Synchrotron Frequency

From AstroBaki
Revision as of 12:48, 15 December 2015 by C207 (talk | contribs)
(diff) ← Older revision | Latest revision (diff) | Newer revision → (diff)
Jump to navigationJump to search

Synchrotron Characteristic Frequency

Suppose you are observing an emitting synchrotron radiation. Since radiation is just being emitted forward by the , you won’t see radiation from the electron very often. In fact, you’ll just see it once per revolution. Each time you do see it, you will see a spike in power. We’d like to figure out long in time these pulses are separated. To do this, we have the following equations for relativistic motion:

Now and . There are also contributions of the self-interaction of the electron’s field with the electron, but we’ll neglect these as being a minor perturbation. Then:

Let’s define to be the “pitch angle” between and (that is, the angle which makes the travel in a helix instead of a circle). Then:

where is the projected radius of orbit, looking down on . Thus:

The time to make an orbit is , neglecting radiation reactions, so:

Photons Chasing Photons

The photons emitted by the are being squished together by the fact that the is itself moving close to the speed of light. If some is spiraling around, there is only a tiny arc over which the emits photons that we can see. We would like to calculate this arc in order to figure the width of the pulse of radiation an observer sees from synchrotron radiation. The width of the arc over which the emits radiation that we see (as the electron sweeps its beam past us) is just the width of the beam that the emits, which is . The time interval over which this arc is swept out is determined by the time it takes the to travel an angle of around the circle. However, we can also calculate this by noting that the change in v over the interval must come from the acceleration of the field:

Now , so:

Finishing Synchrotron Characteristic Frequency

In computing the time width of the pulses received from an emitting synchrotron radiation, we first measure the time during which the electron emits radiation toward the observer (starting at some initial point 1 and finishing at point 2):

However, during the time the electron was emitting this radiation, it was also moving toward us, so we receive these photons in a shorter burst than they were emitted at. The difference in the actual physical length of the emission goes from being to (we assume that for the duration of the emission, the is going approximately straight at you). Thus we can get the actual time width of the pulse:

For , , so:

This factor of comes from the following:

Using , we can deduce the synchrotron frequency. We’ve just done an approximate computation here. Rybicki & Lightman do it for real and get