : Fleishman and Kuznetsov pdf?dl=0 Magnetography of Flaring Loops : Gary et al D Simulations of flaring loops: Kuznetsov et al

3 version running on Windows, Unix and Mac platforms already available on SSW create or import 3D magnetic field models import numerically defined density and temperature coronal models create magnetic flux tubes and populate them with user-defined nonuniform thermal plasma and anisotropic, nonuniform, nonthermal electron distributions investigate the spatial and spectral properties of radio and X-ray emission calculated from the model, and compare the model-derived images and spectra with observational data shared-object libraries containing fast gyrosynchrotron emission codes developed in FORTRAN and C++ soft and hard X-ray codes developed in IDL FORTRAN-based potential-field extrapolation routine IDL-based linear force free field extrapolation routine

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7 LFFF = cm

8 SOHO-MDI L= cm R= cm B 0 =140G

9 OVSA 2.8GHz T chromo = 3500K T corona = K T loop = MK

10 OVSA 8.6GHz n 0 = cm 3

11 RHESSI MeV n b = cm 3 N b = E 0 =18keV E break =40keV E max =5MeV 1 = = 3.7

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13 X-ray 15keV model on RHESSI kev OVSA image at 5.6 GHz on microwave 5.6 GHz model X-ray 15keV model on microwave 5.6GHz model RHESSI 12-25keV on OVSA 5.6 GHz

14 What s new in terms of AR Modeling? Integrated tools for generating data-driven chromospheric models Assignment to each photospheric pixel of vertical 1D adaptive height step chromospheric models (Fontenla et al. 2009) Integrated tools for generating coronal models User defined closed loops heating functions Assignment of voxel-dependent DEM distributions to compute EUV emission from TR and chromosphere (EBTEL- Klimchuk et al. 2008) Assignment of densities and temperatures derived from the moments of the DEM distributions Generation of Microwave, EUV, and soft X-ray maps based on the combined chromospheric and coronal models Ability to import numerically defined chromo and coronal models and compute MW, EUV, and X-ray synthetic emission maps Upgrade of the SSW GX_Simulator package coming this summer

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17 White Light Magnetic Field Bz

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19 Photospheric Decomposition 1. IN (Inter Network) 2. NW (Network) 3. Enhanced NW 4. Sunspot Penumbra 5. Sunspot Umbra 6. Facula 7. Plage

20 Temperature as a function of height for a number of components from 1D static solar atmospheres Brightness temperature spectra computed from the 1D models

21 Voxel Height Total Hydrogen Density Neutral Hydrogen Density Proton Density Temperature Magnetic Field

22 Q(x,y,z)=Q(Bmed, L, alpha) DEM(x,y,z)

23 Q x, y, z = Q 0 α B 2 L 1 Q 0 α = q 0 q 1 + q 4 +tanh α q 2 tanh α q 3 Closed Magnetic Field Lines alpha Closed Loop Heating Rate

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25 Density Slice Temperature Slice

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27 Q x, y, z = Q 0 α B 2 Q 0 α = q 0 q 1 + q 4 e q 2 Log α +q 3 2 Closed Magnetic Field Lines alpha Closed Loop Heating Rate

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29 BIFROST MODEL