(Files in red–history)
28. Aurora Origin
28a. Plus and Minus
29. Low Polar Orbit
30. Magnetic Storms
30.a Chicago Aurora
31. Space Weather
32. Magnetic planets
33. Cosmic Rays
34. Energetic Particles
35. Solar fast Particles
Starting in 1942, Geiger counters and other detectors, set up to monitor cosmic rays, have occasionally seen sudden increases in the intensity of the radiation, associated with outbursts on the Sun, mostly with visible flares. The cosmic ray intensity returns to normal within minutes or hours, as the acceleration process ends and as accelerated ions disperse throughout interplanetary space.
On the scale of cosmic radiation, solar-produced ions have relatively low energies, generally below 1 Gev (=billion electron volts) and rarely above 10 Gev. That is why such events are often missed by cosmic ray detectors near the equator, where the lowest energies are excluded by the Earth's magnetic field. The best detectors for observing solar particles are therefore those sensitive to the lowest energies of the cosmic radiation.
In many events the Sun emits enormous numbers of lower-energy ions, with no more than tens of Mev (=millions electron volts). The Earth's magnetic field diverts them to the vicinity of the magnetic poles, where they may temporarily smother the ionosphere and interfere with radio communications. Such "polar cap blackouts" used to bother US military radar installations which scanned the polar cap for hostile missiles.
|Electrons are also accelerated by solar events, though to lower energies. Since electrons are much lighter than positive ions, they are more tightly held by the Sun's magnetic field lines. They are also more likely to lose energy in the form of radio waves, x-rays and gamma rays (the same as magnetospheric electrons). Thus they often do not escape, but their presence is indicated by other emissions, e.g. the bright x-rays seen by Yohkoh. Solar acceleration events are often accompanied by bursts of x-rays, sometimes reaching their peak intensity within seconds and thus suggesting an equally abrupt acceleration process. The GOES monitoring satellites of US National Oceanic and Atmospheric Administration (NOAA), observing the weather from synchronous orbit, also keep tabs on the Sun's activity by means of sensitive x-ray detectors.|
Where and How?
While searching for an explanation of particle acceleration on the Sun, British researchers in the 1950s, in particular Peter Sweet and James Dungey, proposed the idea of magnetic reconnection, an idea later applied to the Earth's magnetosphere and to substorms. Reconnection is still believed to be the energy source of flares and CMEs, but unfortunately, it seems to happen in the lower corona, where magnetic structures are invisible (with a few exceptions--see picture below). The nature of substorms and solar acceleration events may indeed be similar, though their scales differ greatly. However, satellites can be sent to substorms but not to the Sun, and therefore magnetospheric research may well hold clues to some of the problems of solar physics.
Theorists have proposed that reconnection and acceleration on the Sun occur
near the tops of magnetic "arches," of field lines rising from sunspot regions,
like the one pictured above. When the Solar Maximum Mission in 1981 spotted on the Sun's surface two bright pin-point sources of x-rays, appearing at the
beginning of an acceleration event, it was widely assumed that they marked the impact of beams of electrons accelerated at the top of an "arch" and guided by its field lines down to the Sun. More recently, the Japanese x-ray imager
aboard the Yohkoh satellite has observed a bright x-ray source formed at the top of an arch (picture on right), lending further support to the theory.|
| Flare seen in X-rays by Yohkoh.|
Should we Worry?
Author and Curator: Dr. David P. Stern
Mail to Dr.Stern: education("at" symbol)phy6.org
Co-author: Dr. Mauricio Peredo
Spanish translation by J. Méndez