|Scientific Frontline® Space Weather Forecast Center|
Continuum | MDI
Magnetogram | LASCO
C2 | LASCO
C3 | EIT
171 | EIT
195 | EIT
284 | EIT
EUVI 195 Behind | COR1 Behind | COR2 Behind | HI1 Behind | HI2 Behind | EUVI 195 Ahead | COR1 Ahead | COR2 Ahead | HI1 Ahead | HI2 Ahead AIA 094 | AIA 131 | AIA 171 | AIA 193 | AIA 211 | AIA 304 | AIA 335 | AIA 1600 | AIA 1700 | AIA 4500
Solar Winds | Solar Flares | NOAA Space Weather Scales | Sunspot Numbers | Interplanetary Magnetic Field
Glossary of Solar-Terrestrial Terms | Solar, Earth Atmospheric and Climate Gallery
Solar flares are tremendous explosions on the surface of the Sun. In a matter of just a few minutes they heat material to many millions of degrees and release as much energy as a billion megatons of TNT. They occur near sunspots, usually along the dividing line (neutral line) between areas of oppositely directed magnetic fields.
Flares release energy in many forms - electro-magnetic (Gamma rays and X-rays), energetic particles (protons and electrons), and mass flows. Flares are characterized by their brightness in X-rays (X-Ray flux). The biggest flares are X-Class flares. M-Class flares have a tenth the energy and C-Class flares have a tenth of the X-ray flux seen in M-Class flares. The National Oceanic and Atmospheric Administration (NOAA) monitors the X-Ray flux from the Sun with detectors on some of its satellites.
Solar flares are often observed using filters to isolate the light emitted by hydrogen atoms in the red region of the solar spectrum (the H-alpha spectral line). Most solar observatories have H-alpha telescopes and some observatories monitor the Sun for solar flares by capturing images of the Sun every few seconds.
The key to understanding and predicting solar flares is the structure of the magnetic field around sunspots. If this structure becomes twisted and sheared then magnetic field lines can cross and reconnect with the explosive release of energy. In the bottom left, to the left the blue lines represent the neutral lines between areas of oppositely directed magnetic fields. Normally the magnetic field would loop directly across these lines from positive (outward pointing magnetic field) to negative (inward pointing magnetic field ) regions. The small line segments show the strength and direction of the magnetic field measured with the MSFC Vector Magnetograph. These lines and line segments overlie an image of a group of sunspots with a flaring region. The flare (the bright area) lies along a section of a neutral line where the magnetic field is twisted (or sheared) to point along the neutral line instead of across it. We have found that this shear is a key ingredient in the production of solar flares.
Source / Credit: NASA