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An astrophysical plasma is a plasma (an ionized gas) found in astronomy whose physical properties are studied in the science of astrophysics. The vast majority of the baryonic matter of the universe is thought to consist of plasma, a state of matter in which atoms and molecules are so hot, that they have ionized by breaking up into their constituent parts, negatively charged electrons and positively charged ions. Although influenced by gravity, because the particles are charged, they are also strongly influenced by electromagnetic forces, that is, by magnetic and electric fields.

All known astrophysical plasmas are magnetic. They also contain equal numbers of electrons and ions so that they are electrically neutral overall. And because plasmas are highly conductive, any charge imbalances are readily neutralised. However, because plasma phenonenon are very complex, charge imbalances can occur, resulting in a characteristic known as quasineutrality. An example is the influence of our Sun's magnetic field on the electrons and ions in the interplanetary medium (or Solar wind) resulting in the heliospheric current sheet, the largest structure in the Solar system.

Characteristics


Space plasma pioneers Hannes Alfvén and Carl-Gunne Fälthammar divided cosmic plasmas into three different categories (note that other characteristics of low-particle-density interstellar and intergalactic plasmas, means that they are characterised as medium density):
Classification of Magnetic Cosmic Plasmas
CharacteristicSpace plasma density categories
(Note that density does not refer to only particle density)
Ideal comparison
High densityMedium DensityLow Density
Criterionλ << ρλ << ρ << lclc << λlc << λD
ExamplesStellar interior
Solar photosphere
Solar chromosphere/corona
Interstellar/intergalactic space
Ionopshere above 70km
Magnetosphere during
magnetic disturbance.
Interplanetary space
Single charges
in a high vacuum
DiffusionIsotropicAnisotropicAnisotropic and smallNo diffusion
ConductivityIsotropicAnisotropicNot definedNot defined
Electric field parallel to B
in completely ionized gas
SmallSmallAny valueAny value
Particle motion in plane
perpendicular to B
Almost straight path
between collisions
Circle
between collisions
CircleCircle
Path of guiding centre
parallel to B
Straight path
between collisions
Straight path
between collisions
Oscillations
(eg. between mirror points)
Oscillations
(eg. between mirror points)
Debye Distance λDλD << lcλD << lcλD << lcλD >> lc
Magnetohydrodynamics
suitability
YesApproximatelyNoNo
λ=Mean free path. ρ= Larmor radius (gyroradius) of electron. λD=Debye length. lc=Characteristic length
Adapted From Cosmical Electrodynamics (2nd Ed. 1952) Alfvén and Fälthammar

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Magnetoconvection in sheared magnetic fields
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H. Abbasi and H. Hakimi Pajouh The satellite observations of the magnetosphere in the low-frequency ion dynamics revealed several facts: (1) localized structures for electric field signal parallel to the magnetic field; (2) anisotropy for the electron velocity distribution such that T<Ion cyclotron instabilities of parallel shear flow of collisional plasma
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