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| ||V1 ||[:TimeAverage IQUV:Time Average IQUV] || Perform a time average of IQUV polarization elements with interpolation of input frames to centered time of interest ||Time, duration, Lev1 Filtergrams (on CCD coordinates) ||Time-Averaged IQUV (on CCD coordinates) ||12 Minutes ||Duration, Filtering ||No ||Stage 3 ||HMI Calibration ||No ||Temporal Anti-aliasing filter ||J. Schou ||Remap includes geometry and vector transform. See A1. ||High June || ||V2 ||[:StokesInversion:Stokes Inversion] || Invert Stokes Parameters to determine vector magnetic field components at each CCD pixel; field not disambiguated. ||IQUV (on CCD coordinates) ||'''^B^,,vec,,'''=B,,total,,,FF, inclination, azimuth(180), uncertainties (on CCD coordinates) ||12-minute ||Quick,Threshold ||Yes ||Stage 3 ||90% ||60% ||Earlier JSOC version worked ||R. Bogart, S. Tomczyk, J. Borrero, Y. Liu ||Disk/CCD geometry, angles relative to Line of Sight ||High July || ||V3 ||[:FieldDisambiguation:Field Disambiguation] || Resolve ambiguity in the azimuthal field component inherent in inversion; will be model and method dependent ||'''^B^,,vec,,''' (on CCD coordinates) ||360 Azimuth, uncertainty (on CCD coordinates) ||12-minute ||Patch,FD,Quick ||Yes ||Stage 2 ||80% ||50% ||Averaging vs. Sampling ||T. Hoeksema ||Disk/CCD geometry, angles relative to line of sight ||High July/August || ||V4 ||[:MergeBvec:Merge Vector B] || Merge multiple vector magnetic field images into a temporally averaged magnetogram in solar heliographic coordinates ||Assorted '''^B^,,vec,,''' ||'''^B^,,vec,,''' ||12-minute ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Issues ||L. Svalgaard ||Assemble Vector Magnetogram from Heterogeneous Sources ||Low December || ||V5 || [:BxByBzTransform:Bx,By,Bz Transform] || Transform magnetic field in CCD image coordinates to proper local rectilinear heliographic coordinates suitable for export ||'''^B^,,vec,,''' || (on CCD coordinates) B,,x,,,B,,y,,,B,,z,,; Uncertainties (local on a 2D projection plate with the solar north up) ||On Export ||Options ||No ||Stage 1 ||Code ||DRMS ||Issues ||Y. Liu ||Local heliocentric equatorial rectilinear vector B components for ARPs ||Medium October || ||V6 ||[:BrBtBpTransform:Br,Btheta,Bphi Transform] || Transform image vector field to heliocentric global coordinate system suitable for export ||'''^B^,,vec,,''' (on CCd coordinates) ||B,,r,,,B,,theta,,,B,,phi,,; Uncertainties (on heliographic coordinates) ||On Export ||Options ||No ||Stage 1 ||Code ||DRMS ||Issues ||Y. Liu ||Heliocentric equatorial spherical coordinate vector B components ||Medium October || ||V7 ||[:BtotInAzTransform:B_total Inc Az Transform] || Transform from CCD image coordinates to heliocentric global coordinates suitable for export ||'''^B^,,vec,,''' ||B,,total,,, Inclination, Azimuth; Uncertainties ||On Export ||Options ||No ||Stage 1 ||Code ||DRMS ||Issues ||Y. Liu ||Btot and angles relative to heliocentric equatorial coordinates ||Medium October || ||V8 ||[:VectorB Remap:Vector B Remap] || Convert from CCD Frame vector field to heliocentric vector field components ||'''^B^,,vec,,''', time (on CCD coordinates) ||'''^B^,,vec,,''' HeliographicFrame ||12min ||Rotation Corrections ||No ||Stage 3 ||'''JV2Helio''' ||DRMS ||Differential Rotation, Vector averages ||X. Sun ||Magnetograms in Carrington and Heliographic coordinates ||Medium August || ||V9 || [:VectorBSpatialAverage:Spatially Average Bvec ] || Spatially average vector field components in a single CCD-frame image ||'''^B^,,vec,,''' (on CCD coordinates) ||'''^B^,,vec,,''' (on image coordinates with P angle removed, but retain B0 angle) ||On Export ||Anti-aliasing ||No ||Stage 3 ||'''DeRotMean''' ||DRMS ||Vector geometry ||J. Beck, X. Sun ||Better to invert averaged IQUV? ||High July || ||V10 || [:VectorBTemporalAverage:Temporally Average Bvec ] || Temporally average vector field components in CCD frames accounting for translation due to rotation ||'''^B^,,vec,,''' (on CCD coordinates) ||'''^B^,,vec,,''' (on image coordinates with P angle removed, but retain B0 angle) ||Hours ||Duration, Mapping ||No ||Stage 3 ||'''DeRotMean''' ||DRMS ||Rotation correction, Anti-aliasing ||J. Beck, X. Sun ||Better to invert averaged IQUV? ||High July || ||V11 || CarringtonSynopticMap || Combine series of remapped heliographic images into a standard Carrington synoptic map || '''^B^,,vec,,''' HeliographicFrame || B,,r,, SynopticMap ||Per rotation ||Resolution, Rotation Correction, Averaging ||Yes ||Stage 2 ||Los, makesynop ||No ||Need to balance temporal scale of map and features ||Y. Liu, X. Zhao ||Radial Field ||Medium October || ||V12 || SynchronicFrame || Insert a remapped vector field magnetogram into [the center of] a synchronic synoptic map ||'''^B^,,vec,,''' Magnetograms, SynopticMap, Time ||B,,r,, [:SynopticMap:Synchronic Frame] ||Hourly ||Averaging, Mapping ||No ||Stage 2 ||LoS ||DRMS ||Issues ||X. Zhao, J. T. Hoeksema ||Remark ||Medium October || ||V13 || DailySynchronicUpdate || Insert time-averaged vector field magnetogram into [the left edge of] the current synchronic map ||SynopticMap, '''^B^,,vec,,''' HeliographicFrame ||B,,r,, [:SynopticMap:Synchronic Frame] ||Daily ||Averaging, Rotation Correction ||Yes ||Stage 2 ||LoS ||DRMS ||Resolution,Averaging,Far Side ||X. Zhao, J. T. Hoeksema ||Input to regular global coronal modeling ||Medium October || |
||V1 ||[[TimeAverage_IQUV|Time Average IQUV]] || Perform a time average of IQUV polarization components with interpolation of input frames to centered time of interest ||Time, duration, Lev1 Filtergrams (on CCD coordinates) ||Time-Averaged IQUV (on CCD coordinates) ||12 Minutes ||Duration, Filtering ||No ||Stage 3 ||HMI Calibration ||No ||Temporal Anti-aliasing filter ||J. Schou ||Remap includes geometry and vector transform. See A1. ||High June || ||V2 ||[[StokesInversion|Stokes Inversion]] || Invert Stokes Parameters to determine vector magnetic field components at each CCD pixel; field not disambiguated. ||IQUV (on CCD coordinates) ||'''^B^,,vec,,'''=B,,total,,,FF, inclination, azimuth(180), uncertainties (on CCD coordinates) ||12-minute ||Quick,Threshold ||Yes ||Stage 3 ||90% ||60% ||Earlier JSOC version worked ||R. Bogart, S. Tomczyk, J. Borrero, Y. Liu ||Disk/CCD geometry, angles relative to Line of Sight ||High July || ||V3 ||[[FieldDisambiguation|Field Disambiguation]] || Resolve ambiguity in the azimuthal field component inherent in inversion; will be model and method dependent ||'''^B^,,vec,,''' (on CCD coordinates) ||360 Azimuth, uncertainty (on CCD coordinates) ||12-minute ||Patch,FD,Quick ||Yes ||Stage 2 ||80% ||50% ||Averaging vs. Sampling ||T. Hoeksema ||Disk/CCD geometry, angles relative to line of sight ||High July/August || ||V4 ||[[MergeBvec|Merge Vector B]] || Merge multiple vector magnetic field images into a temporally averaged magnetogram in solar heliographic coordinates ||Assorted '''^B^,,vec,,''' ||'''^B^,,vec,,''' ||12-minute ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Issues ||L. Svalgaard ||Assemble Vector Magnetogram from Heterogeneous Sources ||Low December || ||V5 || [[BxByBzTransform|Bx,By,Bz Transform]] || Transform magnetic field in CCD image coordinates to proper local rectilinear heliographic coordinates suitable for export ||'''^B^,,vec,,''' || (on CCD coordinates) B,,x,,,B,,y,,,B,,z,,; Uncertainties (local on a 2D projection plate with the solar north up) ||On Export ||Options ||No ||Stage 1 ||Code ||DRMS ||Issues ||Y. Liu ||Local heliocentric equatorial rectilinear vector B components for ARPs ||Medium October || ||V6 ||[[BrBtBpTransform|Br,Btheta,Bphi Transform]] || Transform image vector field to heliocentric global coordinate system suitable for export ||'''^B^,,vec,,''' (on CCd coordinates) ||B,,r,,,B,,theta,,,B,,phi,,; Uncertainties (on heliographic coordinates) ||On Export ||Options ||No ||Stage 1 ||Code ||DRMS ||Issues ||Y. Liu ||Heliocentric equatorial spherical coordinate vector B components ||Medium October || ||V7 ||[[BtotInAzTransform|B_total, Inc, Az Transform]] || Transform from CCD image coordinates to heliocentric global coordinates suitable for export ||'''^B^,,vec,,''' ||B,,total,,, Inclination, Azimuth; Uncertainties ||On Export ||Options ||No ||Stage 1 ||Code ||DRMS ||Issues ||Y. Liu ||Btot and angles relative to heliocentric equatorial coordinates ||Medium October || ||V8 ||[[VectorB_Remap|Vector B Remap]] || Convert from CCD Frame vector field to heliocentric vector field components ||'''^B^,,vec,,''', time (on CCD coordinates) ||'''^B^,,vec,,''' HeliographicFrame ||12min ||Rotation Corrections ||No ||Stage 3 ||'''JV2Helio''' ||DRMS ||Differential Rotation, Vector averages ||X. Sun ||Magnetograms in Carrington and Heliographic coordinates ||Medium August || ||V9 || [[VectorBSpatialAverage|Spatially Average Bvec ]] || Spatially average vector field components in a single CCD-frame image ||'''^B^,,vec,,''' (on CCD coordinates) ||'''^B^,,vec,,''' (on image coordinates with P angle removed, but retain B0 angle) ||On Export ||Anti-aliasing ||No ||Stage 3 ||'''DeRotMean''' ||DRMS ||Vector geometry ||J. Beck, X. Sun ||Better to invert averaged IQUV? ||High July || ||V10 || [[VectorBTemporalAverage|Temporally Average Bvec ]] || Temporally average vector field components in CCD frames accounting for translation due to rotation ||'''^B^,,vec,,''' (on CCD coordinates) ||'''^B^,,vec,,''' (on image coordinates with P angle removed, but retain B0 angle) ||Hours ||Duration, Mapping ||No ||Stage 3 ||'''DeRotMean''' ||DRMS ||Rotation correction, Anti-aliasing ||J. Beck, X. Sun ||Better to invert averaged IQUV? ||High July || ||V11 || CarringtonSynopticMap || Combine series of remapped heliographic vector field images into a standard Carrington synoptic map || '''^B^,,vec,,''' HeliographicFrame || B,,r,, SynopticMap ||Per rotation ||Resolution, Rotation Correction, Averaging ||Yes ||Stage 2 ||Los, makesynop ||No ||Need to balance temporal scale of map and features ||Y. Liu, X. Zhao ||Radial Field ||Medium October || ||V12 || SynchronicFrame || Insert a remapped vector field magnetogram into [the center of] a synchronic synoptic map ||'''^B^,,vec,,''' Magnetograms, SynopticMap, Time ||B,,r,, [[SynopticMap|Synchronic Frame]] ||Hourly ||Averaging, Mapping ||No ||Stage 2 ||LoS ||DRMS ||Issues ||X. Zhao, J. T. Hoeksema ||Remark ||Medium October || ||V13 || DailySynchronicUpdate || Insert [time-averaged] vector field magnetogram at [the left edge of] the current synchronic map ||SynopticMap, '''^B^,,vec,,''' HeliographicFrame ||B,,r,, [[SynopticMap|Synchronic Frame]] ||Daily ||Averaging, Rotation Correction ||Yes ||Stage 2 ||LoS ||DRMS ||Resolution,Averaging,Far Side ||X. Zhao, J. T. Hoeksema ||Input to regular global coronal modeling ||Medium October || |
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| ||V15 || PolarFieldExtrapolation || Interpolate or extrapolate the unobservable polar magnetic field in a synoptic map from a longer time series ||[:SynopticMap:Synoptic Maps] ||Smoothed Polar Field, SynopticMap ||Monthly ||Extra/Inter -polation ||Yes ||Stage 3 ||IDL ||50% ||MDI algorithm doesn't apply ||X. Sun ||Remark ||Medium October || ||V16 || MagneticHarmonicCoefficients || Compute global harmonic coefficients of the magnetic field from a synoptic map ||[:SynopticMap:Synchronic Map] ||Global Harmonic Coefficients ||On Demand ||Global,Local,Order ||Yes ||Stage 3 ||100% ||90% ||Need to use qdport ||X. Sun, X. Zhao ||Remark ||Medium October || ||V17 || [:PotentialField-SourceSurface:Global PFSS Model] || Compute global PFSS model of the coronal magnetic field from a synoptic map ||[:SynopticMap:Synchronic Map] ||Coronal Field Simulation ||Daily ||Options ||Yes ||Stage 2 ||100% ||95% ||Issues ||X. Sun, X. Zhao ||Remark ||Medium October || ||V18 || [:PotentialField-Local:Local Potential Field Model] || Compute local potential magnetic field in corona overlying an active region patch ||ARP B,,r,, ||Local Coronal Field ||12-minute? ||option : (1) pixel size of input map (2) which method to use? ||Yes ? ||Stage 3 ||(1)slow iterative Laplace solver, 100% (2) Green Function 100% (3) FFT method to be tested ||70% ||Need to develop c-wrapper including part to specify patch data. Method 1 is slow. Three methods give different answer because of differrent boundary condition. ||K. Hayashi ||Potential by-product of disambiguation ||High August || ||V19 || [:NonLinearForceFreeField:NLFFF Model] || Compute Non-linear Force Free Field Model of coronal field overlying an ARP ||B,,x,,,B,,y,,,B,,z,, (local on a 2D projection plane with solar north up) ||Coronal Field in Cube ||Daily ||Options ||Archive ||Stage 2 ||Code ||DRMS ||Issues ||Y. Liu ||Remark ||Low January || ||V20 || [:InferredHorizontalFlow-Local:Local Inferred Horizontal Flow] || Determine local horizontal surface flows of magnetic and intensity features ( various methods) ||B,,x,,,B,,y,,,B,,z,, Time Series (local on a 2D projection plane) ||Horizontal Velocity (on local heliocentric coordinates) ||Daily ||Options ||Yes ||Stage 2 ||Code ||DRMS ||Time interval, Experience with HMI data ||T. Hoeksema ||DAVE4VM, ILCT ||Low December || ||V21 || [:InferredHorizontalFlow-Global:Global Inferred Flow Field] || Determine full-disk horizontal surface flows of magnetic and intensity features ||B,,los,, Time Series (on heliographic coordinates) ||Horizontal Velocity (on heliographic coordinates) ||12min.? ||Options ||Yes ? ||Stage 3 ||FLCT 100% in C by G.F. Wrapper 95% in C/Fortran ||95% ||define the cadence (12min is ok?). ||K. Hayashi, G. Fisher ||FLCT ||Low November || |
||V15 || PolarFieldExtrapolation || Interpolate or extrapolate the unobservable polar magnetic field in a synoptic map from a longer time series ||[[SynopticMap|Synoptic Maps]] ||Smoothed Polar Field, SynopticMap ||Monthly ||Extra/Inter -polation ||Yes ||Stage 3 ||IDL ||50% ||MDI algorithm doesn't apply ||X. Sun ||Remark ||Medium October || ||V16 || MagneticHarmonicCoefficients || Compute global harmonic coefficients of the magnetic field from a synoptic map ||[[SynopticMap|Synchronic Map]] ||Global Harmonic Coefficients ||On Demand ||Global,Local,Order ||Yes ||Stage 3 ||100% ||90% ||Need to use qdport ||X. Sun, X. Zhao ||Remark ||Medium October || ||V17 || [[PotentialField-SourceSurface|Global PFSS Model]] || Compute global PFSS model of the coronal magnetic field from a synoptic map ||[[SynopticMap|Synchronic Map]] ||Coronal Field Simulation ||Daily ||Options ||Yes ||Stage 2 ||100% ||95% ||Issues ||X. Sun, X. Zhao ||Remark ||Medium October || ||V18 || [[PotentialField-Local|Local Potential Field Model]] || Compute [high resolution] local potential magnetic field in corona overlying an active region patch ||ARP B,,r,, ||Local Coronal Field ||12-minute? ||option : (1) pixel size of input map (2) which method to use? ||Yes ? ||Stage 3 ||(1)slow iterative Laplace solver, 100% (2) Green Function 100% (3) FFT method to be tested ||70% ||Need to develop c-wrapper including part to specify patch data. Method 1 is slow. Three methods give different answer because of differrent boundary condition. ||K. Hayashi ||Potential by-product of disambiguation ||High August || ||V19 || [[NonLinearForceFreeField|NLFFF Model]] || Compute Non-linear Force Free Field Model of coronal field overlying an ARP ||B,,x,,,B,,y,,,B,,z,, (local on a 2D projection plane with solar north up) ||Coronal Field in Cube ||Daily ||Options ||Archive ||Stage 2 ||Code ||DRMS ||Issues ||Y. Liu ||Remark ||Low January || ||V20 || [[InferredHorizontalFlow-Local|Local Inferred Horizontal Flow]] || Determine local horizontal surface flows of magnetic and intensity features ( various methods) ||B,,x,,,B,,y,,,B,,z,, Time Series (local on a 2D projection plane) ||Horizontal Velocity (on local heliocentric coordinates) ||Daily ||Options ||Yes ||Stage 2 ||Code ||DRMS ||Time interval, Experience with HMI data ||T. Hoeksema ||DAVE4VM, ILCT ||Low December || ||V21 || [[InferredHorizontalFlow-Global|Global Inferred Flow Field]] || Determine full-disk horizontal surface flows of magnetic and intensity features ||B,,los,, Time Series (on heliographic coordinates) ||Horizontal Velocity (on heliographic coordinates) ||12min.? ||Options ||Yes ? ||Stage 3 ||FLCT 100% in C by G.F. Wrapper 95% in C/Fortran ||95% ||define the cadence (12min is ok?). ||K. Hayashi, G. Fisher ||FLCT ||Low November || |
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| ||V24 || ModelDynamicCorona || Compute time-evolving characteristics of the solar corona ||B,,r,, [:SynopticMap:Synchronic Map] ||Coronal Parameters ||Daily,Monthly ||Options ||Yes ||Stage 3 and 4 ||90%. ||50% ||Details to be determined. Most of the codes are ready. ||K.Hayashi, J.Linker ||TVD-MUSCL, MARS-CORHEL ||Low December || | ||V24 || ModelDynamicCorona || Compute time-evolving characteristics of the solar corona ||B,,r,, [[SynopticMap|Synchronic Map]] ||Coronal Parameters ||Daily,Monthly ||Options ||Yes ||Stage 3 and 4 ||90%. ||50% ||Details to be determined. Most of the codes are ready. ||K.Hayashi, J.Linker ||TVD-MUSCL, MARS-CORHEL ||Low December || |
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| ||V26 || [:Model3DARField:Model 3D Field over ARP ] || Perform high-resolution modeling of coronal magnetic field overlying active region patches ||'''^B^,,vec,,''' - ARP + Global ||Out ||(on demand) ||N/A ||No? ||Stage 1 ||(html) ||DRMS ||Issues ||K. Hayashi ||Link to external group codes ||Low March || ||V27 || [:SpaceWeatherProducts-Local:Browse & Space Weather Products - Local ] || Compute space weather products from local active region patches ||ARP '''^B^,,vec,,''' (local, on a 2D projection plane with solar north up) ||Activity Indices ||12-minute ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Issues ||T. Hoeksema ||Alerts Possible ||Low December || ||V28 || [:SpaceWeatherProducts-Global:Browse & Space Weather Products - Global ] || Compute Space-weather products from global synoptic magnetic field data ||B,,r,, [:SynopticMap:Synchronic Maps]/frames ||1 AU predictions ||Daily ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Issues ||T. Hoeksema ||Remark ||Low December || |
||V26 || [[Model3DARField|Model 3D Field over ARP ]] || Perform high-resolution modeling of coronal magnetic field overlying active region patches ||'''^B^,,vec,,''' - ARP + Global ||Out ||(on demand) ||N/A ||No? ||Stage 1 ||(html) ||DRMS ||Issues ||K. Hayashi ||Link to external group codes ||Low March || ||V27 || [[SpaceWeatherProducts-Local|Browse & Space Weather Products - Local ]] || Compute space weather products from local active region patches ||ARP '''^B^,,vec,,''' (local, on a 2D projection plane with solar north up) ||Activity Indices ||12-minute ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Issues ||T. Hoeksema ||Alerts Possible ||Low December || ||V28 || [[SpaceWeatherProducts-Global|Browse & Space Weather Products - Global ]] || Compute Space-weather products from global synoptic magnetic field data ||B,,r,, [[SynopticMap|Synchronic Maps]]/frames ||1 AU predictions ||Daily ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Issues ||T. Hoeksema ||Remark ||Low December || |
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| ||A1 ||FeatureRecognition || Identify, locate, and track significant active regions on the solar disk ||HMI/AIA/EVE + Other Solar Observations ||Active Region Patch locations and boundaries ||12 minute ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Interface with HEK ||T. Hoeksema ||M. Turmon, C. [:DeForest:DeForest, J. Zhang] ||High || | ||A1 ||FeatureRecognition || Identify, locate, and track significant active regions on the solar disk ||HMI/AIA/EVE + Other Solar Observations ||Active Region Patch locations and boundaries ||12 minute ||Options ||Yes ||Stage 1 ||Code ||DRMS ||Interface with HEK ||T. Hoeksema ||M. Turmon, C. [[DeForest|DeForest, J. Zhang]] ||High || |
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| ||L1 || [:B LOS-Stokes:Line-of-sight B] || Compute line-of-sight magnetic field from circularly polarized light filtergrams (MDI method) ||Circularly polarized filtergrams (on CCD coordinates) ||Line-of-Sight Magnetogram (on CCD coordinates) ||45 seconds ||None ||Yes ||Stage 3 ||HMI Test ||DRMS ||Issues ||J. Schou, S. Couvidat ||Remark ||High June || ||L2 || [:B LOS-Average:Average B_los] || Temporally and spatially average line-of-sight magnetic field images ||Magnetograms (on CCD coordinates) ||Magnetogram (on CCD coordinates) ||90s ||Cadence; spatial averaging ||No ||Stage 2 ||MDI Code ||DRMS ||Issues ||E. Benevolenskaya ||Develop various options ||High July || ||L3 || [:B LOS-Remap:Remap B_los] || Remap line-of-sight magnetic field images to heliographic coordinates ||Magnetogram (on CCD coordinates) ||[:HeliographicFrame:Heliographic Frame] ||Cadence ||Options ||Archive ||Stage 4 ||'''JV2Helio''' ||DRMS ||Issues ||L. Svalgaard ||Remark ||High June || ||L4 || [:B LOS-Remap and Average:B_los Remap & Average] || Combine magnetic images and perform temporal and spatial averaging ||Magnetograms (on CCD coordinates) ||[:HeliographicFrame:Heliographic Frame] ||Cadence ||Options ||Archive ||Stage 3 ||'''DeRotMean''' ||DRMS ||Issues ||J. Beck ||Remark ||High July || ||L5 || [:B LOS-CarringtonMap:B_los Carrington Map] || Construct standard synoptic maps from line-of-sight magnetograms ||[:HeliographicFrame:Heliographic Frames] ||SynopticMap ||Cadence ||Options ||Archive ||Stage 4 ||MDI Code ||DRMS ||Issues ||Y. Liu ||Remark ||Medium July || ||L6 || [:B LOS-SynchronicFrame:B_los Synchronic Frame] || Construct line-of-sight synchronic frame from synoptic map and magnetogram ||[:HeliographicFrame:Heliographic Frames], SynopticMap ||SynopticMap ||Cadence ||Options ||Archive ||Stage 2 ||MDI Code ||DRMS ||Issues ||X. Zhao, T. Hoeksema ||Remark ||Medium August || ||L7 || [:B LOS-DailySynchronicMap:B_los Daily Synchronic Map] || Construct daily synchronic map from line-of-sight magnetograms ||[:HeliographicFrame:Heliographic Frames] ||SynopticMap ||Cadence ||Options ||Archive ||Stage 2 ||MDI Code ||DRMS ||Issues ||X. Zhao, X. Sun ||Remark ||Medium August || ||L8a || [:B LOS-MDI Emulation:B_los MDI Emulation] || Compute ideal magnetogram from MDI data for comparison with HMI ||MDI magnetogram ||Ideal Magnetogram ||Cadence ||Resolution ||Archive ||Stage 3 ||Code ||DRMS ||Issues ||P. Scherrer ||Module needs development ||Medium September || ||L8b || [:B LOS-HMI Emulation:B_los HMI Emulation] || Compute ideal magnetogram from HMI data for comparison with MDI ||HMI magnetogram ||Ideal Magnetogram ||Cadence ||Resolution ||Archive ||Stage 1 ||Code ||DRMS ||Issues ||P. Scherrer ||Remark ||Medium October || ||L9 ||["HMI MeanField"] || Compute mean solar magnetic field from HMI magnetogram ||Magnetogram ||Mean Field ||Cadence ||Options ||Archive ||Status 2 ||Code ||DRMS ||Issues ||L. Svalgaard ||Remark ||Low January || |
||L1 || [[B_LOS-Stokes|Line-of-sight B]] || Compute line-of-sight magnetic field from filtergrams in circularly polarized light (MDI method) ||Circularly polarized filtergrams (on CCD coordinates) ||Line-of-Sight Magnetogram (on CCD coordinates) ||45 seconds ||None ||Yes ||Stage 3 ||HMI Test ||DRMS ||Issues ||J. Schou, S. Couvidat ||Remark ||High June || ||L2 || [[B_LOS-Average|Average B_los]] || Temporally and spatially average line-of-sight magnetic field images ||Magnetograms (on CCD coordinates) ||Magnetogram (on CCD coordinates) ||90s ||Cadence; spatial averaging ||No ||Stage 2 ||MDI Code ||DRMS ||Issues ||E. Benevolenskaya ||Develop various options ||High July || ||L3 || [[B_LOS-Remap|Remap B_los]] || Remap line-of-sight magnetic field images to heliographic coordinates ||Magnetogram (on CCD coordinates) ||[[HeliographicFrame|Heliographic Frame]] ||Cadence ||Options ||Archive ||Stage 4 ||'''JV2Helio''' ||DRMS ||Issues ||L. Svalgaard ||Remark ||High June || ||L4 || [[B_LOS-Remap_and_Average|B_los Remap & Average]] || Combine magnetic images and perform temporal and spatial averaging ||Magnetograms (on CCD coordinates) ||[[HeliographicFrame|Heliographic Frame]] ||Cadence ||Options ||Archive ||Stage 3 ||'''DeRotMean''' ||DRMS ||Issues ||J. Beck ||Remark ||High July || ||L5 || [[B_LOS-CarringtonMap|B_los Carrington Map]] || Construct standard synoptic maps from line-of-sight magnetograms ||[[HeliographicFrame|Heliographic Frames]] ||SynopticMap ||Cadence ||Options ||Archive ||Stage 4 ||MDI Code ||DRMS ||Issues ||Y. Liu ||Remark ||Medium July || ||L6 || [[B_LOS-SynchronicFrame|B_los Synchronic Frame]] || Construct line-of-sight synchronic frame from synoptic map and magnetogram ||[[HeliographicFrame|Heliographic Frames]], SynopticMap ||SynopticMap ||Cadence ||Options ||Archive ||Stage 2 ||MDI Code ||DRMS ||Issues ||X. Zhao, T. Hoeksema ||Remark ||Medium August || ||L7 || [[B_LOS-DailySynchronicMap|B_los Daily Synchronic Map]] || Construct daily synchronic map from line-of-sight magnetograms ||[[HeliographicFrame|Heliographic Frames]] ||SynopticMap ||Cadence ||Options ||Archive ||Stage 2 ||MDI Code ||DRMS ||Issues ||X. Zhao, X. Sun ||Remark ||Medium August || ||L8a || [[B_LOS-MDI_Emulation|B_los MDI Emulation]] || Compute ideal magnetogram from MDI data for comparison with HMI ||MDI magnetogram ||Ideal Magnetogram ||Cadence ||Resolution ||Archive ||Stage 3 ||Code ||DRMS ||Issues ||P. Scherrer ||Module needs development ||Medium September || ||L8b || [[B LOS-HMI Emulation|B_los HMI Emulation]] || Compute ideal magnetogram from HMI data for comparison with MDI ||HMI magnetogram ||Ideal Magnetogram ||Cadence ||Resolution ||Archive ||Stage 1 ||Code ||DRMS ||Issues ||P. Scherrer ||Remark ||Medium October || ||L9 ||[[HMI_MeanField]] || Compute mean solar magnetic field from HMI magnetogram ||Magnetogram ||Mean Field ||Cadence ||Options ||Archive ||Status 2 ||Code ||DRMS ||Issues ||L. Svalgaard ||Remark ||Low January || |
Descriptive Summary of Magnetic Field Modules
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HMI Pipeline -- Module Table |
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Vector Magnetic Field Modules |
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Module Link |
Summary |
Input |
Output |
Typical Cadence |
Options |
Archive |
Status |
Heritage / Module Name |
DRMS |
Issues |
Coordinator |
Remarks |
Priority/Need Date |
V1 |
Perform a time average of IQUV polarization components with interpolation of input frames to centered time of interest |
Time, duration, Lev1 Filtergrams (on CCD coordinates) |
Time-Averaged IQUV (on CCD coordinates) |
12 Minutes |
Duration, Filtering |
No |
Stage 3 |
HMI Calibration |
No |
Temporal Anti-aliasing filter |
J. Schou |
Remap includes geometry and vector transform. See A1. |
High June |
|
V2 |
Invert Stokes Parameters to determine vector magnetic field components at each CCD pixel; field not disambiguated. |
IQUV (on CCD coordinates) |
Bvec=Btotal,FF, inclination, azimuth(180), uncertainties (on CCD coordinates) |
12-minute |
Quick,Threshold |
Yes |
Stage 3 |
90% |
60% |
Earlier JSOC version worked |
R. Bogart, S. Tomczyk, J. Borrero, Y. Liu |
Disk/CCD geometry, angles relative to Line of Sight |
High July |
|
V3 |
Resolve ambiguity in the azimuthal field component inherent in inversion; will be model and method dependent |
Bvec (on CCD coordinates) |
360 Azimuth, uncertainty (on CCD coordinates) |
12-minute |
Patch,FD,Quick |
Yes |
Stage 2 |
80% |
50% |
Averaging vs. Sampling |
T. Hoeksema |
Disk/CCD geometry, angles relative to line of sight |
High July/August |
|
V4 |
Merge multiple vector magnetic field images into a temporally averaged magnetogram in solar heliographic coordinates |
Assorted Bvec |
Bvec |
12-minute |
Options |
Yes |
Stage 1 |
Code |
DRMS |
Issues |
L. Svalgaard |
Assemble Vector Magnetogram from Heterogeneous Sources |
Low December |
|
V5 |
Transform magnetic field in CCD image coordinates to proper local rectilinear heliographic coordinates suitable for export |
Bvec |
(on CCD coordinates) Bx,By,Bz; Uncertainties (local on a 2D projection plate with the solar north up) |
On Export |
Options |
No |
Stage 1 |
Code |
DRMS |
Issues |
Y. Liu |
Local heliocentric equatorial rectilinear vector B components for ARPs |
Medium October |
|
V6 |
Transform image vector field to heliocentric global coordinate system suitable for export |
Bvec (on CCd coordinates) |
Br,Btheta,Bphi; Uncertainties (on heliographic coordinates) |
On Export |
Options |
No |
Stage 1 |
Code |
DRMS |
Issues |
Y. Liu |
Heliocentric equatorial spherical coordinate vector B components |
Medium October |
|
V7 |
Transform from CCD image coordinates to heliocentric global coordinates suitable for export |
Bvec |
Btotal, Inclination, Azimuth; Uncertainties |
On Export |
Options |
No |
Stage 1 |
Code |
DRMS |
Issues |
Y. Liu |
Btot and angles relative to heliocentric equatorial coordinates |
Medium October |
|
V8 |
Convert from CCD Frame vector field to heliocentric vector field components |
Bvec, time (on CCD coordinates) |
Bvec HeliographicFrame |
12min |
Rotation Corrections |
No |
Stage 3 |
JV2Helio |
DRMS |
Differential Rotation, Vector averages |
X. Sun |
Magnetograms in Carrington and Heliographic coordinates |
Medium August |
|
V9 |
Spatially average vector field components in a single CCD-frame image |
Bvec (on CCD coordinates) |
Bvec (on image coordinates with P angle removed, but retain B0 angle) |
On Export |
Anti-aliasing |
No |
Stage 3 |
DRMS |
Vector geometry |
J. Beck, X. Sun |
Better to invert averaged IQUV? |
High July |
||
V10 |
Temporally average vector field components in CCD frames accounting for translation due to rotation |
Bvec (on CCD coordinates) |
Bvec (on image coordinates with P angle removed, but retain B0 angle) |
Hours |
Duration, Mapping |
No |
Stage 3 |
DRMS |
Rotation correction, Anti-aliasing |
J. Beck, X. Sun |
Better to invert averaged IQUV? |
High July |
||
V11 |
Combine series of remapped heliographic vector field images into a standard Carrington synoptic map |
Bvec HeliographicFrame |
Br SynopticMap |
Per rotation |
Resolution, Rotation Correction, Averaging |
Yes |
Stage 2 |
Los, makesynop |
No |
Need to balance temporal scale of map and features |
Y. Liu, X. Zhao |
Radial Field |
Medium October |
|
V12 |
Insert a remapped vector field magnetogram into [the center of] a synchronic synoptic map |
Bvec Magnetograms, SynopticMap, Time |
Hourly |
Averaging, Mapping |
No |
Stage 2 |
LoS |
DRMS |
Issues |
X. Zhao, J. T. Hoeksema |
Remark |
Medium October |
||
V13 |
Insert [time-averaged] vector field magnetogram at [the left edge of] the current synchronic map |
SynopticMap, Bvec HeliographicFrame |
Daily |
Averaging, Rotation Correction |
Yes |
Stage 2 |
LoS |
DRMS |
Resolution,Averaging,Far Side |
X. Zhao, J. T. Hoeksema |
Input to regular global coronal modeling |
Medium October |
||
V14 |
Convert standard synoptic vector field map into synchronic map for a particular time |
Bvec HeliographicFrame |
Vector SynopticMap |
Monthly |
Rotation Correction, Resolution |
Yes |
Stage 1 |
Code |
DRMS |
Sensibility of Global Bvec |
X. Zhao, J. T. Hoeksema |
Need to resolve users |
Low December |
|
V15 |
Interpolate or extrapolate the unobservable polar magnetic field in a synoptic map from a longer time series |
Smoothed Polar Field, SynopticMap |
Monthly |
Extra/Inter -polation |
Yes |
Stage 3 |
IDL |
50% |
MDI algorithm doesn't apply |
X. Sun |
Remark |
Medium October |
||
V16 |
Compute global harmonic coefficients of the magnetic field from a synoptic map |
Global Harmonic Coefficients |
On Demand |
Global,Local,Order |
Yes |
Stage 3 |
100% |
90% |
Need to use qdport |
X. Sun, X. Zhao |
Remark |
Medium October |
||
V17 |
Compute global PFSS model of the coronal magnetic field from a synoptic map |
Coronal Field Simulation |
Daily |
Options |
Yes |
Stage 2 |
100% |
95% |
Issues |
X. Sun, X. Zhao |
Remark |
Medium October |
||
V18 |
Compute [high resolution] local potential magnetic field in corona overlying an active region patch |
ARP Br |
Local Coronal Field |
12-minute? |
option : (1) pixel size of input map (2) which method to use? |
Yes ? |
Stage 3 |
(1)slow iterative Laplace solver, 100% (2) Green Function 100% (3) FFT method to be tested |
70% |
Need to develop c-wrapper including part to specify patch data. Method 1 is slow. Three methods give different answer because of differrent boundary condition. |
K. Hayashi |
Potential by-product of disambiguation |
High August |
|
V19 |
Compute Non-linear Force Free Field Model of coronal field overlying an ARP |
Bx,By,Bz (local on a 2D projection plane with solar north up) |
Coronal Field in Cube |
Daily |
Options |
Archive |
Stage 2 |
Code |
DRMS |
Issues |
Y. Liu |
Remark |
Low January |
|
V20 |
Determine local horizontal surface flows of magnetic and intensity features ( various methods) |
Bx,By,Bz Time Series (local on a 2D projection plane) |
Horizontal Velocity (on local heliocentric coordinates) |
Daily |
Options |
Yes |
Stage 2 |
Code |
DRMS |
Time interval, Experience with HMI data |
T. Hoeksema |
DAVE4VM, ILCT |
Low December |
|
V21 |
Determine full-disk horizontal surface flows of magnetic and intensity features |
Blos Time Series (on heliographic coordinates) |
Horizontal Velocity (on heliographic coordinates) |
12min.? |
Options |
Yes ? |
Stage 3 |
FLCT 100% in C by G.F. Wrapper 95% in C/Fortran |
95% |
define the cadence (12min is ok?). |
K. Hayashi, G. Fisher |
FLCT |
Low November |
|
V22 |
Compute solar wind velocity from synoptic field for space weather prediction |
Synoptic Maps |
Solar wind speed / IMF polarity |
Daily |
Options |
Archive |
Stage 2 |
50% |
50% |
New empirical function |
X. Sun, T. Hoeksema |
Remark |
Low January |
|
V23 |
Compute active region characteristics overlying active region patches |
ARP Bvec, Vhorizontal (local, on a 2D projection plane with solar north up) |
Plasma & Magnetic Properties |
On request |
Options |
Yes |
Stage 2 |
Code |
DRMS |
Issues |
Abbett, Wu |
Link to external group codes |
Low March |
|
V24 |
Compute time-evolving characteristics of the solar corona |
Coronal Parameters |
Daily,Monthly |
Options |
Yes |
Stage 3 and 4 |
90%. |
50% |
Details to be determined. Most of the codes are ready. |
K.Hayashi, J.Linker |
TVD-MUSCL, MARS-CORHEL |
Low December |
||
V25 |
Compute heliospheric conditions out to 1 AU from synoptic frames |
Synchronic maps/frames |
Solar Wind Parameters |
Daily/Monthly |
Options |
Archive |
Stage 2 |
CORHEL |
DRMS |
Issues |
T. Hoeksema |
Coordinate with external group codes |
Low February |
|
V26 |
Perform high-resolution modeling of coronal magnetic field overlying active region patches |
Bvec - ARP + Global |
Out |
(on demand) |
N/A |
No? |
Stage 1 |
(html) |
DRMS |
Issues |
K. Hayashi |
Link to external group codes |
Low March |
|
V27 |
Compute space weather products from local active region patches |
ARP Bvec (local, on a 2D projection plane with solar north up) |
Activity Indices |
12-minute |
Options |
Yes |
Stage 1 |
Code |
DRMS |
Issues |
T. Hoeksema |
Alerts Possible |
Low December |
|
V28 |
Compute Space-weather products from global synoptic magnetic field data |
Br Synchronic Maps/frames |
1 AU predictions |
Daily |
Options |
Yes |
Stage 1 |
Code |
DRMS |
Issues |
T. Hoeksema |
Remark |
Low December |
|
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|
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Associated HMI Pipeline Modules |
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|
Module Link |
Summary |
Input |
Output |
Typical Cadence |
Options |
Archive |
Status |
Heritage / Module Name |
DRMS |
Issues |
Coordinator |
Remarks |
Priority/Need Date |
A1 |
Identify, locate, and track significant active regions on the solar disk |
HMI/AIA/EVE + Other Solar Observations |
Active Region Patch locations and boundaries |
12 minute |
Options |
Yes |
Stage 1 |
Code |
DRMS |
Interface with HEK |
T. Hoeksema |
M. Turmon, C. DeForest, J. Zhang |
High |
|
A2 |
Spatially average in the proper way any HMI data product |
HMI Data Product |
DRMS Dataset |
On Demand |
Size, Anti-aliasing |
No |
Stage 2 |
Code |
DRMS |
Vector Field Averaging |
L. Svalgaard |
Remark |
High July |
|
|
|
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Line-of-Sight Magnetic Field Modules |
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|
|
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|
Module Link |
Summary |
Input |
Output |
Typical Cadence |
Options |
Archive |
Status |
Heritage / Module Name |
DRMS |
Issues |
Coordinator |
Remarks |
Priority/Need Date |
L1 |
Compute line-of-sight magnetic field from filtergrams in circularly polarized light (MDI method) |
Circularly polarized filtergrams (on CCD coordinates) |
Line-of-Sight Magnetogram (on CCD coordinates) |
45 seconds |
None |
Yes |
Stage 3 |
HMI Test |
DRMS |
Issues |
J. Schou, S. Couvidat |
Remark |
High June |
|
L2 |
Temporally and spatially average line-of-sight magnetic field images |
Magnetograms (on CCD coordinates) |
Magnetogram (on CCD coordinates) |
90s |
Cadence; spatial averaging |
No |
Stage 2 |
MDI Code |
DRMS |
Issues |
E. Benevolenskaya |
Develop various options |
High July |
|
L3 |
Remap line-of-sight magnetic field images to heliographic coordinates |
Magnetogram (on CCD coordinates) |
Cadence |
Options |
Archive |
Stage 4 |
JV2Helio |
DRMS |
Issues |
L. Svalgaard |
Remark |
High June |
||
L4 |
Combine magnetic images and perform temporal and spatial averaging |
Magnetograms (on CCD coordinates) |
Cadence |
Options |
Archive |
Stage 3 |
DRMS |
Issues |
J. Beck |
Remark |
High July |
|||
L5 |
Construct standard synoptic maps from line-of-sight magnetograms |
Cadence |
Options |
Archive |
Stage 4 |
MDI Code |
DRMS |
Issues |
Y. Liu |
Remark |
Medium July |
|||
L6 |
Construct line-of-sight synchronic frame from synoptic map and magnetogram |
Cadence |
Options |
Archive |
Stage 2 |
MDI Code |
DRMS |
Issues |
X. Zhao, T. Hoeksema |
Remark |
Medium August |
|||
L7 |
Construct daily synchronic map from line-of-sight magnetograms |
Cadence |
Options |
Archive |
Stage 2 |
MDI Code |
DRMS |
Issues |
X. Zhao, X. Sun |
Remark |
Medium August |
|||
L8a |
Compute ideal magnetogram from MDI data for comparison with HMI |
MDI magnetogram |
Ideal Magnetogram |
Cadence |
Resolution |
Archive |
Stage 3 |
Code |
DRMS |
Issues |
P. Scherrer |
Module needs development |
Medium September |
|
L8b |
Compute ideal magnetogram from HMI data for comparison with MDI |
HMI magnetogram |
Ideal Magnetogram |
Cadence |
Resolution |
Archive |
Stage 1 |
Code |
DRMS |
Issues |
P. Scherrer |
Remark |
Medium October |
|
L9 |
Compute mean solar magnetic field from HMI magnetogram |
Magnetogram |
Mean Field |
Cadence |
Options |
Archive |
Status 2 |
Code |
DRMS |
Issues |
L. Svalgaard |
Remark |
Low January |
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See ModuleTemplate