2. Semi-analytical formulae
where is the cyclotron frequency, is the emission frequency, s is an integer, is the angle of the wave vector to the magnetic field, is the angle between the velocity of the electron and the magnetic field (the pitch angle), is the refraction index, and and are the usual Lorentz factor and velocity.
The important factor in Eq. 1 is the refraction index for the Ordinary Mode (OM or `+'), and the eXtra-Ordinary mode (XO or `-'). The refraction index is a function of the ambient density, of the cyclotron frequency, of the emission frequency, and of the angle to the magnetic field, and in general is quite complicated.
The resonance condition defines an ellipse on the electron velocity plane for a given s,, and frequency of emission. In the weakly relativistic case this ellipse becomes a circle (Melrose & Dulk 1982), and Melrose and Dulk use this to derive the frequency of largest growth rate. The frequency and angle for which the largest (in absolute value) negative absorption is expected are those for which the resonance circle is tangent to the outer edge of the loss-cone at the loss-cone opening angle (Melrose & Dulk 1982). This definition results in an equation for the frequency where the largest absorption is expected which is:
This equation has two possible forms of a curve. One for , where as approaches 1 from above, the solution goes to minus infinity. The second form is for , where the solution goes to positive infinity as the kinetic energy approaches zero. Both curves go asymptotically to as goes to infinity.
For the fully relativistic case the equivalent curve to the special resonance circle is a curve of the second form which is tangent to the line .
This new approximation is identical with the Melrose and Dulk approximation (Eq. 2) for the case . It is, however, more general and is a good approximation for the frequencies of negative absorption, even when is large.
It is important to note that even though Eq. 4 is a better approximation, it still assumes a single harmonic s while the absorption coefficient includes a sum over some harmonics (Ramaty 1969). As a result, the frequency with largest negative absorption is usually not exactly the solution of Eq. 4, but a frequency close to it.
Our equation includes the refraction index which is a function of the frequency , and also of the ratio between the plasma frequency and the cyclotron frequency . Our approximation is therefore only semi-analytical, and some numerical computation must be made. The computation, however, is very simple and can be performed very quickly.
Some general properties of the solution can be deduced, and in summary they are for the OM and XO mode:
The harmonic number s of a frequency can be derived from the condition 5 and should be the smallest integer which fits the inequality
Since it is reasonable to assume that the smallest harmonic has the largest contribution, it is sufficient to consider it alone for the purposes of the approximation.
There is another magneto-ionic mode, the Z-mode. The Z-mode is the lower branch of the XO mode, for frequencies smaller than
Emission in the Z-mode can not emerge from the plasma, and therefore can not be observed. Since our purpose is to derive estimates for the observable frequencies, approximate solutions for the Z-mode are not of great interest. However, the Z-mode may be the dominant mode and quench the maser before the other modes are amplified. It is therefore of interest to determine where possible negative frequencies can appear.
The condition for negative absorption in the Z-mode is either , or and not too small. Empirically "not too small" translates as .
We compared the Dulk-Melrose approximation, our new approximation, and a numerical calculation of the absorption coefficients from which the frequencies where the absorption is negative was extracted. The results are that for small the Dulk-Melrose approximation(Eq. 2) is very similar to our new approximation. However, for larger , the new approximation is much better. The new approximation is identical with the result of the full numerical computation for most of the range where there is negative absorption.
© European Southern Observatory (ESO) 1999
Online publication: July 16, 1999