3D Magneto-hydrodynamic simulations of Parker instability with cosmic rays

Lo, Yu-Tsung; Ko, C. M.; Wang, Chih Yueh

doi:10.1016/j.cpc.2010.04.019

Cited by 11 publications

(4 citation statements)

References 9 publications

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“…Cosmic rays can play a dynamical role in the structure and evolution of the interstellar as well as intergalactic medium. For instances, from the hydrodynamic perspective, cosmic rays can affect instabilities, such as, Parker instability, Jeans instability, magnetorotional instability (e.g., Parker 1969Parker , 1966Hanasz & Lesch 2000Ryu et al 2003;Kuwabara et al 2004;Kuwabara & Ko 2006;Ko & Lo 2009;Lo et al 2011;Kuwabara & Ko 2015;Heintz & Zweibel 2018;Heintz et al 2020;Kuwabara & Ko. 2020), and they can modify structures and outflows (e.g., Ko et al 1991;Yang et al 2012;Girichidis et al 2016;Dorfi & Breitschwerdt 2012;Recchia et al 2016;Ruszkowski et al 2017;Mao & Ostriker 2018;Farber et al 2018;Holguin et al 2019;Dorfi et al 2019;Yu et al 2020;Recchia 2020;Ramzan et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Outflows in the presence of cosmic rays and waves with cooling

Ko,

Ramzan,

Chernyshov

2021

Preprint

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Context. Plasma outflow from a gravitational potential well with cosmic rays and self-excited Alfvén waves with cooling and wave damping is studied in the hydrodynamics regime. Aims. We study outflows in the presence of cosmic ray and Alfvén waves including the effect of cooling and wave damping. We seek physically allowable steady-state subsonic-supersonic transonic solutions. Methods. We adopted a multi-fluid hydrodynamical model for the cosmic ray plasma system. Thermal plasma, cosmic rays, and self-excited Alfvén waves are treated as fluids. Interactions such as cosmic-ray streaming instability, cooling, and wave damping were fully taken into account. We considered one-dimensional geometry and explored steady-state solutions. The model is reduced to a set of ordinary differential equations, which we solved for subsonic-supersonic transonic solutions with given boundary conditions at the base of the gravitational potential well. Results. We find that physically allowable subsonic-supersonic transonic solutions exist for a wide range of parameters. We studied the three-fluid system (considering only forward-propagating Alfvén waves) in detail. We examined the cases with and without cosmic ray diffusion separately. Comparisons of solutions with and without cooling and with and without wave damping for the same set of boundary conditions (on density, pressures of thermal gas, cosmic rays and waves) are presented. We also present the interesting case of a four-fluid system (both forward-and backward-propagating Alfvén waves are included), highlighting the intriguing relation between different components.

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Section: Introductionmentioning

confidence: 99%

Outflows in the presence of cosmic rays and waves with cooling

Ko,

Ramzan,

Chernyshov

2021

Preprint

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“…The influence of CRs on various instabilities has been studied by means of linear analysis and MHD simulations, for instance, the evolution of Parker instability (Parker 1966;Hanasz 1997;Hanasz & Lesch 2000;Ryu et al 2003;Kuwabara et al 2004;Lo et al 2011), Parker-Jeans instability (Kuznetsov & Ptuskin 1983;Kuwabara & Ko 2006), magneto-rotational instability (Khajenabi 2012), Kelvin-Helmholtz instability (Suzuki et al 2014), and also galactic dynamo (Parker 1992;Hanasz et al 2004Hanasz et al , 2009. The results of these works showed that in some cases the growth rate has some intriguing dependence on the cosmic ray pressure and the coupling of CR and thermal plasma (i.e., the cosmic ray diffusion coefficient).…”

Section: Introductionmentioning

confidence: 99%

Magneto-rotational instability with the effect of cosmic rays

Kuwabara

2015

Proc. IAU

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We present the results obtained from linear stability analysis and 2.5dimensional magnetohydrodynamic (MHD) simulations of the magnetorotational instability (MRI), including the effects of cosmic rays (CRs). We took into account of the CR diffusion along the magnetic field but neglect the cross-field-line diffusion. Two models are considered in this paper: shearing box model and differentially rotating cylinder model. We studied how MRI is affected by the initial CR pressure (i.e., energy) distribution. In the shearing box model, the initial state is uniform distribution. Linear analysis shows that the growth rate of MRI does not depend on the value of CR diffusion coefficient. In the differentially rotating cylinder model, the initial state is a constant angular momentum polytropic disk threaded by weak uniform vertical magnetic field. Linear analysis shows that the growth rate of MRI becomes larger if the CR diffusion coefficient is larger. Both results are confirmed by MHD simulations. The MHD simulation results show that the outward movement of matter by the growth of MRI is not impeded by the CR pressure gradient, and the centrifugal force which acts to the concentrated matter becomes larger. Consequently, the growth rate of MRI is increased. On the other hand, if the initial CR pressure is uniform, then the growth rate of the MRI barely depends on the value of the CR diffusion coefficient.

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“…For instances, in the past couple decades, efforts have been made on the understanding of the influencing of cosmic rays on instabilities related to interstellar medium (such as, Parker instability, Jeans instability, magnetorotional instability, see, e.g. Parker 1966; Corresponding author: C. M. Ko cmko@astro.ncu.edu.tw Kuznetsov & Ptuskin 1983;Hanasz & Lesch 2000Ryu et al 2003;Kuwabara et al 2004;Kuwabara & Ko 2006;Ko & Lo 2009;Lo et al 2011;Kuwabara & Ko 2015;Heintz & Zweibel 2018;Heintz et al 2020); and on cosmic ray modified structures and outflows (e.g., shocks, galactic halo, stellar and galactic winds, see e.g., Drury & Völk 1981;McKenzie & Völk 1982;Ko et al 1997;Ko 2001;Ghosh & Ptuskin 1983;Ko et al 1991;Ko 1991a;Ko et al 1988;Ko 1991b;Ipavich 1975;Zirakashvili et al 1996;Everett et al 2008;Yang et al 2012;Girichidis et al 2016;Recchia et al 2016;Ruszkowski et al 2017;Mao & Ostriker 2018;Farber et al 2018;Holguin et al 2019;Dorfi & Breitschwerdt 2012;Dorfi et al 2019;Yu et al 2020). Especially, in the past ten years or so, there are a lot of attentions on cosmic ray modified galactic wind.…”

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confidence: 99%

Outflows in the presence of cosmic rays and waves

Ramzan,

Ko,

Chernyshov

2020

Preprint

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Plasma outflow or wind against a gravitational potential under the influence of cosmic rays is studied in the context of hydrodynamics. Cosmic rays interact with the plasma via hydromagnetic fluctuations. In the process, cosmic rays advect and diffuse through the plasma. We adopt a multi-fluid model in which besides thermal plasma, cosmic rays and self-excited Alfvén waves are also treated as fluids. We seek possible physically allowable steady state solutions of three-fluid (one Alfvén wave) and fourfluid (two Alfvén waves) models with given the boundary conditions at the base of the potential well. Generally speaking, there are two classes of outflows, subsonic and supersonic (with respect to a suitably defined sound speed). Three-fluid model without cosmic ray diffusion can be studied in the same way as the classic stellar wind problem, and is taken as a reference model. When cosmic ray diffusion is included, there are two categories of solutions. One of them resembles the three-fluid model without diffusion, and the other behaves like thermal wind at large distances when the waves wither and cosmic rays are decoupled from the plasma. We also inspect the effect of wave damping mechanisms (such as, nonlinear Landau damping). Roughly speaking, the effect is much smaller in supersonic outflow than in subsonic outflow.

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3D Magneto-hydrodynamic simulations of Parker instability with cosmic rays

Cited by 11 publications

References 9 publications

Outflows in the presence of cosmic rays and waves with cooling

Outflows in the presence of cosmic rays and waves with cooling

Magneto-rotational instability with the effect of cosmic rays

Outflows in the presence of cosmic rays and waves

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