CASI_STUDIO

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Figura 1: The energy loss spectrum of the May 17th, 2012 SPE (as seen on board the ISS by ALTEA detector), integrated over the polar passages, is shown in comparison with a reference period of quiet sun (April 20th–May 16th). Both spectra are normalized by the effective time of detector acquisition, by the geometrical factor and by the energy loss unit.

Figura 2: Active regions AR11429 and AR11430 as observed by SDO imagers around the March 7th event: (a) SDO/HMI Continuum; (b) SDO/ HMI Magnetogram; (c) SDO/AIA 335 A ̊ ; [d] SDO/AIA 171 A ̊ .

CASI_STUDIO_PAR_3

CASI_STUDIO_PAR_4

Figura 3: GOES proton data (above) and ALTEA data below, during the December 13th, 2006 SPE. The different component and modulation of the ALTEA measurements are marked. On the bottom right a typical day in a quite period to enlarge the south - north poles asymmetry.

Figura 4: Proton and helium absolute fluxes as measured by PAMELA for the SEP event on 14 December 2006.

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CASI_STUDIO_PAR_6

Figura 5: Time profile of the geomagnetic cutoff latitudes measured by PAMELA, for different rigidity bins (color code). The vertical lines mark the beginning of the storm initial, main and recovery phases, respectively.

Figura 6: (Top) PAMELA’s pitch angle distribution (background subtracted) in three rigidity ranges. The curves through the data are meant to guide the eye. Also shown is the world-wide neutron monitor pitch angle distribution averaged between 0158 and 0220 UT.

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