Astrophysical jets and solar loops in the lab

Physics Today ◽

10.1063/1.4796245 ◽

2010 ◽

Vol 63 (5) ◽

pp. 21-21

Author(s):

Stephen G. Benka

Keyword(s):

Astrophysical Jets ◽

Solar Loops

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Complex astrophysical experiments relating to jets, solar loops, and water ice dusty plasma

Journal of Plasma Physics ◽

10.1017/s0022377815000604 ◽

2015 ◽

Vol 81 (5) ◽

Cited By ~ 5

Author(s):

P. M. Bellan ◽

X. Zhai ◽

K. B. Chai ◽

B. N. Ha

Keyword(s):

Plasma Jets ◽

Lateral Acceleration ◽

Astrophysical Jets ◽

Water Ice ◽

Weakly Ionized ◽

Solar Loops ◽

Vertically Aligned ◽

Rayleigh Taylor Instability ◽

Plasma Loop ◽

Kink Instability

Recent results of three astrophysically relevant experiments at Caltech are summarized. In the first experiment magnetohydrodynamically driven plasma jets simulate astrophysical jets that undergo a kink instability. Lateral acceleration of the kinking jet spawns a Rayleigh–Taylor instability, which in turn spawns a magnetic reconnection. Particle heating and a burst of waves are observed in association with the reconnection. The second experiment uses a slightly different setup to produce an expanding arched plasma loop which is similar to a solar corona loop. It is shown that the plasma in this loop results from jets originating from the electrodes. The possibility of a transition from slow to fast expansion as a result of the expanding loop breaking free of an externally imposed strapping magnetic field is investigated. The third and completely different experiment creates a weakly ionized plasma with liquid nitrogen cooled electrodes. Water vapour injected into this plasma forms water ice grains that in general are ellipsoidal and not spheroidal. The water ice grains can become quite long (up to several hundred microns) and self-organize so that they are evenly spaced and vertically aligned.

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A Study of Mechanisms Producing Astrophysical Jets.

10.21236/ada194100 ◽

1988 ◽

Author(s):

Kenneth C. Turner

Keyword(s):

Astrophysical Jets

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Instabilities in Three‐dimensional Simulations of Astrophysical Jets Crossing Tilted Interfaces

The Astrophysical Journal ◽

10.1086/305099 ◽

1998 ◽

Vol 493 (1) ◽

pp. 81-90 ◽

Cited By ~ 15

Author(s):

Jagbir S. Hooda ◽

Paul J. Wiita

Keyword(s):

Three Dimensional ◽

Astrophysical Jets ◽

Three Dimensional Simulations

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The content of astrophysical jets

Astronomische Nachrichten ◽

10.1002/asna.202113989 ◽

2021 ◽

Author(s):

Gustavo E. Romero

Keyword(s):

Astrophysical Jets

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Study of relativistic magnetized outflows with relativistic equation of state

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2101 ◽

2019 ◽

Vol 488 (4) ◽

pp. 5713-5727

Author(s):

Kuldeep Singh ◽

Indranil Chattopadhyay

Keyword(s):

Magnetic Field ◽

Angular Momentum ◽

Equation Of State ◽

Polar Angle ◽

Relativistic Equation ◽

Azimuthal Velocity ◽

Astrophysical Jets ◽

Composition Parameter ◽

Field Lines ◽

Flow Experiences

ABSTRACT We study relativistic magnetized outflows using relativistic equation of state having variable adiabatic index (Γ) and composition parameter (ξ). We study the outflow in special relativistic magnetohydrodynamic regime, from sub-Alfvénic to super-fast domain. We showed that, after the solution crosses the fast point, magnetic field collimates the flow and may form a collimation-shock due to magnetic field pinching/squeezing. Such fast, collimated outflows may be considered as astrophysical jets. Depending on parameters, the terminal Lorentz factors of an electron–proton outflow can comfortably exceed few tens. We showed that due to the transfer of angular momentum from the field to the matter, the azimuthal velocity of the outflow may flip sign. We also study the effect of composition (ξ) on such magnetized outflows. We showed that relativistic outflows are affected by the location of the Alfvén point, the polar angle at the Alfvén point and also the angle subtended by the field lines with the equatorial plane, but also on the composition of the flow. The pair dominated flow experiences impressive acceleration and is hotter than electron–proton flow.

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