Dissipative Processes and Their Role in the Evolution of Radio Galaxies
Abstract
:1. Introduction
2. Jet Stability
2.1. Why Are Jets Unstable?
- KHI arises due to transition layers (either contact discontinuities or continuous changes) in the velocity component tangential to this layer;
- Rayleigh–Taylor instability (RTI) can grow in expanding/contracting jets, with the equivalent to the gravity acceleration being given by the changes in the radial velocity;
- centrifugal instability (CFI) also grows in expanding jets with non-zero azimuthal velocities;
- CDI arises due to deformations in the toroidal component of the magnetic field, and the so-called pressure-driven instability arises when the magnetic rings that constitute the magnetic structure in the case of toroidal component dominated field are displaced from their equilibrium configuration (under certain magnetic field radial distributions, [71]);
- centrifugal buoyancy is caused by rotation, when the centrifugal force is large enough to bend the magnetic lines;
- MRI can develop in a magnetized, rotating jet with differential rotation (and decreasing angular velocity with radius; see [69]).
- No rotation ():
- Rotation ():
- No rotation ():
- Rotation():
- -
- Centrifugal buoyancy ([94]).
- If , there is no azimuthal dependence and the instability produces axisymmetric oscillations of the jets; produces antisymmetric distributions of the physical parameters that result in helical oscillations; produces elliptical deformations, etc.
- A radial structure with no zeros between the jet axis and its surface (i.e., global changes that do not cross the equilibrium value at any point) corresponds to the surface or fundamental modes, whereas if the radial structure crosses the equilibrium value, the modes are called body or reflection modes, with the number of zeros giving the order (one zero for the first body/reflection mode, and so on).
2.2. The Linear Regime
2.2.1. Hydrodynamical Jets
2.2.2. Magnetized Jets
KHI and CDI
Stability of magnetized, rotating jets
2.3. The Non-Linear Regime (or ’Then, Why Are (Some) Jets So Stable?’)
3. Jet Star/Cloud Interactions
4. Influence of Entrainment on Jet Evolution
5. Discussion
5.1. Mass-Load and Dissipation
- Strong relative mass-load (): in this case, and the conservation equation tells us that the initial jet enthalpy is transferred to the entrained flow.
- Mild relative mass-load (): in this case, could be both smaller than or larger than zero, depending on the value of the terms accounting for deceleration (so the initial jet enthalpy can grow).
- Small relative mass-load (): in this case, we could neglect the source term q in the conservation equation above, and would be left with the Bernoulli expression for adiabatic evolution: , where expansion of a hot jet flow translates into acceleration.
5.2. Jet Evolution: A Summary
5.3. A Final Comment on FRI/FRII Dichotomy and VHE Emission
Funding
Acknowledgments
Conflicts of Interest
References
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1. | I will use throughout the paper. |
2. | The short wavelength pressure-driven (or Z-pinch) instability, which can grow for a particular initial distribution of magnetic field and gas pressure [71] can be taken as a particular type of CDI. |
3. | There are aspects relevant to the parameter space covered by each of the referred papers (e.g., magnetically versus particle dominated, or hot versus cold jets, etc.) that are not taken into account in this list. |
4. | Although there are other optionsi Istomin and Pariev (1994, 1996) [92] consider variations of the field up to the jet radius and set the boundary condition at that point |
5. | Despite this structure is arbitrarilly introduced in the set-up of many simulations and stability analysis, a sheath is probably surrounding the fast jet spines, either from the jet formation region, where a wind can be formed from the accretion disk [109], or because of simple kinetic energy dissipation at the jet-environment shearing layer. |
6. | Please note that the definition of the pitch varies among papers and that it can also be found as . |
7. | |
8. | |
9. | The direct conversion of magnetic energy into internal energy implies dissipative mechanisms beyond an ideal MHD description. |
KHI | ✓ | ✓ | ✓ | − | ✓ | ✓ |
CDI | ✓ | ✓ | ✓ | × | ✓ | ✓ |
RTI/CFI | × | × | − | ✓ | − | × |
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Perucho, M. Dissipative Processes and Their Role in the Evolution of Radio Galaxies. Galaxies 2019, 7, 70. https://doi.org/10.3390/galaxies7030070
Perucho M. Dissipative Processes and Their Role in the Evolution of Radio Galaxies. Galaxies. 2019; 7(3):70. https://doi.org/10.3390/galaxies7030070
Chicago/Turabian StylePerucho, Manel. 2019. "Dissipative Processes and Their Role in the Evolution of Radio Galaxies" Galaxies 7, no. 3: 70. https://doi.org/10.3390/galaxies7030070