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