Linear theory of the Rayleigh–Taylor instability at a discontinuous surface of a relativistic flow

Matsumoto, Jin; Aloy, M. Á.; Perucho, M.

doi:10.1093/mnras/stx2012

Cited by 37 publications

(37 citation statements)

References 69 publications

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“…where A is the relativistic Atwood number (Matsumoto et al 2017). Based on this, the growth rate and the critical wavelength of the "relativistic" magnetic RTI in the jet-cocoon system are surmised as follows: The density in equations (26) and (28) Then, the growth rate and critical wavelength of the relativistic magnetic RTI at the jet interface are expected to be…”

Section: Effect Of Magnetic Fieldmentioning

confidence: 99%

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Propagation, cocoon formation, and resultant destabilization of relativistic jets

Matsumoto

Masada

2019

Monthly Notices of the Royal Astronomical Society

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A cocoon is a by-product of a propagating jet that results from shock heating at the jet head. Herein, considering simultaneous cocoon formation, we study the stability of relativistic jets propagating through the uniform ambient medium. Using a simple analytic argument, we demonstrate that independent from the jet launching condition, the effective inertia of the jet is larger than that of the cocoon when the fully relativistic jet oscillates radially owing to the pressure mismatch between jet and cocoon. In such situations, it is expected that the onset condition for the oscillation-induced Rayleigh-Taylor instability is satisfied at the jet interface, resulting in the destabilization of the relativistic jet during its propagation. We have quantitatively verified and confirmed our prior expectation by performing relativistic hydrodynamic simulations in three dimensions. The possible occurrences of the Richtmyer-Meshkov instability, oscillation-induced centrifugal instability and Kelvin-Helmholtz instability are also discussed.

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Section: Effect Of Magnetic Fieldmentioning

confidence: 99%

“…The linear theory of RTI at a discontinuous surface of relativistic flows is addressed in Matsumoto et al (2017). The onset condition is given analytically by…”

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confidence: 99%

Propagation, cocoon formation, and resultant destabilization of relativistic jets

Matsumoto

Masada

2019

Monthly Notices of the Royal Astronomical Society

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“…2). In particular, in reference [81], the authors develop the linear analysis and confirm the prediction given by [80] about the stability condition…”

Section: Hydrodynamical Jetsmentioning

confidence: 73%

“…The requirement of small-scale instabilities that can explain the way in which FRI jets decelerate along the first kiloparsecs [27] has brought the attention of theorists upon the possibility that the RTI or the CFI develop in expanding jets. Different authors have studied the development of Rayleigh-Taylor instability in jets undergoing expansion and recollimation ( [80][81][82], see Fig. 2).…”

Section: Hydrodynamical Jetsmentioning

confidence: 99%

Dissipative Processes and Their Role in the Evolution of Radio Galaxies

Perucho

2019

Galaxies

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Particle acceleration in relativistic jets, to very high levels of energy, occurs at the expense of the dissipation of magnetic or kinetic energy. Therefore, understanding the processes that can trigger this dissipation is key to the characterization of the energy budgets and particle acceleration mechanisms in action in active galaxies. Instabilities and entrainment are two obvious candidates to trigger dissipation. On the one hand, supersonic, relativistic flows threaded by helical fields, as expected from the standard formation models of jets in supermassive black-holes, are unstable to a series of magnetohydrodynamical instabilities, such as the Kelvin–Helmholtz, current-driven, or possibly the pressure-driven instabilities. Furthermore, in the case of expanding jets, the Rayleigh–Taylor and centrifugal instabilities may also develop. With all these destabilizing processes in action, a natural question is to ask how can some jets keep their collimated structure along hundreds of kiloparsecs. On the other hand, the interaction of the jet with stars and clouds of gas that cross the flow in their orbits around the galactic centers provides another scenario in which kinetic energy can be efficiently converted into internal energy and particles can be accelerated to non-thermal energies. In this contribution, I review the conditions under which these processes occur and their role both in jet evolution and propagation and energy dissipation.

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“…From the results summarised in this paper, currently favoured scenarios to explain jet deceleration are either the growth of small scale instabilities [14,15,16], stellar mass-load (e.g., [9,36]), or a combination of both. In reference [5], the authors show that deceleration seems to occur from the boundaries to the axis in some cases, and more homogeneously in other sources.…”

Section: Final Remarksmentioning

confidence: 97%

Radio source evolution and the interplay with the host galaxy

Perucho¹

2019

Proceedings of International Conference on Black Holes as Cosmic Batteries: UHECRs and Multimessenger Astronomy — PoS(BHCB2018)

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There is compelling evidence showing that extragalactic jets are a crucial ingredient in the evolution of host galaxies and their environments. Extragalactic jets are well collimated and relativistic, both in terms of thermodynamics and kinematics at sub-parsec and parsec scales. They generate strong shocks in the ambient medium, associated with observed hotspots in FRII radio galaxies, and carve cavities that are filled with the shocked jet flow, dragging a large fraction of the interstellar gas along, in the form of slow, massive outflows within the host galaxies. In this paper, I discuss relevant processes associated to jet evolution in the frame of FRI-FRII dichotomy. In particular, I focus on the role of 1) the interaction between galactic atmospheres and the jet head on global FRII jet kinematics, and 2) mass load by stellar winds or small-scale instabilities on jet deceleration in FRI jets. The results presented are based on 3D relativistic hydrodynamical (RHD) and/or 2D axisymmetric, time-independent relativistic magnetohydrodynamical (RMHD) simulations.

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Linear theory of the Rayleigh–Taylor instability at a discontinuous surface of a relativistic flow

Cited by 37 publications

References 69 publications

Propagation, cocoon formation, and resultant destabilization of relativistic jets

Propagation, cocoon formation, and resultant destabilization of relativistic jets

Dissipative Processes and Their Role in the Evolution of Radio Galaxies

Radio source evolution and the interplay with the host galaxy

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