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Radio Emission Radio Emission from Masuda from Masuda
SourcesSources
New Jersey Institute of New Jersey Institute of TechnologyTechnology
Sung-Hong ParkSung-Hong Park
ContentsContents
Introduction of Masuda SourcesIntroduction of Masuda Sources Gyro-Synchrotron Radiation (GSR) Gyro-Synchrotron Radiation (GSR)
from Masuda Sourcesfrom Masuda Sources Diffusive Synchrotron Radiation Diffusive Synchrotron Radiation
(DSR) from Masuda Sources(DSR) from Masuda Sources Discussion amp SummaryDiscussion amp Summary
1-1 Yohkoh SXT and HXT 1-1 Yohkoh SXT and HXT SpecificationSpecification
InstrumentInstrument Fourier-Fourier-synthesis type synthesis type collimatorcollimator
Energy bandEnergy band 15-24-35-57-15-24-35-57-100 keV (4 100 keV (4 bands)bands)
Angular Angular resolutionresolution
~ 5 arc sec~ 5 arc sec
Field of viewField of view Full solar diskFull solar disk
Effective areaEffective area ~ 70 cm~ 70 cm22
Time resolution Time resolution 05 sec05 sec
InstrumentInstrument Modified Modified Wolter type I Wolter type I grazing grazing incident mirrorincident mirror
Wavelength Wavelength rangerange
3-60 Aring 3-60 Aring (selectable (selectable with filters)with filters)
Angular Angular resolutionresolution
~ 25 arc sec~ 25 arc sec
Field of viewField of view Full solar diskFull solar disk
Time resolution Time resolution Up to 05 secUp to 05 sec
lt SXT lt SXT gtgt
lt HXT lt HXT gtgt
1-2 X-ray Observation of 1-2 X-ray Observation of Masuda FlaresMasuda Flares
Image of the Soft X-ray Telescope (SXT) and the Hard X-ray Telescope (HXT) on board the Yohkoh satellite
1-3 Plasma Parameters of 1-3 Plasma Parameters of Masuda SourcesMasuda Sources
Emitting Volume V Emitting Volume V [cm[cm33]]
125 125 10102626
Electron Number Electron Number Density nDensity nee [cm [cm-3-3]]
101099
Electron Temperature Electron Temperature TTe e [K][K]
2 2 101077
Spectral Index of Spectral Index of Electron Energy Electron Energy Distribution Distribution δδ
33
Magnetic field Magnetic field Strength B [G]Strength B [G]
40-120 40-120
2-1 Gyro-Synchrotron 2-1 Gyro-Synchrotron Radiation (GSR)Radiation (GSR)
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
ContentsContents
Introduction of Masuda SourcesIntroduction of Masuda Sources Gyro-Synchrotron Radiation (GSR) Gyro-Synchrotron Radiation (GSR)
from Masuda Sourcesfrom Masuda Sources Diffusive Synchrotron Radiation Diffusive Synchrotron Radiation
(DSR) from Masuda Sources(DSR) from Masuda Sources Discussion amp SummaryDiscussion amp Summary
1-1 Yohkoh SXT and HXT 1-1 Yohkoh SXT and HXT SpecificationSpecification
InstrumentInstrument Fourier-Fourier-synthesis type synthesis type collimatorcollimator
Energy bandEnergy band 15-24-35-57-15-24-35-57-100 keV (4 100 keV (4 bands)bands)
Angular Angular resolutionresolution
~ 5 arc sec~ 5 arc sec
Field of viewField of view Full solar diskFull solar disk
Effective areaEffective area ~ 70 cm~ 70 cm22
Time resolution Time resolution 05 sec05 sec
InstrumentInstrument Modified Modified Wolter type I Wolter type I grazing grazing incident mirrorincident mirror
Wavelength Wavelength rangerange
3-60 Aring 3-60 Aring (selectable (selectable with filters)with filters)
Angular Angular resolutionresolution
~ 25 arc sec~ 25 arc sec
Field of viewField of view Full solar diskFull solar disk
Time resolution Time resolution Up to 05 secUp to 05 sec
lt SXT lt SXT gtgt
lt HXT lt HXT gtgt
1-2 X-ray Observation of 1-2 X-ray Observation of Masuda FlaresMasuda Flares
Image of the Soft X-ray Telescope (SXT) and the Hard X-ray Telescope (HXT) on board the Yohkoh satellite
1-3 Plasma Parameters of 1-3 Plasma Parameters of Masuda SourcesMasuda Sources
Emitting Volume V Emitting Volume V [cm[cm33]]
125 125 10102626
Electron Number Electron Number Density nDensity nee [cm [cm-3-3]]
101099
Electron Temperature Electron Temperature TTe e [K][K]
2 2 101077
Spectral Index of Spectral Index of Electron Energy Electron Energy Distribution Distribution δδ
33
Magnetic field Magnetic field Strength B [G]Strength B [G]
40-120 40-120
2-1 Gyro-Synchrotron 2-1 Gyro-Synchrotron Radiation (GSR)Radiation (GSR)
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
1-1 Yohkoh SXT and HXT 1-1 Yohkoh SXT and HXT SpecificationSpecification
InstrumentInstrument Fourier-Fourier-synthesis type synthesis type collimatorcollimator
Energy bandEnergy band 15-24-35-57-15-24-35-57-100 keV (4 100 keV (4 bands)bands)
Angular Angular resolutionresolution
~ 5 arc sec~ 5 arc sec
Field of viewField of view Full solar diskFull solar disk
Effective areaEffective area ~ 70 cm~ 70 cm22
Time resolution Time resolution 05 sec05 sec
InstrumentInstrument Modified Modified Wolter type I Wolter type I grazing grazing incident mirrorincident mirror
Wavelength Wavelength rangerange
3-60 Aring 3-60 Aring (selectable (selectable with filters)with filters)
Angular Angular resolutionresolution
~ 25 arc sec~ 25 arc sec
Field of viewField of view Full solar diskFull solar disk
Time resolution Time resolution Up to 05 secUp to 05 sec
lt SXT lt SXT gtgt
lt HXT lt HXT gtgt
1-2 X-ray Observation of 1-2 X-ray Observation of Masuda FlaresMasuda Flares
Image of the Soft X-ray Telescope (SXT) and the Hard X-ray Telescope (HXT) on board the Yohkoh satellite
1-3 Plasma Parameters of 1-3 Plasma Parameters of Masuda SourcesMasuda Sources
Emitting Volume V Emitting Volume V [cm[cm33]]
125 125 10102626
Electron Number Electron Number Density nDensity nee [cm [cm-3-3]]
101099
Electron Temperature Electron Temperature TTe e [K][K]
2 2 101077
Spectral Index of Spectral Index of Electron Energy Electron Energy Distribution Distribution δδ
33
Magnetic field Magnetic field Strength B [G]Strength B [G]
40-120 40-120
2-1 Gyro-Synchrotron 2-1 Gyro-Synchrotron Radiation (GSR)Radiation (GSR)
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
1-2 X-ray Observation of 1-2 X-ray Observation of Masuda FlaresMasuda Flares
Image of the Soft X-ray Telescope (SXT) and the Hard X-ray Telescope (HXT) on board the Yohkoh satellite
1-3 Plasma Parameters of 1-3 Plasma Parameters of Masuda SourcesMasuda Sources
Emitting Volume V Emitting Volume V [cm[cm33]]
125 125 10102626
Electron Number Electron Number Density nDensity nee [cm [cm-3-3]]
101099
Electron Temperature Electron Temperature TTe e [K][K]
2 2 101077
Spectral Index of Spectral Index of Electron Energy Electron Energy Distribution Distribution δδ
33
Magnetic field Magnetic field Strength B [G]Strength B [G]
40-120 40-120
2-1 Gyro-Synchrotron 2-1 Gyro-Synchrotron Radiation (GSR)Radiation (GSR)
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
1-3 Plasma Parameters of 1-3 Plasma Parameters of Masuda SourcesMasuda Sources
Emitting Volume V Emitting Volume V [cm[cm33]]
125 125 10102626
Electron Number Electron Number Density nDensity nee [cm [cm-3-3]]
101099
Electron Temperature Electron Temperature TTe e [K][K]
2 2 101077
Spectral Index of Spectral Index of Electron Energy Electron Energy Distribution Distribution δδ
33
Magnetic field Magnetic field Strength B [G]Strength B [G]
40-120 40-120
2-1 Gyro-Synchrotron 2-1 Gyro-Synchrotron Radiation (GSR)Radiation (GSR)
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
2-1 Gyro-Synchrotron 2-1 Gyro-Synchrotron Radiation (GSR)Radiation (GSR)
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
2-2 Kleinrsquos Approximate 2-2 Kleinrsquos Approximate numerical treatment of GSRnumerical treatment of GSR
The emissivity j and absorption coefficient k radiated by n particles per unit volume with charge ndashq and mass m in a magnetic field B are then
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
2-2 Kleinrsquos Computation Code 2-2 Kleinrsquos Computation Code for GSRfor GSR
If the pitch-angle integration by Laplacersquos method of approximate asymptotic integration and a weakly anisotropic distribution (Petrosian 1981) are considered
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
2-3 GSR from Masuda Sources2-3 GSR from Masuda Sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-1 Diffusive Synchrotron 3-1 Diffusive Synchrotron RadiationRadiation
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-2 Derivation for Non-3-2 Derivation for Non-Relativistic DSRRelativistic DSR
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-3 Estimation of Randomly 3-3 Estimation of Randomly Magnetic Field StrengthMagnetic Field Strength
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-4 Calculation of the NRDSR 3-4 Calculation of the NRDSR intensity from electronsintensity from electrons
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda SourcesSources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
3-5 NRDSR from Masuda 3-5 NRDSR from Masuda sourcessources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
4 Discussion amp Summary4 Discussion amp Summary
The GSR and DSR are very different for The GSR and DSR are very different for different model of the Masuda sources different model of the Masuda sources which implies a way of distinguishing which implies a way of distinguishing between the modelsbetween the models
To observe the radio emissions from the To observe the radio emissions from the Masuda sources we need a radio telescope Masuda sources we need a radio telescope (or array) which has 1-10 GHz observational (or array) which has 1-10 GHz observational frequency band with high spectral frequency band with high spectral resolution and at least 7 arcsec spatial resolution and at least 7 arcsec spatial resolution corresponding to the typical size resolution corresponding to the typical size of the Masuda sourcesof the Masuda sources
