The PLANETOCOSMICS Geant4 application L. Desorgher Physikalisches Institut, University of Bern.

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The PLANETOCOSMICS Geant4 application L. Desorgher Physikalisches Institut, University of Bern

Outline Motivation Description of the code Simulation results for the Earth + validation Simulation results for Mars Simulation results for Mercury Results for Jupiter and Europa

Energetic particles in space Energetic particles in space Permises Interdites Galactic cosmic rays ~10 MeV->10 26 eV Solar energetic particles ~keV-> GeV Radiation belts in magnetosphere ~keV->10 2 MeV

Motivation : model the interactions of energetic particles with planets Motivation : model the interactions of energetic particles with planets Permises Interdites Atmosphere ionisation Sputtering of atmosphere and surface Production of cosmogenic nuclides Measurements of the soil composition Quantify the radiation environment of planets Albedo, CRAND process Dose for aircrew and space mission Dose vs depth in soil

Laurent Desorgher5 PLANETOCOSMICS GEANT4 Application Interaction of energetic particles with Planet Atmospheres and Soils.

Laurent Desorgher6 PLANETOCOSMICS Geant4 Application Propagation of charged particles in the Planet Magnetosphere

PLANETOCOSMICS PLANETOCOSMICS Permises Interdites Interaction of energetic particles with Earth, Mars, Mercury Fluxes of secondary particles at user defined altitudes atmospheric depths, and soil depths Energy deposited vs atmospheric depth and vs soil depth Propagation in magnetic field Different coordinate system relative to planets Visualisation of particle trajectories and field lines Analysis based on Root or AIDA

Flux of ionising particles over Moscow in 2000 Flux of ionising particles over Moscow in 2000 Permises Interdites

Atmosphere ionisation induced by GCR Atmosphere ionisation induced by GCR Permises Interdites New Hampshire Durham 1969

Neutron flux at 56 g cm -2 R c =0.8 GV in June 1997 Permises Interdites

The 20 th January 2005 Ground Level Enhancement Neutron Monitor Observations

From NM data we deduce the characteristic of the solar proton population outside the magnetosphere: apparent source pitch angle distribution rigidity spectrum Propagation in the magnetosphere with PLANETOCOSMICS Flux at the top of the atmosphere Air shower computed with PLANETOCOSMICS Ionisation secondary flux Effective dose January 20, 2005 GLE: The Method

Atmospheric ionisation at 300 g cm -2 at 06:57 on January 20 th, 2005

Permises Interdites ENDF This work Flux of neutrons on Mars (-47.8 N and 174 E) induced by galactic cosmic ray protons at solar minimum

Contribution of different particle types to Ambient equivalent dose on Mars Permises Interdites ENDF This work

10 MeV e - in the most magnetized region of Mars Permises Interdites ENDF This work

Permises Interdites ENDF This work Magnetic shielding on Mars at N and 174 E 10 MeV protons 1 10 MeV e - Tracking of 10 7 downward mono-energetic particles starting at 300 km altitude Detection of number of particles that hits the ground in function of position

Laurent Desorgher18 Mercury Soil + Dipole B0= 300 nT 10 GeV protons from dayside e- >1 MeV e+ > 1 MeV proton > 10 MeV

Quasi trapped e - in Mercury dipole Gurtner et al, 2006

Effective Vertical Cut-off Rigidity at Jupiter Gurtner et al, 2006 Effective Vertical Cut-off Rigidity at Jupiter

Radiations at Europa (~9.4 R j ) Gurtner et al, 2006

Dose in Europa soil (ice) Gurtner et al, 2006

More informations on Gurtner et al, 2005 cosray.unibe.ch/~laurent/planetocosmics