Maximum Brightness Temperature of an Incoherent Synchrotron Source : Inverse Compton Limit - a Misnomer

TL;DR

The paper argues that the commonly cited inverse Compton limit of ~10^{12} K for synchrotron sources is a misnomer, and the actual physical limit is around 10^{11} K due to equipartition constraints, not inverse Compton effects.

Contribution

It clarifies that the brightness temperature limit is governed by equipartition, not inverse Compton effects, challenging the traditional understanding.

Findings

Brightness temperature limit is about 10^{11} K due to equipartition.

Extreme deviations from equipartition require unrealistic energy changes.

VLBI observations do not show brightness temperatures exceeding 10^{11} K.

Abstract

We show that an upper limit of ~ 10^{12} K on the peak brightness temperature for an incoherent synchrotron radio source, commonly referred to in the literature as an inverse Compton limit, may not really be due to inverse Compton effects. We show that a somewhat tighter limit T_{eq} ~ 10^{11} is actually obtained for the condition of equipartition of energy between radiating particles and magnetic fields which happens to be a configuration of minimum energy for a self-absorbed synchrotron radio source. An order of magnitude change in brightness temperature from T_{eq} in either direction would require departures from equipartition of about eight orders of magnitude, implying a change in total energy of the system up to ~ 10^{4} times the equipartition value. Constraints of such extreme energy variations imply that brightness temperatures may not depart much from T_{eq}. This is supported by the fact that at the spectral turnover, brightness temperatures much lower than ~ 10^{11} K are also not seen in VLBI observations. Higher brightness temperatures in particular, would require in the source not only many orders of magnitude higher additional energy for the relativistic particles but also many order of magnitude weaker magnetic fields. Diamagnetic effects do not allow such extreme conditions, keeping the brightness temperatures close to the equipartition value, which is well below the limit where inverse Compton effects become important.