low energy electromagnetic physics
DESCRIPTION
Budker Inst. of Physics IHEP Protvino MEPHI Moscow Pittsburg University. Low Energy Electromagnetic Physics. Maria Grazia Pia INFN Genova S. Chauvie, A. De Angelis, G. Depaola, R. Giannitrapani, A. S. Howard, V. Ivanchenko, F. Longo, F. Marchetto, R. Nartallo, P. Nieminen, M.G. Pia, - PowerPoint PPT PresentationTRANSCRIPT
Maria Grazia Pia, INFN Genova
Low Energy Electromagnetic PhysicsLow Energy Electromagnetic Physics
Maria Grazia PiaINFN Genova
S. Chauvie, A. De Angelis, G. Depaola, R. Giannitrapani, A. S. Howard, V. Ivanchenko, F. Longo, F. Marchetto, R. Nartallo, P. Nieminen, M.G. Pia,
G. Santin, A. Solanoon behalf of the Geant4 LowE Electromagnetic Working Group
Budker Inst. of PhysicsIHEP ProtvinoMEPHI Moscow Pittsburg University
ESTECESTEC, 13-15 June 2001
http://www.ge.infn/geant4/lowE
Maria Grazia Pia, INFN Genova
ESA Space Environment & Effects Analysis Section
X-Ray Surveys of Asteroids and Moons
Induced X-ray line emission:indicator of target composition(~100 m surface layer)
Cosmic rays,jovian electrons
Geant3.21
ITS3.0, EGS4
Geant4
Solar X-rays, e, p
Courtesy SOHO EIT
C, N, O line emissions included
How the project started
BepiColombo mission to Mercury
Maria Grazia Pia, INFN Genova
How it evolved
Low energy models (250 eV to 100 GeV) for electrons and photons, based on the LLNL database
Extensions to lower energies foreseen Alternative models foreseen Models for positrons foreseen
Low energy models for positive charged hadrons Ziegler and ICRU databases and parametrisations
Low energy models for negative charged hadrons Unique to Geant4 Based on experimental data (where available) + theoretical model
Low energy models for positive charged ions Negative ions foreseen
Polarised models Compton already implemented, other in progress
Maria Grazia Pia, INFN Genova
Low energy e.m. extensions
Fundamental for space and medical applications, neutrino experiments, antimatter spectroscopy etc.
Low energy hadrons and ions models based on Ziegler and ICRU data and parameterisations
Barkas effect:models for antiprotons
e, down to 250 eV (positrons in progress)