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Solar Mass Ejections
Ejecciones de masa solar (Videos)
In this experience, we will learn what Sun storms are and how they can affect our daily life.
The material for the classroom before coming to ESAC can be divided into two categories:
Like other stars, the Sun is a ball of hot (millions of Celsius degrees) gas (91% Hydrogen and 9% Helium) held by gravitational forces. The Sun is in an equilibrium of being pulled together by its own gravitational force and pushed apart by the energy released by thermonuclear reactions in its core.
The Sun and other stars shine because of this thermonuclear energy produced in the core. On the contrary, the planets are bright just by reflection of the sunlight.
As most stars, the Sun has magnetic fields where its plasma from the convective zone circulates in loops that are visible from the surface. Sometimes these loops break, creating "flares" and a shower of charged particles leaves the loop and travels through the Solar System.
We are very lucky that the Earth is shielded by the Van Allen Belts. They protect us from these solar storms which is not the case for example for Venus, which may be one of the reasons why there is no life there.
Some of the ionized particles from the solar storms are caught by our magnetic fields. Close to the N-S poles, where the magnetic poles are, these particles ionize the atmosphere in such a way that wonderful Auroras are seen, such as in this very nice picture.
Our Sun has been studied not only by solar telescopes placed on the Earth but also from satellites sent to space. Since 1995 a cooperative ESA & NASA mission called SOHO has been studying the Sun.
There is a new ESA mission, Solar Orbiter, that is currently under development at ESAC. It will be launched in 2018 to study the Sun and its effects on the Earth. It will also analyze data from the sun's poles for the first time.
Are you ready to learn more about our closest star?