Non-resonant Alfvénic instability activated by high temperature of ion beams in compensated-current astrophysical plasmas

• Published in: Astronomy and astrophysics (Berlin) 2018-07, Vol.615, p.A169
• Main Authors: Malovichko, P., Voitenko, Y., De Keyser, J.
• Format: Article
• Language: English
• Subjects: Bulk density; Cosmic rays; Cyclotron frequency; Cyclotrons; Demagnetization; Growth rate; High temperature; instabilities; Ion beams; Ions; ISM: supernova remnants; Kinetic theory; Magnetic fields; Magnetohydrodynamics; Mathematical analysis; plasmas; Plasmas (physics); Proton beams; solar wind; Stability; Stability analysis; Supernova remnants; Supernovae; Temperature dependence; Terrestrial environments; Wave propagation; waves
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201731710

Context. Compensated-current systems are established in response to hot ion beams in terrestrial foreshock regions, around supernova remnants, and in other space and astrophysical plasmas. Aims. We study a non-resonant reactive instability of Alfvén waves propagating quasi-parallel to the background magnetic field B0 in such systems. Methods. The instability is investigated analytically in the framework of kinetic theory applied to the hydrogen plasmas penetrated by hot proton beams. Results. The instability arises at parallel wavenumbers kz that are sufficiently large to demagnetize the beam ions, kzVTb/ωBi ≳ 1 (here VTb is the beam thermal speed along B0 and ωBi is the ion-cyclotron frequency). The Alfvén mode is then made unstable by the imbalance of perturbed currents carried by the magnetized background electrons and partially demagnetized beam ions. The destabilizing effects of the beam temperature and the temperature dependence of the instability threshold and growth rate are demonstrated for the first time. The beam temperature, density, and bulk speed are all destabilizing and can be combined in a single destabilizing factor αb triggering the instability at αb > αbthr α b > α b thr $ \alpha_\text{b}>\alpha_\text{b}^\text{thr} $ , where the threshold value varies in a narrow range 2.43 ≤  αbthr ≤ 4.87 2.43 ≤ α b thr ≤ 4.87 $ 2.43\leq\alpha_\text{b}^\text{thr}\leq4.87 $ . New analytical expressions for the instability growth rate and its boundary in the parameter space are obtained and can be directly compared with observations. Two applications to terrestrial foreshocks and foreshocks around supernova remnants are briefly discussed. In particular, our results suggest that the ions reflected by the shocks around supernova remnants can drive stronger instability than the cosmic rays.