等离子体_等离子体清洗

2024-08-09 04:57:29

1.什么是等离子体？火焰是等离子体吗？

2.什么是等离子态？

3.等离子体简介

4.等离子体中主要基元反应过程

等离子体_等离子体清洗

将固体加热到熔点时,粒子的平均动能超过晶格的结合能,固体会变成液体；

将液体加热到沸点时,粒子的动能会超过粒子之间的结合能,液体会变成气体.

如果把气体进一步加热,气体则部分电离或完全电离,即原子的外层电子会摆脱原子核的束缚成为自由电子,而失去外层电子的原子变成离子.当带电粒子的比例超过一定程度时,电离气体凸现出明显的电磁性质,而其中的正离子和负离子（电子）的数目相等,因此被称为等离子体（plasma),又叫物质的第四态.

等离子体是处于等离子态的物质的总称,当然不是热量.

空气是气体,不是等离子体.但是空气中是存在少量电离的离子的.

本人是等离子体专业的研究生,上述内容准确可靠.

参考资料：

《等离子体物理学》（高教）

什么是等离子体？火焰是等离子体吗？

等离子体

维基百科，自由的百科全书

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等离子灯

放大

等离子灯

等离子体（等离子态，电浆，英文：Plasma）是一种电离的气体，由于存在电离出来的自由电子和带电离子，等离子体具有很高的电导率，与电磁场存在极强的耦合作用。等离子态在宇宙中广泛存在，常被看作物质的第四态（有人也称之为“超气态”）。等离子体由克鲁克斯在1879年发现，“Plasma”这个词，由朗廖尔在1928年最早用。

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o 2.1 电离

o 2.3 速率分布

* 3 参见

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常见的等离子体

等离子体是存在最广泛的一种物态，目前观测到的宇宙物质中，99%都是等离子体。

* 人造的等离子体

o 荧光灯，霓虹灯灯管中的电离气体

o 核聚变实验中的高温电离气体

o 电焊时产生的高温电弧

* 地球上的等离子体

o 火焰（上部的高温部分）

o 闪电

o 大气层中的电离层

o 极光

* 宇宙空间中的等离子体

o 恒星

o 太阳风

o 行星际物质

o 恒星际物质

o 星云

* 其它等离子体

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等离子体的性质

等离子态常被称为“超气态”，它和气体有很多相似之处，比如：没有确定形状和体积，具有流动性，但等离子也有很多独特的性质。

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电离

等离子体和普通气体的最大区别是它是一种电离气体。由于存在带负电的自由电子和带正电的离子，有很高的电导率，和电磁场的耦合作用也极强：带电粒子可以同电场耦合，带电粒子流可以和磁场耦合。描述等离子体要用到电动力学，并因此发展起来一门叫做磁流体动力学的理论。

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组成粒子

和一般气体不同的是，等离子体包含两到三种不同组成粒子：自由电子，带正电的离子和未电离的原子。这使得我们针对不同的组分定义不同的温度：电子温度和离子温度。轻度电离的等离子体，离子温度一般远低于电子温度，称之为“低温等离子体”。高度电离的等离子体，离子温度和电子温度都很高，称为“高温等离子体”。

相比于一般气体，等离子体组成粒子间的相互作用也大很多。

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速率分布

一般气体的速率分布满足麦克斯韦分布，但等离子体由于与电场的耦合，可能偏离麦克斯韦分布。

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参见

* 等离子体物理学

取自"://zh.wikipedia.org/wiki/%E7%AD%89%E7%A6%BB%E5%AD%90%E4%BD%93"

Category: 等离子体物理学

Plasma (physics)

From Wikipedia, the free encyclopedia.

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This article is about plasma in the sense of an ionized gas. For other uses of the term, such as blood plasma, see plasma (disambiguation).

A Plasma lamp, illustrating some of the more complex phenomena of a plasma, including filamentation

Enlarge

A Plasma lamp, illustrating some of the more complex phenomena of a plasma, including filamentation

In physics and chemistry, a plasma is an ionized gas, and is usually considered to be a distinct phase of matter. "Ionized" in this case means that at least one electron has been removed from a significant fraction of the molecules. The free electric charges make the plasma electrically conductive so that it couples strongly to electromagnetic fields. This fourth state of matter was first identified by Sir William Crookes in 1879 and dubbed "plasma" by Irving Langmuir in 1928, because it reminded him of a blood plasma Ref.

Contents

[hide]

* 1 Common plasmas

* 2 Characteristics

o 2.1 Plasma scaling

o 2.2 Temperatures

o 2.3 Densities

o 2.4 Potentials

* 3 In contrast to the gas phase

* 4 Complex plasma phenomena

* 5 Ultracold Plasmas

* 6 Mathematical descriptions

o 6.1 Fluid

o 6.2 Kinetic

o 6.3 Particle-in-cell

* 7 Fundamental plasma parameters

o 7.1 Frequencies

o 7.2 Lengths

o 7.3 Velocities

o 7.4 Dimensionless

o 7.5 Miscellaneous

* 8 Fields of active research

* 9 See also

* 10 External links

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Common plasmas

A solar coronal mass ejection blasts plasma throughout the Solar System. ://antwrp.gsfc.nasa.gov/apod/ap020516.html Ref & Credit

Enlarge

A solar coronal mass ejection blasts plasma throughout the Solar System. ://antwrp.gsfc.nasa.gov/apod/ap020516.html Ref & Credit

Plasmas are the most common phase of matter. The entire visible universe outside the Solar System is plasma, since all we can see are stars. Since the space between the stars is filled with a plasma, although a very sparse one (see interstellar- and intergalactic medium), essentially the entire volume of the universe is plasma. In the Solar System, the planet Jupiter accounts for most of the non-plasma, only about 0.1% of the mass and 10-15 of the volume within the orbit of Pluto. Alfvén also noted that due to their electric charge, very small grains also behe as ions and form part of a plasma (see dusty plasmas).

Commonly encountered forms of plasma include:

* Artificially produced

o Inside fluorescent lamps (low energy lighting), neon signs

o Rocket exhaust

o The area in front of a spacecraft's heat shield during reentry into the atmosphere

o Fusion energy research

o The electric arc in an arc lamp or an arc welder

o Plasma ball (sometimes called a plasma sphere or plasma globe)

* Earth plasmas

o Flames (ie. fire)

o Lightning

o The ionosphere

o The polar aurorae

* Space and astrophysical

o The Sun and other stars (which are plasmas heated by nuclear fusion)

o The solar wind

o The Interplanetary medium (the space between the planets)

o The Interstellar medium (the space between star systems)

o The Intergalactic medium (the space between galaxies)

o The Io-Jupiter flux-tube

o Accretion disks

o Interstellar nebulae

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Characteristics

The term plasma is generally reserved for a system of charged particles large enough to behe as one. Even a partially ionized gas in which as little as 1% of the particles are ionized can he the characteristics of a plasma (i.e. respond to magnetic fields and be highly electrically conductive).

In technical terms, the typical characteristics of a plasma are:

1. Debye screening lengths that are short compared to the physical size of the plasma.

2. Large number of particles within a sphere with a radius of the Debye length.

3. Mean time between collisions usually is long when compared to the period of plasma oscillations.

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Plasma scaling

Plasmas and their characteristics exist over a wide range of scales (ie. they are scaleable over many orders of magnitude). The following chart deals only with conventional atomic plasmas and not other exotic phenomena, such as, quark gluon plasmas:

Typical plasma scaling ranges: orders of magnitude (OOM)

Characteristic Terrestrial plasmas Cosmic plasmas

Size

in metres (m) 10-6 m (lab plasmas) to:

102 m (lightning) (~8 OOM) 10-6 m (spacecraft sheath) to

1025 m (intergalactic nebula) (~31 OOM)

Lifetime

in seconds (s) 10-12 s (laser-produced plasma) to:

107 s (fluorescent lights) (~19 OOM) 101 s (solar flares) to:

1017 s (intergalactic plasma) (~17 OOM)

Density

in particles per

cubic metre 107 to:

1021 (inertial confinement plasma) 1030 (stellar core) to:

100 (i.e., 1) (intergalactic medium)

Temperature

in kelvins (K) ~0 K (Crystalline non-neutral plasma[2]) to:

108 K (magnetic fusion plasma) 102 K (aurora) to:

107 K (Solar core)

Magnetic fields

in teslas (T) 10-4 T (Lab plasma) to:

103 T (pulsed-power plasma) 10-12 T (intergalactic medium) to:

107 T (Solar core)

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Temperatures

The central electrode of a plasma lamp, showing a glowing blue plasma streaming upwards. The colors are a result of the radiative recombination of electrons and ions and the relaxation of electrons in excited states back to lower energy states. These processes emit light in a spectrum characteristic of the gas being excited.

Enlarge

The defining characteristic of a plasma is ionization. Although ionization can be caused by UV radiation, energetic particles, or strong electric fields, (processes that tend to result in a non-Maxwellian electron distribution function), it is more commonly caused by heating the electrons in such a way that they are close to thermal equilibrium so the electron temperature is relatively well-defined. Because the large mass of the ions relative to the electrons hinders energy transfer, it is possible for the ion temperature to be very different from (usually lower than) the electron temperature.

The degree of ionization is determined by the electron temperature relative to the ionization energy (and more weakly by the density) in accordance with the Saha equation. If only a small fraction of the gas molecules are ionized (for example 1%), then the plasma is said to be a cold plasma, even though the electron temperature is typically several thousand degrees. The ion temperature in a cold plasma is often near the ambient temperature. Because the plasmas utilized in plasma technology are typically cold, they are sometimes called technological plasmas. They are often created by using a very high electric field to accelerate electrons, which then ionize the atoms. The electric field is either capacitively or inductively coupled into the gas by means of a plasma source, e.g. microwes. Common lications of cold plasmas include plasma-enhanced chemical vapor deposition, plasma ion doping, and reactive ion etching.

A hot plasma, on the other hand, is nearly fully ionized. This is what would commonly be known as the "fourth-state of matter". The Sun is an example of a hot plasma. The electrons and ions are more likely to he equal temperatures in a hot plasma, but there can still be significant differences.

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Densities

Next to the temperature, which is of fundamental importance for the very existence of a plasma, the most important property is the density. The word "plasma density" by itself usually refers to the electron density, that is, the number of free electrons per unit volume. The ion density is related to this by the erage charge state \langle Z\rangle of the ions through n_e=\langle Z\rangle n_i. (See quasineutrality below.) The third important quantity is the density of neutrals n0. In a hot plasma this is small, but may still determine important physics. The degree of ionization is ni / (n0 + ni).

[edit]

Potentials

Lightning is an example of plasma present at Earth's surface. Typically, lightning discharges 30 thousand amps, at up to 100 million volts, and emits light, radio wes, x-rays and even gamma rays [1]. Plasma temperatures in lightning can roach 28,000 kelvins and electron densities may exceed /m3.

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Since plasmas are very good conductors, electric potentials play an important role. The potential as it exists on erage in the space between charged particles, independent of the question of how it can be measured, is called the plasma potential or the space potential. If an electrode is inserted into a plasma, its potential will generally lie considerably below the plasma potential due to the development of a Debye sheath. Due to the good electrical conductivity, the electric fields in plasmas tend to be very small, although where double layers are formed, the potential drop can be large enough to accelerate ions to relativistic velocities and produce synchrotron radiation such as x-rays and gamma rays. This results in the important concept of quasineutrality, which says that, on the one hand, it is a very good roximation to assume that the density of negative charges is equal to the density of positive charges (n_e=\langle Z\rangle n_i), but that, on the other hand, electric fields can be assumed to exist as needed for the physics at hand.

The magnitude of the potentials and electric fields must be determined by means other than simply finding the net charge density. A common example is to assume that the electrons satisfy the Boltzmann relation, n_e \propto e^{e\Phi/k_BT_e}. Differentiating this relation provides a means to calculate the electric field from the density: \vec{E} = (k_BT_e/e)(\nabla n_e/n_e).

It is, of course, possible to produce a plasma that is not quasineutral. An electron beam, for example, has only negative charges. The density of a non-neutral plasma must generally be very low, or it must be very small, otherwise it will be dissipated by the repulsive electrostatic force.

In astrophysical plasmas, Debye screening prevents electric fields from directly affecting the plasma over large distances (ie. greater than the Debye length). But the existence of charged particles causes the plasma to generate and be affected by magnetic fields. This can and does cause extremely complex behior, such as the generation of plasma double layers, an object that separates charge over a few tens of Debye lengths. The dynamics of plasmas interacting with external and self-generated magnetic fields are studied in the academic discipline of magnetohydrodynamics.

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In contrast to the gas phase

Plasma is often called the fourth state of matter. It is distinct from the three lower-energy phases of matter; solid, liquid, and gas, although it is closely related to the gas phase in that it also has no definite form or volume. There is still some disagreement as to whether a plasma is a distinct state of matter or simply a type of gas. Most physicists consider a plasma to be more than a gas because of a number of distinct properties including the following:

Property Gas Plasma

Electrical Conductivity Very low

Very high

1. For many purposes the electric field in a plasma may be treated as zero, although when current flows the voltage drop, though small, is finite, and density gradients are usually associated with an electric field according to the Boltzmann relation.

2. The possibility of currents couples the plasma strongly to magnetic fields, which are responsible for a large variety of structures such as filaments, sheets, and jets.

3. Collective phenomena are common because the electric and magnetic forces are both long-range and potentially many orders of magnitude stronger than gritational forces.

Independently acting species One Two or three

Electrons, ions, and neutrals can be distinguished by the sign of their charge so that they behe independently in many circumstances, hing different velocities or even different temperatures, leading to new types of wes and instabilities, among other things

Velocity distribution Maxwellian May be non-Maxwellian

Whereas collisional interactions always lead to a Maxwellian velocity distribution, electric fields influence the particle velocities differently. The velocity dependence of the Coulomb collision cross section can amplify these differences, resulting in phenomena like two-temperature distributions and run-away electrons.

Interactions Binary

Two-particle collisions are the rule, three-body collisions extremely rare. Collective

Each particle interacts simultaneously with many others. These collective interactions are about ten times more important than binary collisions.

[edit]

Complex plasma phenomena

Tycho's Supernova remnant, a huge ball of expanding plasma. Langmuir coined the name plasma because of its similarity to blood plasma, and Hannes Alfvén noted its cellular nature. Note also the filamentary blue outer shell of X-ray emitting high-speed electrons

Enlarge

Plasma may exhibit complex behiour. And just as plasma properties scale over many orders of magnitude (see table above), so do these complex features. Many of these features were first studied in the laboratory, and in more recent years, he been lied to, and recognised throughout the universe. Some of these features include:

* Filamentation, the striations or "stringy things" seen in a "plasma ball", the aurora, lightning, and nebulae. They are caused by larger current densities, and are also called magnetic ropes or plasma cables.

* Double layers, localised charge separation regions that he a large potential difference across the layer, and a vanishing electric field on either side. Double layers are found between adjacent plasmas regions with different physical characteristics, and can accelerate ions and produce synchrotron radiation (such as x-rays and gamma rays).

* Birkeland currents, a magnetic-field-aligned electric current, first observed in the Earth's aurora, and also found in plasma filaments.

* Circuits. Birkeland currents imply electric circuits, that follow Kirchhoff's circuit laws. Circuits he a resistance and inductance, and the behiour of the plasma depends on the entire circuit. Such circuits also store inductive energy, and should the circuit be disrupted, for example, by a plasma instability, the inductive energy will be released in the plasma.

* Cellular structure. Plasma double layers may separate regions with different properties such as magnetization, density, and temperature, resulting in cell-like regions. Examples include the magnetosphere, heliosphere, and heliospheric current sheet.

* Critical ionization velocity in which the relative velocity between an ionized plasma and a neutral gas, may cause further ionization of the gas, resulting in a greater influence of electomagnetic forces.

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Ultracold Plasmas

It is also possible to create ultracold plasmas, by using lasers to trap and cool neutral atoms to temperatures of 1 mK or lower. Another laser then ionizes the atoms by giving each of the outermost electrons just enough energy to escape the electrical attraction of its parent ion.

The key point about ultracold plasmas is that by manipulating the atoms with lasers, the kinetic energy of the liberated electrons can be controlled. Using standard pulsed lasers, the electron energy can be made to correspond to a temperature of as low as 0.1 K ? a limit set by the frequency bandwidth of the laser pulse. The ions, however, retain the millikelvin temperatures of the neutral atoms. This type of non-equilibrium ultracold plasma evolves rapidly, and many fundamental questions about its behiour remain unanswered. Experiments conducted so far he revealed surprising dynamics and recombination behiour that are pushing the limits of our knowledge of plasma physics.

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Mathematical descriptions

Plasmas may be usefully described with various levels of detail. However the plasma itself is described, if electric or magnetic fields are present, then Maxwell's equations will be needed to describe them. The coupling of the description of a conductive fluid to electromagnetic fields is known generally as magnetohydrodynamics, or simply MHD.

[edit]

Fluid

The simplest possibility is to treat the plasma as a single fluid governed by the Nier Stokes Equations. A more general description is the two-fluid picture, where the ions and electrons are considered to be distinct.

[edit]

Kinetic

For some cases the fluid description is not sufficient. Kinetic models inc

什么是等离子态？

火焰一般可以看作等离子体，不过构成火焰的粒子的电离程度并不高。这将在后面进行详细讨论。那什么是等离子体呢？下面就来先为大家介绍它。

什么是等离子体？

等离子体又叫做电浆，被视为物质的第4种形态，或者称为“超气态”。简单来说就是电离了的“气体”，由离子、电子以及未电离的中性粒子组成，整体呈电中性。等离子体并不需要完全由离子构成。

等离子体属于非凝聚态，构成等离子体的粒子之间游离程度较高，粒子间的相互作用不强。至于凝聚态，就是由大量处于聚集状态的粒子构成的物态，液体和固体就是最常见的凝聚态。

等离子体并不神秘。气体通常都是由分子或原子构成的，而等离子体就是被电离（电离就是原子得到或者失去核外电子形成离子的一种过程，离子都带电）的气体。几乎所有气体都存在一定程度的电离，只是电离程度极低，因此并不能算作等离子体。并且物体要称之为等离子体，还需要具备等离子体所具备的特性，比如存在等离子体振荡、会受电磁场影响等。等离子体振荡是等离子体中的电子在惯性和离子的静电力作用下发生的简谐振动。

等离子体是宇宙中最常见的物态。宇宙中最常见的天体就是恒星，星系也是由恒星构成的，像太阳等恒星就是一个巨大的等离子体，它占了整个宇宙中物质形态的99%。自然界中的闪电就是等离子体。用人工方法，如核聚变、核裂变，也可产生等离子体。

不同等离子体在温度和密度方面差异巨大。以温度划分，等离子体可分为高温等离子体和低温等离子体。等离子体的温度分别用电子温度和离子温度表示，两者相等（或者说相差不多）则称为高温等离子体，不相等则称为低温等离子体。

最常见的等离子体是高温等离子体。处于核聚变状态的物质、电弧、闪电、极光等都是高温等离子体。高温等离子体在切割、冶炼、焊接等领域都有广泛的应用。

低温等离子体又叫做非平衡态等离子，可以存在于常温状态。辉光放电、电晕放电等现象都可以产生低温等离子体。日光灯（又叫做荧光灯）就是通过低压状态的汞蒸气通电后会发生辉光放电，并发射出紫外线，激发荧光粉发光的。在日常生活中大家耳熟能详的等离子电视，就是利用低温等离子体制成的显示器。除此之外还有等离子体涂层。

（上图为电晕放电现象）

为什么火焰属于等离子体？

火焰也是物质，是燃烧时的产物，能够发光发热。在太空中，没有重力作用，火焰会呈现为球形。

火焰的温度有高有低，不同材质燃烧时所形成的火焰，具有不同的温度。打火机火焰的温度大约在400度左右，酒精灯火焰的温度在600~700度，普通炉火的温度大约在800度左右，一般的纸张燃烧时产生的火焰温度仅为200多度。

此外，火焰又分为焰心、中焰和外焰，其中外焰由于与氧气或者氧化剂接触更充分，燃烧反应也更充分，因此温度更高。当可燃物与氧化剂接触时，温度达到着火点就会产生火焰。

一些材质燃烧时还会产生一些固体小颗粒，在热气上升的带动下夹杂在火焰中。不同的材质在燃烧时，火焰的颜色也各不相同。

一般来说温度越高，火焰中粒子的电离程度也就越高，火焰的温度一般都很高，属于高温等离子体。一些温度较低的火焰，由于电离程度太低，因此并不能完全算作等离子体，只能算是处于激发态（原子或者分子吸收能量后，被激发到高能级，尚未电离的状态）的高温气体。

上面已经说过，磁场能够影响等离子体。如果高温火焰是等离子体的话，必然会受到强磁场的影响。实验证明，火焰会受到磁场影响。

（如上图实验所示，磁场的变化能够对蜡烛火焰产生影响）

通过对等离子体有了一定的了解，相信大家也明白为什么火焰属于等离子体了。

感谢阅读，热爱科学的朋友，欢迎关注我。

等离子体简介

等离子态是物质的第四种形态——前三种为固态、液态和气态。等离子态的物体可以自由地占据可用空间，这一特征与气态十分相似，但是它的原理更加复杂，原子变成了离子并且释放出它们的电子，而电子可以自由地在充满气体的空间中流动。等离子是许多常见设备的主要组成部分，如荧光管（一种由电流引起的低温等离子体）。

然而，在武器研究方面，人们最感兴趣的等离子体是高能等离子体，高能等离子体的温度十分高，因此它的粒子有足够高的能量来引起互相之间的核聚变。

用聚变能量供电，这些等离子炮会把大气粒子吸进来，在聚变反应堆里加至过热，然后射出高能的等离子体产物。武器的战斗威力是目标几乎完全被毁灭。

由于与大气的交互作用，武器的射程相对较短，但是它的效果仍然相当可观。金属装甲只能提高武器的效力，而越大的坦克在等离子体武器面前下场越是糟糕。最初的是要将这种武器安装在坦克上并大量生产。

等离子体中主要基元反应过程

分类: 教育/科学 >> 科学技术

解析:

等离子体是由部分电子被剥夺后的原子及原子被电离后产生的正负电子组成的离子化气体状物质，它是除去固、液、气外，物质存在的第四态。等离子体是一种很好的导电体，利用经过巧妙设计的磁场可以捕捉、移动和加速等离子体。等离子体物理的发展为材料、能源、信息、环境空间，空间物理，地球物理等科学的进一步发展提新的技术和工艺。

看似“神秘”的等离子体，其实是宇宙中一种常见的物质，在太阳、恒星、闪电中都存在等离子体，它占了整个宇宙的99％。现在人们已经掌握利用电场和磁场产生来控制等离子体。例如焊工们用高温等离子体焊接金属。

等离子体可分为两种：高温和低温等离子体。以上提到的是高温等离子体。现在低温等离子体广泛运用于多种生产领域。例如：等离子电视，婴儿尿布表面防水涂层，增加啤酒瓶阻隔性。更重要的是在电脑芯片中的蚀刻运用，让网络时代成为现实。

高温等离子体只有在温度足够高时发生的。太阳和恒星不断地发出这种等离子体，组成了宇宙的99％。低温等离子体是在常温下发生的等离子体（虽然电子的温度很高）。低温等离子体体可以被用于氧化、变性等表面处理或者在有机物和无机物上进行沉淀涂层处理。

等离子体是物质的第四态，即电离了的“气体”，它呈现出高度激发的不稳定态，其中包括离子(具有不同符号和电荷)、电子、原子和分子。其实，人们对等离子体现象并不生疏。在自然界里，炽热烁烁的火焰、光辉夺目的闪电、以及绚烂壮丽的极光等都是等离子体作用的结果。对于整个宇宙来讲，几乎99．9％以上的物质都是以等离子体态存在的，如恒星和行星际空间等都是由等离子体组成的。用人工方法，如核聚变、核裂变、辉光放电及各种放电都可产生等离子体。分子或原子的内部结构主要由电子和原子核组成。在通常情况下，即上述物质前三种形态，电子与核之间的关系比较固定，即电子以不同的能级存在于核场的周围，其势能或动能不大。

等离子体中主要基元反应过程包括电离、激发和复合等过程。

一、等离子体的过程

1、初级电离

物质在外加电场、光子、撞击等作用下，原子或分子中的电子被剥离，形成自由电子和阳离子。

2、二级电离

自由电子和阳离子在等离子体中通过碰撞和吸收能量，可以进一步产生更多的自由电子和离子，这个过程称为二级电离。

3、复合

等离子体中的带电粒子通过碰撞和相互反应，可以重新结合成中性粒子，这个过程称为复合。

二、等离子体和固体电解质有什么区别

1、物质状态

等离子体是一种电离的气体状物质，由部分电子被剥夺后的原子及原子团被电离后产生的正负离子组成。而固体电解质则是一种固体离子导体电解质，具有固态物质的特性。

2、电性质