The source abundances of the cosmic ray elements belonging to the ultra heavy component (those with atomic number over 30) may be calculated from the experimental results obtained in the Earth's neighbourhood by several experiments on board of satellites (Ariel-6, HEAO-3, UHCRE), based on scintillation detectors, Cerenkov counters and plastic track detectors respectively. Our Group has collabaorated on the abundance measurements of ions with atomic number over 65 at energies over 2 GeV/nucleon recorded in the UHCRE, that have been determined with a charge uncertainty around 2 charge units. Introducing relativistic corrections to the expression related to track formation mechanisms should allow to reduce this charge uncertainty. The propagation calculation to the cosmic ray sources of the results obtained using several models (quasi-static, dynamic, as well as based on Monte Carlo methods) that allow to solve the transport equation should lead to charcterise the nuclear astrophysical processes that take place in the sources of the ultra heavy component of cosmic rays. The possibility of collecting new data, with good charge resolution, of cosmic ray elements with atomic number over 30, specially in the region compromised between 30 and 65, prompts us to develop the prototype of an instrument, based on surface barrier Si detectors, that could be shipped in future satellite missions that orbit the Earth in orbits having low inclination with respect to the equatorial plane (MINISAT program).
|Effective start/end date||21/12/97 → 21/12/00|
Explore the research topics touched on by this project. These labels are generated based on the underlying awards/grants. Together they form a unique fingerprint.