Does overall thermal equilibrium exist between ions and electrons in a weakly collisional, magnetized, turbulent plasma? And, if not, how is thermal energy partitioned between ions and electrons? This is a fundamental question in plasma physics, the answer to which is also crucial for predicting the properties of far-distant astronomical objects such as accretion disks around black holes. In the context of disks, this question was posed nearly two decades ago and has since generated a size-able literature. Here we provide the answer for the case in which energy is injected into the plasma via Alfvénic turbulence: Collisionless turbulent heating typically acts to disequilibrate the ion and electron temperatures. Numerical simulations using a hybrid fluid-gyrokinetic model indicate that the ion–electron heating-rate ratio is an increasing function of the thermal-to-magnetic energy ratio, β i : It ranges from ∼0.05 at β i = 0.1 to at least 30 for β i & 10. This energy partition is approximately insensitive to the ion-to-electron temperature ratio T i /Te. Thus, in the absence of other equilibrating mechanisms, a collisionless plasma system heated via Alfvénic turbulence will tend toward a nonequilib-rium state in which one of the species is significantly hotter than the other, i.e., hotter ions at high β i and hotter electrons at low β i . Spectra of electromagnetic fields and the ion distribution function in 5D phase space exhibit an interesting new magnetically dominated regime at high β i and a tendency for the ion heating to be mediated by nonlinear phase mixing (“entropy cascade”) when β i . 1 and by linear phase mixing (Landau damping) when β i 1.
|Number of pages||6|
|Journal||Proceedings of the National Academy of Sciences of the United States of America|
|Publication status||Published - 2019 Jan 15|
- Accretion flows
- Particle heating
- Plasma turbulence
ASJC Scopus subject areas