Storms of solar radiation
ShareStorms of solar radiation
The storms of solar radiation occur when an eruption magnetic large-scale, often causing a mass ejection cme and a solar flare associated with it, accelerates the charged particles in the solar atmosphere at very high speeds. The particles most important of these are protons that can be accelerated to large fractions of the speed of light.
At these speeds, the protons can traverse the 150 million km from the sun to the Earth in just 10 minutes or less. When they arrive at Earth, the protons moving fast penetrate into the magnetosphere that protects the Earth from charged particles of lower energy. Once inside the magnetosphere, the particles are guided by the magnetic field lines and penetrate into the atmosphere near the north and south poles.
NOAA ranks the storm of solar radiation by using the scale space-based weather from NOAA in a scale of S1 - S5. The scale is based on measurements of proton energy taken by the GOES satellite in orbit geosincrónica. The start of a storm of solar radiation is defined as the time in which the flow of protons to energies of 10 MeV is greater or equal to 10 units of proton flux (1 pfu 1 particle*cm-2*s-1*ster-1).
The end of a storm of solar radiation is defined as the last time that the proton flux of 10 MeV is measured to or above 10 pfu. This definition allows multiple injections from flares and shocks in interplanetary to be covered by a single storm of solar radiation. A storm of solar radiation can persist for periods of time ranging from hours to days.The storms of solar radiation can cause a number of impacts close to the Ground. When the proton energy collide with satellites or humans in space, can penetrate deep into the object with which they collide and cause damage to electronic circuits or DNA biological.
During the storms of solar radiation is more extreme, the passengers and crew of aircraft of high flight in high latitudes may be exposed to risk of radiation. In addition, when the proton energy collide with the atmosphere, ionize the atoms and molecules thus creating free electrons. These electrons create a layer near the bottom of the ionosphere that can absorb radio waves of high frequency (HF) making the radio communication is difficult or impossible.
SWPC currently predicts the probability of occurrence (S1 Minor Radiation Storm) as part of our products of discussion of prognosis and prognosis of 3 days, and emits a warning for an event on S1 or higher than expected; as well as a warning for when it is expected that the level of protons of 100 MeV scope 1 pfu. In addition, SWPC issues alerts when it reaches each level radiation storm scale space-based weather NOAA (S1-S5) and/or when the protons of 100 MeV reached 1 pfu.
At these speeds, the protons can traverse the 150 million km from the sun to the Earth in just 10 minutes or less. When they arrive at Earth, the protons moving fast penetrate into the magnetosphere that protects the Earth from charged particles of lower energy. Once inside the magnetosphere, the particles are guided by the magnetic field lines and penetrate into the atmosphere near the north and south poles.
The end of a storm of solar radiation is defined as the last time that the proton flux of 10 MeV is measured to or above 10 pfu. This definition allows multiple injections from flares and shocks in interplanetary to be covered by a single storm of solar radiation. A storm of solar radiation can persist for periods of time ranging from hours to days.The storms of solar radiation can cause a number of impacts close to the Ground. When the proton energy collide with satellites or humans in space, can penetrate deep into the object with which they collide and cause damage to electronic circuits or DNA biological.
During the storms of solar radiation is more extreme, the passengers and crew of aircraft of high flight in high latitudes may be exposed to risk of radiation. In addition, when the proton energy collide with the atmosphere, ionize the atoms and molecules thus creating free electrons. These electrons create a layer near the bottom of the ionosphere that can absorb radio waves of high frequency (HF) making the radio communication is difficult or impossible.
SWPC currently predicts the probability of occurrence (S1 Minor Radiation Storm) as part of our products of discussion of prognosis and prognosis of 3 days, and emits a warning for an event on S1 or higher than expected; as well as a warning for when it is expected that the level of protons of 100 MeV scope 1 pfu. In addition, SWPC issues alerts when it reaches each level radiation storm scale space-based weather NOAA (S1-S5) and/or when the protons of 100 MeV reached 1 pfu.
Keywords: radiation, solar, protons, storm, proton, scale, high, particles, energy, pfu, MeV, time, Earth, atmosphere, collide, NOAA, penetrate, storms, near, magnetosphere
