Solar proton events originate from three main sources: 1) impulsive solar flares that accelerate particles at the flare site, 2) coronal mass ejections that produce variable intensity solar energetic particle events, and 3) solar wind processes like shocks that can further accelerate particles. These events impact the ionosphere in three stages - first solar flare photons ionize the dayside atmosphere, then CME shocks accelerate and precipitate particles into the polar atmospheres, and finally CME sheath compression causes dayside auroras while the sheath and magnetic cloud interact with the dayside magnetosphere. Data on solar proton fluxes across energy bands is obtained from the GOES mission and downloaded from the NOAA website.

1. Solar Proton Events
ASLAM A .M

2. What is a Particle Events?

3. Origin?
 Three SEP Origin:
 1. Impulsive flares particles accelerate to higher energies
at the flare site itself presumably by magnetic
reconnection.
 2. ICMEs produce SEPs :have highly variable intensity–
time profiles that are different from the flare-related particle
signatures
 3.Solar wind processes can also form shocks and
accelerate energetic particles in to higher energies besides
the ICME shocks

4. THE TIME SEQUENCE OF SFEs ON THE
IONOSPHERE
(a) solar flare photon ionization
of the subsolar dayside
atmosphere. Flare particles
precipitate into the polar
atmosphere.
(b) ICME shock particle
acceleration and precipitation
into the polar atmospheres.
(c)ICME shock/sheath
compression of the dayside
magnetosphere causing dayside
auroras, ICME sheath/ MC

5. DATA AND SOURCES
GOES mission measures the solar proton flux in seven different energy
bands ranging from 0.8 MeV-500 MeV (0.8-4 MeV, 4-9 MeV, 9-15 MeV,
15-40 MeV, 40-80 MeV, 80-165 MeV, 165-500 MeV).
GOES particle flux with five minute time resolution. The downloaded raw
data from the URL http://spidr.ngdc.noaa.gov/ was then processed by
filtering the missing values and bad data points, to obtain the final usable

6. Thank You