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Vladimir Mikhailov (NRNU MEPHI Moscow) On behavior PAMELA collaboration
SUB CUTOFF SPECTRA OF ELECTRONS AND POSITRONS
measured in the PAMELA experiment
O Adriani c GC Barbarino g GA Bazilevskaja l R Bellotti j M Boezio e EA Bogomolov kL Bonechi c M Bongi c V Bonvicini e SV Borisov b S Bottai c A Bruno j F Cafagna j
D Campana g R Carbone g P Carlson f M Casolino a G Castellini d L Consiglio g MP De Pascale a C De Santis a N De Simone a V Di Felice a AM Galper b
LA Grishantseva b WGillard f G Jerse e AV Karelin b SV Koldashov b SYu Krutkov k AN Kvashnin l AA Leonov b VV Malakhov b L Marcelli a AMayorov b W Menn h VV
Mikhailov b EMocchiutti e A Monaco j N Mori c NN Nikonov k G Osteria g P Papini cFPalma M Pearce f P Picozza a C Pizzolotto e M Ricci i SB Ricciarini c L Rossetto f MF Runtso b S J Stochaj eM Simon h R Sparvoli a P Spillantini c YuI Stozhkov l A
Vacchi e E Vannuccini c GI Vasiliev k SA Voronov b G Wu f YT Yurkin b G Zampa e N Zampa e VG Zverev b
a - INFN Structure of Rome ldquoTor Vergatardquo and Physics Department of University of Rome ldquoTor Vergatardquo Rome Italyb - Moscow Engineering and Physics Institute Moscow Russiac - INFN Structure of Florence and Physics Department of University of Florence Florence Italyd - IFAC Florence Italy e - INFN Structure of Trieste and Physics Department of University of Trieste Trieste Italyf - KTH Department of Physics Stockholm Swedeng - INFN Structure of Naples and Physics Department of University of Naples Naples Italyh ndash University at Siegen Siegen Germanyi- INFN Laboratori Nazionali di Frascati Frascati Italyj - INFN Structure of Bari and Physics Department of University Bari Italyk - Ioffe Physical Technical Institute St Petersburg Russial - Lebedev Physical Institute Moscow Russia
Secondary production in residual atmosphere and results of old experiments
CR proton
Interaction point
Secondary positron
bull Production of charged pions in CR protons interaction with residual atmosphere
е и 02е++ е- bull Trapping of secondary particles live time T(h)
Intensity (h) ~Icr (h)T(h)~ 1 constant (h)
Total electron amppositron flux measured in equatorial region
Rcutgt10GV before 1999
N Grigorov Possibility of existence of a radiation belt around the earth consisting of electrons with energies of 100 MeV and above Soviet Physics Doklady Vol 22 p305 1977
The cosmic ray intensity above the atmosphere (Phys Rev 75 1 1949)ldquoSecondaries emerging from the atmosphere and executing orbits in the Earthrsquos magnetic field undoubtedly contribute in (hellip) intensity above t he atmosphererdquo
OSO-3 measurements of atmospheric gamma rays (ApJ1972177341)
PAMELA is here
Satellite was launched 15062006 on elliptical polar orbit with inclination 700
altitude 350-610km More then 20TB
data were gathered in 5 Years
Main object of PAMELA
magnetic spectrometer is detail investigation of energy spectra antiparticles in cosmic
rays in energy interval50 MeV ndash 300 GeV
MDR ~ 1TeVCalorimeter ~ 16Xo
Geomfactor= 216 cm2srLivetime ~ 5years
Calorimeter+ToF+tracker selection provide rejection factor ~104-105
See papers E Mocchiutti ID815 L Rossetto ID 667 for more details
PAMELA instrument
Satellite ResursDK 1 has elliptical orbit 350-
610km with inclination ~700 The instrument is
pointed to zenith mainly Attitude information
fixed every 30 sec For every event geographic
and geomagnetic coordinates are calculated
Pitch-angle of every events calculated using IGRF
model and direction inside the instrument
Count rate of top PAMELA counter low energy ~MeV protons ratePolar region Equatorial region and South Atlantic Anomaly (SAA) are clearly seen
Altitude of geomagnetic field lines L-shell =112
PAMELA IS HERE
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
O Adriani c GC Barbarino g GA Bazilevskaja l R Bellotti j M Boezio e EA Bogomolov kL Bonechi c M Bongi c V Bonvicini e SV Borisov b S Bottai c A Bruno j F Cafagna j
D Campana g R Carbone g P Carlson f M Casolino a G Castellini d L Consiglio g MP De Pascale a C De Santis a N De Simone a V Di Felice a AM Galper b
LA Grishantseva b WGillard f G Jerse e AV Karelin b SV Koldashov b SYu Krutkov k AN Kvashnin l AA Leonov b VV Malakhov b L Marcelli a AMayorov b W Menn h VV
Mikhailov b EMocchiutti e A Monaco j N Mori c NN Nikonov k G Osteria g P Papini cFPalma M Pearce f P Picozza a C Pizzolotto e M Ricci i SB Ricciarini c L Rossetto f MF Runtso b S J Stochaj eM Simon h R Sparvoli a P Spillantini c YuI Stozhkov l A
Vacchi e E Vannuccini c GI Vasiliev k SA Voronov b G Wu f YT Yurkin b G Zampa e N Zampa e VG Zverev b
a - INFN Structure of Rome ldquoTor Vergatardquo and Physics Department of University of Rome ldquoTor Vergatardquo Rome Italyb - Moscow Engineering and Physics Institute Moscow Russiac - INFN Structure of Florence and Physics Department of University of Florence Florence Italyd - IFAC Florence Italy e - INFN Structure of Trieste and Physics Department of University of Trieste Trieste Italyf - KTH Department of Physics Stockholm Swedeng - INFN Structure of Naples and Physics Department of University of Naples Naples Italyh ndash University at Siegen Siegen Germanyi- INFN Laboratori Nazionali di Frascati Frascati Italyj - INFN Structure of Bari and Physics Department of University Bari Italyk - Ioffe Physical Technical Institute St Petersburg Russial - Lebedev Physical Institute Moscow Russia
Secondary production in residual atmosphere and results of old experiments
CR proton
Interaction point
Secondary positron
bull Production of charged pions in CR protons interaction with residual atmosphere
е и 02е++ е- bull Trapping of secondary particles live time T(h)
Intensity (h) ~Icr (h)T(h)~ 1 constant (h)
Total electron amppositron flux measured in equatorial region
Rcutgt10GV before 1999
N Grigorov Possibility of existence of a radiation belt around the earth consisting of electrons with energies of 100 MeV and above Soviet Physics Doklady Vol 22 p305 1977
The cosmic ray intensity above the atmosphere (Phys Rev 75 1 1949)ldquoSecondaries emerging from the atmosphere and executing orbits in the Earthrsquos magnetic field undoubtedly contribute in (hellip) intensity above t he atmosphererdquo
OSO-3 measurements of atmospheric gamma rays (ApJ1972177341)
PAMELA is here
Satellite was launched 15062006 on elliptical polar orbit with inclination 700
altitude 350-610km More then 20TB
data were gathered in 5 Years
Main object of PAMELA
magnetic spectrometer is detail investigation of energy spectra antiparticles in cosmic
rays in energy interval50 MeV ndash 300 GeV
MDR ~ 1TeVCalorimeter ~ 16Xo
Geomfactor= 216 cm2srLivetime ~ 5years
Calorimeter+ToF+tracker selection provide rejection factor ~104-105
See papers E Mocchiutti ID815 L Rossetto ID 667 for more details
PAMELA instrument
Satellite ResursDK 1 has elliptical orbit 350-
610km with inclination ~700 The instrument is
pointed to zenith mainly Attitude information
fixed every 30 sec For every event geographic
and geomagnetic coordinates are calculated
Pitch-angle of every events calculated using IGRF
model and direction inside the instrument
Count rate of top PAMELA counter low energy ~MeV protons ratePolar region Equatorial region and South Atlantic Anomaly (SAA) are clearly seen
Altitude of geomagnetic field lines L-shell =112
PAMELA IS HERE
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Secondary production in residual atmosphere and results of old experiments
CR proton
Interaction point
Secondary positron
bull Production of charged pions in CR protons interaction with residual atmosphere
е и 02е++ е- bull Trapping of secondary particles live time T(h)
Intensity (h) ~Icr (h)T(h)~ 1 constant (h)
Total electron amppositron flux measured in equatorial region
Rcutgt10GV before 1999
N Grigorov Possibility of existence of a radiation belt around the earth consisting of electrons with energies of 100 MeV and above Soviet Physics Doklady Vol 22 p305 1977
The cosmic ray intensity above the atmosphere (Phys Rev 75 1 1949)ldquoSecondaries emerging from the atmosphere and executing orbits in the Earthrsquos magnetic field undoubtedly contribute in (hellip) intensity above t he atmosphererdquo
OSO-3 measurements of atmospheric gamma rays (ApJ1972177341)
PAMELA is here
Satellite was launched 15062006 on elliptical polar orbit with inclination 700
altitude 350-610km More then 20TB
data were gathered in 5 Years
Main object of PAMELA
magnetic spectrometer is detail investigation of energy spectra antiparticles in cosmic
rays in energy interval50 MeV ndash 300 GeV
MDR ~ 1TeVCalorimeter ~ 16Xo
Geomfactor= 216 cm2srLivetime ~ 5years
Calorimeter+ToF+tracker selection provide rejection factor ~104-105
See papers E Mocchiutti ID815 L Rossetto ID 667 for more details
PAMELA instrument
Satellite ResursDK 1 has elliptical orbit 350-
610km with inclination ~700 The instrument is
pointed to zenith mainly Attitude information
fixed every 30 sec For every event geographic
and geomagnetic coordinates are calculated
Pitch-angle of every events calculated using IGRF
model and direction inside the instrument
Count rate of top PAMELA counter low energy ~MeV protons ratePolar region Equatorial region and South Atlantic Anomaly (SAA) are clearly seen
Altitude of geomagnetic field lines L-shell =112
PAMELA IS HERE
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
PAMELA is here
Satellite was launched 15062006 on elliptical polar orbit with inclination 700
altitude 350-610km More then 20TB
data were gathered in 5 Years
Main object of PAMELA
magnetic spectrometer is detail investigation of energy spectra antiparticles in cosmic
rays in energy interval50 MeV ndash 300 GeV
MDR ~ 1TeVCalorimeter ~ 16Xo
Geomfactor= 216 cm2srLivetime ~ 5years
Calorimeter+ToF+tracker selection provide rejection factor ~104-105
See papers E Mocchiutti ID815 L Rossetto ID 667 for more details
PAMELA instrument
Satellite ResursDK 1 has elliptical orbit 350-
610km with inclination ~700 The instrument is
pointed to zenith mainly Attitude information
fixed every 30 sec For every event geographic
and geomagnetic coordinates are calculated
Pitch-angle of every events calculated using IGRF
model and direction inside the instrument
Count rate of top PAMELA counter low energy ~MeV protons ratePolar region Equatorial region and South Atlantic Anomaly (SAA) are clearly seen
Altitude of geomagnetic field lines L-shell =112
PAMELA IS HERE
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Main object of PAMELA
magnetic spectrometer is detail investigation of energy spectra antiparticles in cosmic
rays in energy interval50 MeV ndash 300 GeV
MDR ~ 1TeVCalorimeter ~ 16Xo
Geomfactor= 216 cm2srLivetime ~ 5years
Calorimeter+ToF+tracker selection provide rejection factor ~104-105
See papers E Mocchiutti ID815 L Rossetto ID 667 for more details
PAMELA instrument
Satellite ResursDK 1 has elliptical orbit 350-
610km with inclination ~700 The instrument is
pointed to zenith mainly Attitude information
fixed every 30 sec For every event geographic
and geomagnetic coordinates are calculated
Pitch-angle of every events calculated using IGRF
model and direction inside the instrument
Count rate of top PAMELA counter low energy ~MeV protons ratePolar region Equatorial region and South Atlantic Anomaly (SAA) are clearly seen
Altitude of geomagnetic field lines L-shell =112
PAMELA IS HERE
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Satellite ResursDK 1 has elliptical orbit 350-
610km with inclination ~700 The instrument is
pointed to zenith mainly Attitude information
fixed every 30 sec For every event geographic
and geomagnetic coordinates are calculated
Pitch-angle of every events calculated using IGRF
model and direction inside the instrument
Count rate of top PAMELA counter low energy ~MeV protons ratePolar region Equatorial region and South Atlantic Anomaly (SAA) are clearly seen
Altitude of geomagnetic field lines L-shell =112
PAMELA IS HERE
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Study terrestrial magnetosphereStudy terrestrial magnetosphere
Spectra of protonsSpectra of protons
Secondary re-entrant-albedo protons
Magnetic polar cups( galactic protons)
Geomagnetic cutoff
Trapped protons in SAA See more in FCafagna ID963
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Primary CR
Secondary CR
Equatorial region Geomagnetic latitude lt03 Data of 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Pamela and AMS measurements AMS flew on-board the Space Shuttle during decade in 1998 Inclination ~560 altitude ~400km (Phys Lett B 484 200010ndash22)
e- e+
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Latitudinal behavior of electronpositron spectra
Positrons
GeV
Electrons
GeV
electronspositrons
GeV
L-shell
electronspositrons
GeV
L-shell
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
M Honda (2009)
Calculated energy spectra at 550km for vertical cut-off0 ndash 06 06 - 11 ndash 15 15 - 2 2 ndash 4 4 ndash 7 7 ndash 10 10 ndash 14 GV
10 ndash 14 GV 4-7 GV
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Primary component
East-west effect
Rigidity cut off from East direction is ~60GV due to shadow of the Earth from West
direction ~10GV =gt source of secondary electrons is supressed e+e- ratio is high
Fig modified from httphepbuedu~superkew-effecthtml
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
01 1 10 1000
1
2
3
4
5
Fp
os
Fel
Energy GeV
L=12
Positron to electron ratio in equatorial region
Pitch-angle distributions of ratios
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Longitudinal behavior of electronpositron spectra
0-40 Longitude degree 120-160 240-280
GeV
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Observation at Llt12 Data of PAMELA for August 2006 Comparison of data Bgt024Gs (equatorial subcut-off data) and Blt021Gs (SAA data)
Calculated spectra of trapped electrons and positrons from Gusev et al 2002 Earth Planets Space
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Conclusion
1 Subcutoff electron and positron fluxes were measured by the PAMELA experiment with high accuracy from 100MV to cutoff Rigidity
2 Electron and positron fluxes have a complex structure depending from direction energy latitude and longitude
3 New data might be useful to tune models of secondary production
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Thank you
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Proton spectra since August 2006 till September of 2009 effect of solar modulation is visible
Low energy proton intensity is increasing with time
The changes of solar modulation parameter since 072006 till 022008
Galactic proton spectra
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
Primary component was increasing in time during 2006-2009 Secondary electrons and positrons are practically constant small variations of counting rate are possible due to orbit rotation mean Lshell and
pitch-angle
secondary
primaryFluxes are normalized to September 2006
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