JP2002008892A - Plasma analyzing device and method - Google Patents

Abstract

PROBLEM TO BE SOLVED: To provide a plasma analyzing method and device whereby three- dimensional simulation can be made even if the system is such that chemical reactions of ions are produced. SOLUTION: This plasma analyzing device equipped with an input means, calculating means, and output means for analyzing a plasma is provided with a plasma analyzing means by means of the equation of motion and the Maxwell' s equations, a boundary conditions setting means to give the boundary conditions of the plasma, and an ion chemical reaction condition setting means to set the condition about the ion chemical reactions of the plasma.

Description

DETAILED DESCRIPTION OF THE INVENTION

[0001]

[0001] 1. Field of the Invention [0002] The present invention relates to a plasma analyzer and an analysis method. In particular, it is possible to simulate the distribution of plasma density and velocity and the electromagnetic field in three dimensions from the equation of motion and the Maxwell's equation of the electromagnetic field, which describe the plasma in space as a simulation model, even in a system where ion chemical reactions occur. It is.

[0002] The present invention can be used in the space development related industry, the field of plasma engineering, and the like.

[0003]

2. Description of the Related Art In computer simulations of plasma phenomena such as the interaction between the solar wind and the plasma of a planet, a hybrid code that treats ions as particles and electrons as fluid has been used. Using a model that regards the planet as a non-magnetic solid sphere, the plasma interaction between the solar wind and the planet can be simulated. An example of applying the hybrid code to space plasma is described in the following paper.

(1) Leroy, M .; M. , D. Win
ske, C.I. C. Goodrich, C .; S. Wu, a
nd K. Papadopoulos, "The best
ructure of perpendicular
bow shocks ", Journal of Ge
Ophthalmic Research, vol. 8
7, pp. 5081-5094 (1982).

FIG. 12A shows a model for analyzing a plasma interaction between a solar wind and a planet, considering the planet as a non-magnetic solid.

Considering the planet 110 as a non-magnetic solid sphere,
This shows that the solar wind, which is a plasma stream, is irradiated. In this model, the solar wind plasma ions that irradiate the planet are reflected on the planet's surface, and some ions enter the planet and disappear inside.

[0007] The results of simulating this model with a hybrid code are described in detail in the following papers and the like.

(2) Shimazu, H .; , "Thre
e-dimensional hybrid simu
ration of magnetized plus
maflow around an obstacl
e ", Earth, Planets and Spac
e, vol. 51, pp 383-393 (199
9).

[0009]

Description of the Prior Art In the case where the ionosphere exists above the planet, FIG.
Simulating the interaction with the solar wind, assuming that the planet is a solid as in the above, does not really fit. Above the actual planet is the ionosphere, which can be thought of as a plasma mass. Therefore, the inventor of the present application attempted a simulation using a planet as a plasma mass ("3D hybrid simulation of the interaction between the solar wind and Mars Venus-type planet", The 106th Annual Meeting and Lecture of the Geoscience Society of Japan, Sendai Citizen) Hall, November 9, 1999-
Announced at Lecture Number B12-P054 on the 12th).

FIG. 12 (b) shows a model in which the planet is treated as a plasma mass of a sphere having a radius R and the solar wind irradiates the plasma mass.

In FIG. 12B, reference numeral 110 denotes a planet, which is a plasma mass. The ions (H ⁺ ) of the solar wind irradiating the planet enter the interior of the planet and sometimes mix with the ions (O ⁺ ) in the planet.

FIG. 13 schematically shows the results of computer simulation of the plasma density, velocity distribution, and electromagnetic field by solving the equation of motion and the maximum equation of ions using the hybrid code for this model.
Shown in

In FIG. 13, reference numeral 110 denotes a planet, which is a plasma mass. 111 is a shock wave (a bow shock, hereinafter referred to as a shock). As shown in FIG. 13, the solar wind is a supersonic plasma flow, and when this plasma flow enters the magnetosphere of the planet, a shock 111 is generated on the front.

FIG. 14A shows parameters used for analysis using a plasma lump model. FIG. 14B shows a model that gives the initial condition and the boundary condition. FIG.
In (b), the magnetic flux density is given by the following equation.

[0015]

(Equation 1)

In the simulation, the outer space is 64 × 64
A space (lattice space) divided into × 64, and the average values of the particle density, particle velocity, and the like inside the space are defined as the respective values at the lattice points. The cosmic plasma phenomenon was simulated using the equation of motion, the Maxwell equation, and the like, in which the values at the lattice points were converted into data.

Alben velocity V in simulation
The ratio of _A to the speed of light c is expressed as V _A / c = ω _ci / ω _pi = 1.0 × 1
^0-4 . ω _ci is the cyclotron angular frequency of the ion. ω _pi is the angular frequency of the ion plasma oscillation.

The ratio of the thermal pressure to the magnetic pressure was β _e = β _i = 1 for electrons and ions. The speed of the solar wind is v _SW = 4
. 0V _A.

A planet wrapped in the ionosphere is represented as a plasma sphere of radius R. The solar wind flows from left to right in the x-axis direction, and the magnetic flux density is in the y-direction. In the initial state, the dynamic pressure of the solar wind and the pressure of the planetary plasma are almost balanced.
L indicates the size of the outer space to be simulated. The supply rate of ions to the plasma sphere is 0.256 ω _pi .

FIGS. 15A, 15B, and 15C show simulation results of a model using a planet as a plasma sphere.

FIG. 15A is a cross-sectional view at y = L / 2, and shows the x component of the ion velocity at the time of _ωcit = 37.5 after the start of the simulation. The ion velocity is Vix /
It is represented by _VA . In FIG. 13A, the center of the planet is at coordinates (102.4, 102.4), and the solar wind is blowing in the x-axis direction (from left to right). A shock is formed as shown. The planet radius is R = 6.4r _L (r
_L = v _SW / ω _ci ).

FIG. 15B shows the magnitude of the magnetic flux density in the sectional view at y = L / 2. The magnetic flux density is | B | / Bo
(Bo is the magnitude of the magnetic flux density given in the initial condition). FIG. 15C shows the distribution of oxygen ions of the planet in a cross-sectional view at y = L / 2. FIG. 16 (a)
FIG. 4 is a cross-sectional view at x = L / 2, showing the magnitude of magnetic flux density as a result of the simulation when ω _cit = 37.5 after the start of the simulation. In FIG. 16A,
Planets are indicated by solid circles, and shock surfaces are indicated by hazy circles surrounding the planet. As shown in FIG. 16 (a), in the simulation, the height of the shock from the planet is large in the positive direction of the z-axis and small in the negative direction of the z-axis. I have.

This is different from the actual observation result. The actual observation result shows the height of the shock from the planet, as shown in FIG.
As shown in the figure, it has been observed that it is small in the positive direction of the z-axis and large in the negative direction of the z-axis (the shock surface is shifted in the negative direction of the z-axis with respect to the planet).

FIG. 16B is a cross-sectional view at x = 3L / 4, and shows the magnitude of the magnetic flux density at ω _cit = 37.5 after the start of the simulation.

The above model of the interaction between the solar wind and the planetary plasma does not deal with ionic reactions (photoionization, charge exchange, etc.) occurring in the high layers of the planet. Therefore, the simulation result of the positional relationship between the shock surface and the planet was not always correct.

An object of the present invention is to provide a plasma analysis apparatus and method capable of accurately performing three-dimensional simulation even in a plasma system in which a chemical reaction of ions occurs.

[0027]

FIG. 1 shows the basic configuration of the present invention.

In FIG. 1, reference numeral 1 denotes initial condition holding means for inputting initial conditions input by the input means 6. Reference numeral 2 denotes a plasma boundary condition holding unit that holds the plasma boundary condition input by the input unit 6. Reference numeral 3 denotes ion chemical reaction condition holding means for holding conditions for the chemical reaction of the plasma inputted by the input means 6. Reference numeral 4 denotes a plasma analysis means for performing a plasma analysis based on particle motion equations, Maxwell equations, initial conditions, boundary conditions, ion chemical reaction conditions, and data representing the plasma state (data such as ion generation rate). . Reference numeral 5 denotes an analysis result output means for outputting an analysis result.
6 is an input means. Reference numeral 7 denotes a plasma state data holding unit.

The operation of the basic configuration of the present invention shown in FIG. 1 will be described.

The input means 6 inputs initial conditions, boundary conditions of plasma, and conditions of a chemical reaction occurring in plasma. Further, plasma state data such as the ion cyclotron frequency of the plasma and the ion generation rate are input and held in the state data holding means 7. The plasma analysis means 4 analyzes a state generated in the plasma based on initial conditions, boundary conditions, ion chemical reaction conditions, and plasma state data. The output means 5 outputs the obtained plasma state.

The chemical reaction conditions include, for example, in the case of the interaction between the solar wind and the planet, when the ion (H ⁺ ) of the solar wind and the planetary ion (O ⁺ ) are set, H ⁺ + O → H + O ⁺ (planetary plasma). It is. O and H are atoms that are not ionized, and are excluded from the plasma in the analysis. Under such a chemical reaction condition, a current change occurs due to an ion reaction, which affects the motion of the plasma. As will be described later, in the simulation of the interaction between the solar wind and the planetary ions, according to the simulation apparatus and method of the present invention, the relationship between the planet and the height of the shock cannot be obtained by the method prior to the present invention. However, as shown in FIG. 8, the results became consistent with the actual observation results.

According to the present invention, not only the initial conditions and boundary conditions of the plasma, but also the ion reaction conditions can be analyzed under the simulation conditions, so that even in a plasma system in which an ion chemical reaction occurs, the plasma can be accurately three-dimensionally analyzed. Be able to simulate.

The plasma analyzing apparatus and method of the present invention can be applied not only to space plasma but also to plasma in a laboratory or the like.

[0034]

DETAILED DESCRIPTION OF THE PREFERRED EMBODIMENTS A hybrid code for implementing the present invention will be described. In the following, B, E,
v and j are all three-dimensional vectors, and are represented by a vector B, a vector E, a vector v, a vector j, and the like, respectively. Vector x is a position vector. B represents magnetic flux density, E represents electric field, v represents ion velocity, and j represents current.

The basic equations for analysis using the hybrid code are as follows.

Equation of motion of ion

[0037]

(Equation 2)

Equation for ion velocity

[0039]

(Equation 3)

Equation of motion of an electronic fluid (without mass)

[0041]

(Equation 4)

However, the electron temperature _Te is constant.

Maxwell equation

[0044]

(Equation 5)

[0045]

(Equation 6)

Quasi-neutral condition _ne = _ni = n (6) In the present embodiment, it is assumed that the electric conductivity is infinite (η =
0).

In the simulation, the above equation is used after being differentiated.

When Maxwell's equation (4) is differentiated, the following is obtained.

[0049]

(Equation 7)

The vector j _{k + 1} is obtained from the vector B _{k + 1} using the equation (5).

When the equations (1) and (2) are differentiated, the following is obtained.

[0052]

(Equation 8)

[0053]

(Equation 9)

The magnetic flux density at time k can be expressed as follows by the magnetic flux density at time k + 1 and the magnetic flux density at time k-1.

[0055]

(Equation 10)

The position vector at time k + 1 can be expressed as follows.

[0057]

[Equation 11]

[0058] velocity vector of the grid point v _i and density n _i is obtained by summing the ion velocity and density for each grid point. The velocity vector v _e of the electronic fluid is obtained by the following expression representing the current.

[0059]

(Equation 12)

The electric field vector E can be obtained from the electron velocity vector v _e , the equation of motion of the electron fluid, and the quasi-neutral condition.

The density and velocity of ions at a lattice point are set so as to be larger from those closer to the lattice point and smaller at those farther from the lattice point.

Specifically, a shape function as shown in FIG. 4 is used.

The density is

[0064]

(Equation 13)

Is obtained.

The speed average is

[0067]

[Equation 14]

Is obtained. N is the total number of particles in the space to be simulated.

FIG. 2 shows an embodiment of the apparatus configuration of the present invention.

FIG. 2 shows a configuration for analysis using a hybrid code that treats ions as particles and electrons as fluid.

Reference numeral 11 denotes initial conditions to be input (magnetic flux density vectors B ₀ , B ₁ , electric field vector E ₀ , particle density n ₀ , particle velocity vector v _i0 ). Reference numeral 12 denotes an input unit. Reference numeral 13 denotes an operation means. 14 is the time k + of the operation result
1, electric field vector E _{k + 1} , magnetic flux density vector B
_{k + 1} , current density vector _{Jk + 1} , particle density _{nk + 1} , particle position vector _{xk + 1} , and particle velocity vector vk _{+ 1} . Reference numeral 15 denotes an output unit. Reference numeral 20 denotes a data holding unit. 21 is an initial condition holding unit. Reference numeral 22 denotes a boundary condition holding unit. Reference numeral 17 denotes state data, which represents parameters such as an ion generation rate. Numeral 31 denotes an arithmetic expression holding unit which holds an arithmetic expression used for analysis by the hybrid code, and holds the above-mentioned difference equation and other expressions necessary for the arithmetic operation. 32 is a differential ion motion equation. 33 is a differential electron motion equation. 34 is a differential Maxwell equation. 35 is an equation of the velocity of the electronic fluid. 36 is a particle neutral condition, and _ni = _ne =
n. Numeral 36 is an equation for calculating the average of the particle density and the average of the particle velocity. Reference numeral 37 denotes other expressions necessary for the operation.

A case where the interaction between the solar wind and planets (Mars, Venus, etc.) is simulated by the following model using the plasma analysis apparatus of the present invention will be described. The plasma generation rate, the radius of the plasma sphere, and the initial magnetic flux density are the same as in the preceding simulation (the above-mentioned plasma mass model).

(1) Assume that there is photoionization outside the plasma sphere (1.0R and 1.3R dayside) representing a planet of radius R.

[0074] ^{O + hν → O + + e} - (2) and there is a charge exchange in the same area.

H ⁺ + O → H + O ⁺ Neutralized molecules are irrelevant to the calculation, and in the case of (1), O ⁺ is generated at a certain ratio. H of the solar wind
⁺ Shall not be changed. The position to be generated is determined using random numbers so as to be uniformly distributed in the above-mentioned area.
In the case of (2), the solar wind disappears at a certain rate, and O ⁺
Is equivalent to generating That is, 1.0R and 1.3
A predetermined ratio of the solar wind ions (H ⁺ ) reached during R disappears. O at the position where it disappeared
Generate ⁺ . This result appears in the change of the vectors v _i and n by the particle averaging process (described later), which affects the overall calculation. In (1) and (2), the ion velocity is determined by a random number so that the temperature has the same velocity distribution as the temperature of the planetary ions. The velocity distribution is set to be a Maxwell distribution represented by the following equation (13).

[0076]

(Equation 15)

A is determined as follows.

[0078]

(Equation 16)

[0079] (1/2) is a mv _th ² = k _B T. n is the particle density, m is the ion mass, k _B is the Boltzmann constant, T
Is the temperature.

FIG. 3 is a flowchart of the operation of the configuration of FIG.
It is. The operation of FIG. 3 will be described. Magnetic flux density and electric
Initial condition vector B for field, particle velocity and density₀,vector
 B ₁, Vector E₁, Vector v_i0, N.
B₀Are the same as those in FIG.

The initial conditions are set so that the solar wind and the ion velocity of the planet have a Maxwell distribution. The solar wind temperature and the planetary plasma temperature are the same.

At S2, the electric field vectors E _k and B _k−1 at time k are calculated.
To obtain B _{k + 1} according to Maxwell's equation. Next, in S3, the current density vector J _{k + 1} at time k + 1 is obtained by using the magnetic flux density vector B _{k + 1} at time k + 1 according to the Maxwell equation. Then the ion particle density n _i in S4, the electron density n _e (= n) between the speed v _i and time k + 1
Use the current density vector J _{k + 1,} obtains the time k + 1 of the electron velocity vector v _e.

Next, at S5, the velocity of the electron at time k + 1 is calculated.
Kutor v_e, Magnetic flux density vector B_{k + 1}, Current density vector
Le J_{k + 1}, Charge density n_e, Boltzmann constant k_B, Electron temperature
Degree T _eAnd the electric field vector E at time k + 1_{k + 1}Seeking
Confuse. Next, the time is updated by k = k + 2, and after S2
Is repeated.

For the above main routine, boundary conditions, ion reaction conditions, averaging of particle density, and averaging of particle velocity are performed in subroutines (S11, S12, S13, S1).
Process in 4).

At S11, the boundary condition between the solar wind and the plasma mass is input. Let the planet be a plasma sphere of radius R. It is assumed that the ions of the solar wind are protons (H ⁺ ) and the ions of the planet having a radius R are oxygen ions (O ⁺ ).

At S12, ion reaction conditions are input.

As described above, (1) It is assumed that photoionization (O + hν → O ⁺ + e ⁻ ) occurs outside the plasma sphere including the planet (dayside of 1.0R and 1.3R). Yield in this embodiment was 0.256ω _pi.

(3) Charge exchange (H ⁺ + O →
H + O ⁺ ). In the present embodiment, the generation rate is 0.212 ω _pi .

At S13, the average of the particle density is obtained. The average of the particle density is obtained based on the shape function in FIG. 4 based on all the particles in the outer space.

The -1 and +1 on the horizontal axis of the shape function in FIG. 4 indicate the space to be simulated by 64 × 64 × 64.
, The average particle density at the lattice points is approximately the average of the particle densities in the lattice.

In S14, the average of the particle velocities is determined. The average is obtained from all the particles in the space using the shape function of FIG. 4 in the same manner as the particle density.

The results of S13 and S14 are called and used in S4 and S5.

FIG. 5 is an explanatory diagram of the above model.

Reference numeral 110 denotes a planet, a plasma having a radius R.
It is a sphere. The ions are oxygen ions (O ⁺). radius
In the region of 1.0R and 1.3R, the photoionization reaction (O + hν →
O⁺+ E^-) And charge exchange (H⁺+ O → H + O⁺)But
is there.

FIGS. 6A and 6B show simulation results. 6 (a) and 6 (b) are respectively
The x component of the electron velocity on the y = L / 2 plane when only photoionization at time 37.5 / ωci and charge exchange are present is shown. The planet center is at (102.4, 102.4).

As shown in FIGS. 6A and 6B, a bow shock is generated.

FIGS. 7A and 7B show that y = L when there is only photoionization and when there is charge exchange, respectively.
2 shows the magnetic flux density on the / 2 plane. A magnetic barrier is formed as shown. FIG. 7A shows that when comparing FIG. 7B, the strength of the magnetic barrier is larger when charge exchange is included.

FIG. 8 (a) shows that x =
The magnetic field strength of the L / 2 plane is shown. FIG. 8B shows the magnetic field strength on the x = L / 2 plane when there is charge exchange.

In FIG. 8A, the height of the shock measured from the center of the planet is 7.98% larger than the other side with respect to the center of the planet in the + z direction. The direction of asymmetry is consistent with previous simulations with neither photoionization nor charge exchange. However, Figure 8 including charge exchange
In the case of (b), the asymmetry of the shock height with respect to the center of the planet is opposite to the case of FIG. 8 (a), and agrees with the actual observation result. The height of the shock from the planet is 7.79% greater in the electric field direction (-z direction) than in the opposite direction.

To confirm the cause of the difference in shock altitude, the velocity distribution of ions was considered.

FIGS. 9A and 9B show the phase space distribution (v _z -x) of the ion velocity along the line y = z = L / 2.
Is shown. FIG. 9A shows the case where there is only photoionization, and FIG. 9B shows the case where there is charge exchange. The difference between FIGS. 9A and 9B is the edge portion of [x / (c / ω _pi ) = around 70]. If there is a charge exchange, the planet ions are accelerated in the -z direction.

As a reason for this acceleration, the Hall term (j × B term, where j
Is the current, which is called the Hall current). Figure 1
0 indicates a j × B z component (x component and y component are
smaller than the z component). When comparing FIG. 10A and FIG. 10B, the size is larger when there is charge exchange. Z component of J × B is mainly generated by the j _x and B _y (x-axis is the direction of the solar wind flow, the y-axis is the magnetic field direction of the circumference). The current jx is generated by the difference in velocities between ions and electrons due to the occurrence of charge exchange.

The ions are affected by the electric field due to the Hall term and are accelerated to the -z direction. FIG.
(A) and (b) are x = 80c / ωpi, y = L / 2,
5 shows a distribution of a velocity space (v _z −v _x ) at Z = 80 c / ω pi. FIG. 11A shows the case where there is only photoionization, and FIG. 11B shows the case where there is charge exchange. The presence of charge exchange indicates that the ions are scattered by the electric field.

The above is a simulation in the case where the charge exchange is H ⁺ + O → H + O ⁺ , but a simulation was also performed in the case where the next charge exchange reaction occurs.

H ⁺ + H → H + H ⁺ The resulting direction of asymmetric shock height was shown to be similar to that of oxygen. Therefore, it was confirmed that the hole current generates a shock asymmetry, which is consistent with the actual observation.

As described above, in the previous simulation, the result was that the height of the shock wave (shock) was low in the direction of the electric field (− (vector v _e ) × (vector B) direction (−z direction)). However, according to the result of actually examining Venus, it is known that the shock altitude is large in the direction of the electric field. When the planet was regarded as a plasma lump, the simulation showed different results from the actual one. However, when the simulation was performed in consideration of the charge exchange, the actual observation and simulation results agreed. . When only the photoionization was considered, the simulation and the actual observation did not agree. If there is charge exchange, the solar wind ions disappear, O ⁺ is generated, and extra current is generated. As a result, a strong magnetic barrier is created.
Therefore, it is considered that this magnetic barrier causes a difference in shock height.

[0107]

As described above, according to the present invention, an ion reaction can be easily given to the analysis of a plasma phenomenon, and an accurate simulation of the plasma phenomenon becomes possible.

In particular, when the present invention is used as an apparatus for analyzing space plasma, it becomes possible to reproduce the asymmetry of the direction of the electric field of the shock wave generated in front of the planet, and to accurately simulate the space plasma. Can be.

[Brief description of the drawings]

FIG. 1 is a diagram showing a basic configuration of the present invention.

FIG. 2 is a diagram showing an embodiment of the device configuration of the present invention.

FIG. 3 is a diagram showing a flowchart of the embodiment of the present invention.

FIG. 4 is a diagram illustrating an example of a shape function.

FIG. 5 is a diagram showing an example of a space plasma model.

FIG. 6 is a diagram showing a simulation result of the present invention.

FIG. 7 is a diagram showing a simulation result of the present invention.

FIG. 8 is a diagram showing a simulation result of the present invention.

FIG. 9 is a diagram showing a simulation result of the present invention.

FIG. 10 is a diagram showing a simulation result of the present invention.

FIG. 11 is a diagram showing a simulation result of the present invention.

FIG. 12 is a diagram illustrating an example of a plasma model.

FIG. 13 is a diagram showing an example of a simulation result based on a plasma lump model.

FIG. 14 is a diagram showing an example of parameters and initial conditions used for analyzing a plasma phenomenon.

FIG. 15 is a diagram showing a simulation result based on a plasma lump model.

FIG. 16 is a diagram showing a simulation result based on a plasma lump model.

[Description of Signs] 1: Initial condition holding means 2: Plasma boundary condition holding means 3: Ion chemical reaction condition holding means 4: Plasma analysis means 5: Analysis result output means 6: Input means 7: State data holding means

Claims (8)

[Claims] An apparatus for analyzing a plasma, comprising an input means, an arithmetic means and an output means, comprising: an equation of motion;
A plasma analysis apparatus comprising plasma analysis means for analyzing plasma by using Macwell equations, and performing plasma analysis using an ion chemical reaction of plasma as an analysis condition. 2. The plasma analysis apparatus according to claim 1, wherein the plasma analysis means analyzes the plasma using ions as particles and electrons as fluid. 3. The plasma analyzer according to claim 1, further comprising means for setting a chemical reaction condition in a system to be analyzed. 4. A plasma generating means for generating plasma at a constant rate in a plasma mass, wherein the planet is made into a plasma mass, a solar wind is made into ions incident from the outside, and a chemical reaction between the solar wind and the outside of the plasma mass or plasma mass. 5. The plasma analysis apparatus according to claim 4, wherein space plasma is analyzed by using as an ion chemical reaction condition. 5. A plasma phenomena is analyzed by arithmetic means in accordance with plasma ion chemical reaction conditions set by input means, equations of motion of plasma particles and Macwell equations, and an analysis result is output by output means. Plasma analysis method. 6. The plasma analysis method according to claim 5, wherein the equation of motion analyzes the plasma by regarding ions as particles and electrons as fluid. 7. The plasma analysis method according to claim 5, wherein plasma analysis is performed on condition that an ion chemical reaction of a system to be analyzed is performed. 8. A planet is regarded as a plasma mass, a plasma is generated in the plasma mass at a fixed rate, and a solar wind is used as the incident ion, and the solar wind and the plasma mass, or the solar wind and ions around the outside of the plasma mass are generated. The plasma analysis method according to claim 7, wherein space plasma is analyzed under a condition of a chemical reaction.