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Dissipation triggers dynamical two-stream instability

Dissipation triggers dynamical two-stream instability
Dissipation triggers dynamical two-stream instability
Two coupled, interpenetrating fluids suffer instabilities beyond certain critical counterflows. For ideal fluids, an energetic instability occurs at the point where a sound mode inverts its direction due to the counterflow, while dynamical instabilities only occur at larger relative velocities. Here we discuss two relativistic fluids, one of which is dissipative. Using linearized hydrodynamics, we show that in this case the energetic instability turns dynamical, i.e., there is an exponentially growing mode, and this exponential growth only occurs in the presence of dissipation. This result is general and does not rely on an underlying microscopic theory. It can be applied to various two-fluid systems for instance in the interior of neutron stars. We also point out that under certain circumstances the two-fluid system exhibits a mode analogous to the r-mode in neutron stars that can become unstable for arbitrarily small values of the counterflow.
gr-qc, astro-ph.HE, hep-ph, physics.plasm-ph
https://www.mdpi.com/2571-712X/2/4/28
457-480
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Schmitt, Andreas
1765159f-255f-45e7-94ea-58c1c883d65f
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Schmitt, Andreas
1765159f-255f-45e7-94ea-58c1c883d65f

Andersson, Nils and Schmitt, Andreas (2019) Dissipation triggers dynamical two-stream instability. Particles, 2 (4), 457-480. (https://www.mdpi.com/2571-712X/2/4/28).

Record type: Article

Abstract

Two coupled, interpenetrating fluids suffer instabilities beyond certain critical counterflows. For ideal fluids, an energetic instability occurs at the point where a sound mode inverts its direction due to the counterflow, while dynamical instabilities only occur at larger relative velocities. Here we discuss two relativistic fluids, one of which is dissipative. Using linearized hydrodynamics, we show that in this case the energetic instability turns dynamical, i.e., there is an exponentially growing mode, and this exponential growth only occurs in the presence of dissipation. This result is general and does not rely on an underlying microscopic theory. It can be applied to various two-fluid systems for instance in the interior of neutron stars. We also point out that under certain circumstances the two-fluid system exhibits a mode analogous to the r-mode in neutron stars that can become unstable for arbitrarily small values of the counterflow.

Full text not available from this repository.

More information

Accepted/In Press date: 18 October 2019
Published date: 31 October 2019
Additional Information: 20 pages, 4 figures, v2: minor changes in the text, references added, version accepted for publication
Keywords: gr-qc, astro-ph.HE, hep-ph, physics.plasm-ph

Identifiers

Local EPrints ID: 440750
URI: http://eprints.soton.ac.uk/id/eprint/440750
DOI: https://www.mdpi.com/2571-712X/2/4/28
PURE UUID: 94a5071d-4a3f-45d5-9b2e-d52dc21f408e
ORCID for Nils Andersson: ORCID iD orcid.org/0000-0001-8550-3843
ORCID for Andreas Schmitt: ORCID iD orcid.org/0000-0003-2858-4450

Catalogue record

Date deposited: 14 May 2020 16:49
Last modified: 16 May 2020 00:46

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