344 Cosmic synchrotron radiation In the year 1054 the Chinese and Japanese civilizations were among the most advanced in the world; they were conscious of the external universe and they recorded, most remarkably, an explosive bright star in that year. (It is amazing that none of the European monks, writing all the books of the middle ages, even bothered to write that a star exploded in the sky, but they did not. )Today we may take a picture of that star, and what we see is shown in Fig 34-7. On the outside is a big mass of red filaments, which is produced by the atoms of the thin gas ringing"at their natural frequencies; this makes a bright line spectrum with different frequencies in it. The red happens in this case to be due to nitrogen.On the other hand, in the central region is a mysterious, fuzzy patch of light in a continuous distribution of frequency, i. e,, there are no special frequencies associated with particular atoms. Yet this is not dust"lit up "by nearby stars, which is one way by which one can get a continuous spectrum. We can see stars through it, so it is transparent, but it is emitting light In Fig. 34-8 we look at the same obj light in a region of th which has no bright spectral line, so that we see only the central region. But in this case, also, polarizers have been put on the telescope, and the two views correspond to two orientations 90 apart. We see that the pictures are different! That is to say, the light is polarized. The reason, presumably, is that there is a local magnetic field and many very energetic electrons are going around in that magnetic field We have just illustrated how the electrons could go around the field in a circle We can add to this, of course, any uniform motion in the direction of the field, since the force, v x B, has no component in this direction and, as we have already remarked, the synchrotron radiation is evidently polarized in a direction at right angles to the projection of the magnetic field onto the plane of sight. Putting these two facts together, we see that in a region where one picture bright and the other one is black, the light must have its electric field completely polarized in one direction. This means that there is a magnetic field at right angles to this direction, while in other regions, where there is a strong emission in the other picture, the magnetic field must be the other way. If we look carefully at Fig 34-8, we may notice that there is, roughly speaking, a general set of"lines"that go one way in one picture and at right angles to this in the other. The pictures show a kind of fibrous structure. Presumably, the magnetic field lines will tend to extend rela tively long distances in their own direction, and so, presumably, there are long Fig. 34-8. The crab nebula as seen regions of magnetic field with all the electrons spiralling one way, while in another through a blue filter and a polaroid )Electric vector vertical. b)Electric egion the field is the other way and the electrons are also spiralling that way vector horizontal What keeps the electron energy so high for so long a time? After all, it is 900 ears since the explosion-how can they keep going so fast? How they maintain their energy and how this whole thing keeps going is still not thoroughly understood We shall next remark briefly on one other interesting effect of a very fast- noving particle that radiates energy. The idea is very similar to the one we have just discussed. Suppose that there are charged particles in a piece of matter and .Nucleus-ae a very fast electron, say, comes by(Fig. 34-9). Then, because of the electric field around the atomic nucleus the electron is pulled accelerated, so that the curve of its motion has a slight kink or bend in it. If the electron is travelling at very nearly the speed of light, what is the electric field produced in the direction c? Remember our rule: we take the actual motion translate it back wards at speed c, Fig. 34-9. a fast electron and that gives us a curve whose curvature measures the electric field. It was coming radiates energy in the toward us at the speed u, so we get a backward motion, with the whole direction of its motion compressed into a smaller distance in proportion as c-v is smaller than c. So if I-v/c< 1, there is a very sharp and rapid curvature at B, and when we take he second derivative of that we get a very high field in the direction of the motion So when very energetic electrons move through matter they spit radiation in a for ward direction. This is called bremsstrahlung. As a matter of fact, the synchrotron