Real-time image of solar wind (online). What is the solar wind? The solar wind is

Constant radial flow of solar plasma. crowns in interplanetary production. The flow of energy coming from the depths of the Sun heats the corona plasma to 1.5-2 million K. DC. heating is not balanced by energy loss due to radiation, since the corona is small. Excess energy means. degrees are carried away by the S. century. (=1027-1029 erg/s). The crown, therefore, is not in a hydrostatic position. equilibrium, it continuously expands. According to the composition of the S. century. does not differ from corona plasma (solar plasma contains mainly protons, electrons, some helium nuclei, oxygen, silicon, sulfur, and iron ions). At the base of the corona (10 thousand km from the photosphere of the Sun), particles have a radial radial of the order of hundreds of m/s, at a distance of several. solar radii it reaches the speed of sound in plasma (100 -150 km/s), near the Earth's orbit the speed of protons is 300-750 km/s, and their spaces. - from several h-ts to several tens of ppm in 1 cm3. With the help of interplanetary space. stations, it has been established that up to the orbit of Saturn, the flux density of the h-c S. v. decreases according to the law (r0/r)2, where r is the distance from the Sun, r0 is the initial level. S.v. carries with it the loops of the solar power lines. mag. fields, which form the interplanetary magnetic field. . The combination of radial movement h-c S. v. with the rotation of the Sun it gives these lines the shape of spirals. Large-scale structure of mag. The fields in the vicinity of the Sun have the form of sectors, in which the field is directed from the Sun or towards it. The size of the cavity occupied by the S. v. is not precisely known (its radius is apparently no less than 100 AU). At the boundaries of this cavity there is a dynamic S.v. must be balanced by the pressure of interstellar gas, galactic. mag. fields and galactic space rays. In the vicinity of the Earth, the collision of the flow of h-c S. v. with geomagnetic field generates a stationary shock wave in front of the earth's magnetosphere (from the side of the Sun, Fig.).

S.v. flows around the magnetosphere, as it were, limiting its extent in space. Changes in solar intensity associated with solar flares, phenomena. basic cause of geomagnetic disturbances. fields and magnetosphere (magnetic storms).

For the Sun it loses from the north. =2X10-14 part of its mass Msol. It is natural to assume that the outflow of matter, similar to the S.E., also exists in other stars (""). It should be especially intense in massive stars (with mass = several tens of Msolns) and with high surface temperatures (= 30-50 thousand K) and in stars with an extended atmosphere (red giants), because in In the first case, the particles of a highly developed stellar corona have a sufficiently high energy to overcome the gravity of the star, and in the second, the parabolic energy is low. speed (escaping speed; (see SPACE SPEEDS)). Means. Mass losses with stellar wind (= 10-6 Msol/year and more) can significantly affect the evolution of stars. In turn, the stellar wind creates “bubbles” of hot gas in the interstellar medium - sources of X-rays. radiation.

Physical encyclopedic dictionary. - M.: Soviet Encyclopedia. . 1983 .

SOLAR WIND - a continuous flow of plasma of solar origin, the Sun) into interplanetary space. At high temperatures, which exist in the solar corona (1.5 * 10 9 K), the pressure of the overlying layers cannot balance the gas pressure of the corona substance, and the corona expands.

The first evidence of the existence of post. plasma flows from the Sun were obtained by L. L. Biermann in the 1950s. on the analysis of forces acting on the plasma tails of comets. In 1957, Yu. Parker (E. Parker), analyzing the conditions of equilibrium of the corona matter, showed that the corona cannot be in hydrostatic conditions. Wed. characteristics of S. v. are given in table. 1. S. flows. can be divided into two classes: slow - with a speed of 300 km/s and fast - with a speed of 600-700 km/s. Fast flows come from regions of the solar corona, where the structure of the magnetic field. fields are close to radial. coronal holes. Slow streamspp. V. are apparently associated with the areas of the crown, in which there is, therefore, Table 1. - Average characteristics of the solar wind in Earth orbit

Speed
Proton concentration
Proton temperature
Electron temperature
Magnetic field strength
Python flux density....	2.410 8 cm -2 c -1
Kinetic energy flux density	0.3 ergcm -2 s -1

Table 2.- Relative chemical composition of the solar wind

	Relative content

	Relative content

In addition to the main components of solar water - protons and electrons; particles were also found in its composition. Measurements of ionization. temperature of ions S. v. make it possible to determine the electron temperature of the solar corona.

In the N. century. differences are observed. types of waves: Langmuir, whistlers, ion-acoustic, waves in plasma). Some of the Alfven type waves are generated on the Sun, and some are excited in the interplanetary medium. The generation of waves smoothes out deviations of the particle distribution function from the Maxwellian one and, in combination with the influence of magnetism. fields to plasma leads to the fact that S. v. behaves like a continuous medium. Alfvén-type waves play a large role in the acceleration of small components of S.

Rice. 1. Massive solar wind. Along the horizontal axis is the ratio of the mass of a particle to its charge, along the vertical axis is the number of particles registered in the energy window of the device in 10 s. Numbers with a “+” sign indicate the charge of the ion.

Stream N. in. is supersonic in relation to the speeds of those types of waves that provide eff. transfer of energy to the S. century. (Alfven, sound). Alfven and sound Mach number C. V. 7. When flowing around the north side. obstacles capable of effectively deflecting it (magnetic fields of Mercury, Earth, Jupiter, Saturn or the conducting ionospheres of Venus and, apparently, Mars), a departing bow shock wave is formed. waves, which allows it to flow around an obstacle. At the same time, in the North century. a cavity is formed - the magnetosphere (either its own or induced), the shape and dimensions of the structure are determined by the magnetic pressure balance. fields of the planet and the pressure of the flowing plasma flow (see. Magnetosphere of the Earth, Magnetospheres of the planets). In case of interaction with S. v. with a non-conducting body (for example, the Moon), a shock wave does not arise. The plasma flow is absorbed by the surface, and a cavity is formed behind the body, gradually filled with plasma C. V.

The stationary process of corona plasma outflow is superimposed by non-stationary processes associated with flares on the Sun. During strong flares, substances are released from the bottom. corona regions into the interplanetary medium. Magnetic variations).

Rice. 2. Propagation of an interplanetary shock wave and ejection from a solar flare. The arrows indicate the direction of motion of the solar wind plasma,

Rice. 3. Types of solutions to the corona expansion equation. The speed and distance are normalized to the critical speed vk and the critical distanceRk. Solution 2 corresponds to the solar wind.

The expansion of the solar corona is described by a system of mass conservation equations, v k) at some critical point. distance R to and subsequent expansion at supersonic speed. This solution gives a vanishingly small value of pressure at infinity, which makes it possible to reconcile it with the low pressure of the interstellar medium. This type of flow was called S. by Yu. Parker. , where m is the proton mass, is the adiabatic exponent, and is the mass of the Sun. In Fig. Figure 4 shows the change in expansion rate from heliocentric. thermal conductivity, viscosity,

Rice. 4. Solar wind speed profiles for the isothermal corona model at different values of coronal temperature.

S.v. provides the basic outflow of thermal energy from the corona, since heat transfer to the chromosphere, el.-magn. coronas and electronic thermal conductivitypp. V. are insufficient to establish the thermal balance of the corona. Electronic thermal conductivity ensures a slow decrease in the ambient temperature. with distance. luminosity of the Sun.

S.v. carries the coronal magnetic field with it into the interplanetary medium. field. The force lines of this field frozen into the plasma form an interplanetary magnetic field. field (IMF). Although the intensity of the IMF is low and its energy density is about 1% of the kinetic density. energy of solar energy, it plays an important role in thermodynamics. V. and in the dynamics of interactions of S. v. with the bodies of the solar system, as well as the streams of the north. among themselves. Combination of expansion of the S. century. with the rotation of the Sun leads to the fact that the mag. the lines of force frozen into the north of the century have the form B R and azimuthal magnetic components. fields change differently with distance near the ecliptic plane:

where is ang. speed of rotation of the Sun, And - radial component of velocityC. c., index 0 corresponds to the initial level. At the distance of the Earth's orbit, the angle between the direction of the magnetic. fields and R about 45°. At large L magnetic.

Rice. 5. Shape of the interplanetary magnetic field line. - angular velocity of rotation of the Sun, and - radial component of plasma velocity, R - heliocentric distance.

S. v., arising over regions of the Sun with different. magnetic orientation fields, speed, temp-pa, particle concentration, etc.) also in cf. change naturally in the cross section of each sector, which is associated with the existence of a fast flow of solar water within the sector. The boundaries of the sectors are usually located within the slow flow of the North century. Most often, 2 or 4 sectors are observed, rotating with the Sun. This structure, formed when the S. is pulled out. large-scalemagn. corona fields, can be observed for several. revolutions of the Sun. The sector structure of the IMF is a consequence of the existence of a current layer (CS) in the interplanetary medium, which rotates together with the Sun. TS creates a magnetic surge. fields - radial IMF have different signs on different sides of the vehicle. This TC, predicted by H. Alfven, passes through those parts of the solar corona that are associated with active regions on the Sun, and separates these regions from the different ones. signs of the radial component of the solar magnet. fields. The TS is located approximately in the plane of the solar equator and has a folded structure. The rotation of the Sun leads to the twisting of the folds of the TC into a spiral (Fig. 6). Being near the ecliptic plane, the observer finds himself either above or below the TC, due to which he falls into sectors with different signs of the IMF radial component.

Near the Sun in the north. there are longitudinal and latitudinal gradients of the velocity of collisionless shock waves (Fig. 7). First, a shock wave is formed, propagating forward from the boundary of the sectors (direct shock wave), and then a reverse shock wave is formed, propagating towards the Sun.

Rice. 6. Shape of the heliospheric current layer. Its intersection with the ecliptic plane (inclined to the solar equator at an angle of ~ 7°) gives the observed sector structure of the interplanetary magnetic field.

Rice. 7. Structure of the interplanetary magnetic field sector. Short arrows show the direction of the solar wind, arrowed lines indicate magnetic field lines, dash-dotted lines indicate the boundaries of the sector (the intersection of the drawing plane with the current layer).

Since the speed of the shock wave is less than the speed of the solar wind, it carries the reverse shock wave in the direction away from the Sun. Shock waves near sector boundaries are formed at distances of ~1 AU. e. and can be traced to distances of several. A. e. These shock waves, as well as interplanetary shock waves from solar flares and circumplanetary shock waves, accelerate particles and are, therefore, a source of energetic particles.

S.v. extends to distances of ~100 AU. e., where the pressure of the interstellar medium balances the dynamic. blood pressure The cavity swept by the S. v. Interplanetary environment). ExpandingS. V. along with the magnet frozen into it. field prevents the penetration of galactic particles into the solar system. space rays of low energies and leads to cosmic variations. high energy rays. A phenomenon similar to the S.V. has been discovered in some other stars (see. Stellar wind).

Lit.: Parker E. N., Dynamics in the interplanetary medium, O. L. Weisberg.

Physical encyclopedia. In 5 volumes. - M.: Soviet Encyclopedia. Editor-in-chief A. M. Prokhorov. 1988 .

See what "SOLAR WIND" is in other dictionaries:

SOLAR WIND, a stream of plasma from the solar corona that fills the Solar System up to a distance of 100 astronomical units from the Sun, where the pressure of the interstellar medium balances the dynamic pressure of the stream. The main composition is protons, electrons, nuclei... Modern encyclopedia

SOLAR WIND, a steady stream of charged particles (mainly protons and electrons) accelerated by the heat of the solar CORONA to speeds high enough for the particles to overcome the Sun's gravity. The solar wind deflects... Scientific and technical encyclopedic dictionary

The sun is a source of a constant stream of particles. Neutrinos, electrons, protons, alpha particles, and heavier atomic nuclei all together make up the corpuscular radiation of the Sun. A significant part of this radiation is a more or less continuous outflow of plasma, the so-called solar wind, which is a continuation of the outer layers of the solar atmosphere - the solar corona. Near the Earth, its speed is usually 400–500 km/s. A stream of charged particles is ejected from the Sun through coronal holes - regions in the Sun's atmosphere with a magnetic field open into interplanetary space.

The first measurements of the solar wind were made in 1959 on the Luna-9 probe. In 1962, Mariner 2, heading towards Venus, made observations of the solar wind and obtained the following results: the speed of the solar wind varied from 350 m/s to 800 m/s, the average concentration of solar wind was 5.4 ions per 1 cm3 , ion temperature 160,000 K. Average magnetic field strength 6*10–5 oersted.

The international space station SOHO has discovered a lot of new information about the solar wind. It turned out that it transports elements such as nickel, iron, silicon, sulfur, calcium, and chromium.

The sun rotates with a period of 27 days. The trajectories of solar wind particles moving along magnetic field induction lines have a spiral structure due to the rotation of the Sun. As a result of the rotation of the Sun, the geometric shape of the solar wind flow will be an Archimedean spiral, reminiscent of the shape of a stream of water from a garden hose rotating around an axis.

On days of solar storms, the solar wind increases sharply. It causes auroras and magnetic storms on Earth, and astronauts should not go into outer space at this time.

Under the influence of the solar wind, the tails of comets are always directed away from the Sun. The Voyager spacecraft detected solar wind even beyond the orbit of Pluto. In fact, we live in a giant heliosphere formed by the solar wind, although we are protected from it by the Earth's magnetic field.

The sun is a powerful source of radio emission. Centimeter-scale radio waves emitted by the chromosphere and longer waves emitted by the corona penetrate into interplanetary space.

If the Sun emits relatively stable radiation in visible rays (changes occur by fractions of a percent), then in the radio range the radiation can change hundreds and even thousands of times. Radio emission from the Sun has two components - constant and variable. The constant component characterizes the radio emission of the quiet Sun. The solar corona emits radio waves as a completely black body with a temperature T = 106 K. The variable component of radio emission from the Sun manifests itself in the form of bursts and noise storms. Noise storms last from several hours to several days. 10 minutes after a strong solar flare, radio emission from the Sun increases thousands and even millions of times compared to radio emission from the quiet Sun and lasts from several minutes to several hours. This radio emission is non-thermal in nature.

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People are getting more and more attention interesting facts about the solar wind. What is this phenomenon? In the late 1940s, savvy astrophysicists concluded that the Sun was collecting gases from interstellar space. For this reason, the theory was put forward about the existence of wind directed towards the sun. After some time, scientists were even able to confirm the existence of the solar wind, but with a slight amendment: the wind comes from the Sun in different directions. Let's look at some interesting facts about this phenomenon:

First of all, you need to know that the definition of “solar wind” describes an astrophysical phenomenon, not a meteorological one. This process is a continuous radiation of plasma into the surrounding space. Through this wind, the Sun seems to remove the excess energy contained in it.
In fact, instead of accumulating substances from the surrounding outer space, the Sun throws out in different directions the substance it contains in a volume equal to one million tons per period corresponding to one revolution of the Earth around its axis.
The speed of particles moving away from the Sun is constantly increasing, since they are pushed by similar matter, the temperature of which is much higher. In addition, the force of attraction of the Sun gradually ceases to act on plasma particles, which are components of the flows.
3
At approximately 20,000 km from the surface, the speed of plasma particles can correspond to tens of thousands of meters per second. After traveling a distance corresponding to several diameters of the sun, the speed of the plasma particles becomes a thousand times greater. Near our planet, this speed becomes hundreds of times higher, and their density becomes much lower than that of the atmosphere.
4
The flow mostly includes protons and electrons, but it also contains nuclei of helium and other elements.
5
The temperature of plasma particles located at the very beginning of the solar wind flows corresponds to approximately two million degrees Kelvin. As you move away, the temperature first increases to 20 million degrees and only then begins to decrease. When the wind flows reach our planet, the plasma particles cool to about 10,000 degrees.
When solar flares occur, the temperature of the plasma near the Earth corresponds to 100 thousand degrees.
7
Our planet's magnetic field protects us well from this radiation. Streams of solar winds literally flow around the earth's atmosphere and sweep further into the surrounding space, gradually reducing their density.
From time to time, the intensity of passing streams of plasma particles is so high that the atmosphere of our planet has difficulty reflecting their impact. Naturally, the solar wind flows recede, but only after some time.
9
When powerful streams of solar winds interact intensively with the magnetic field of our planet, we can observe auroras in the polar regions, as well as record the formation of magnetic storms.
10
The distribution of solar winds cannot be called uniform. The distribution speed can reach its maximum when the wind passes over the so-called coronal holes. The slowest flow of streams can be recorded above streamers. Streams with different flow rates intersect with each other and with our planet.
11
We have learned to obtain the greatest amount of information about the solar wind thanks to specially designed spacecraft. The list of such technological devices includes the well-known Ulysses satellite, thanks to which our knowledge of the solar wind has changed significantly. The chemical composition and speed of plasma flows were studied thanks to such a remarkable device. Additionally, with the help of the satellite, it was possible to determine the level of the magnetic field of our planet.
Another ACE satellite was launched into orbit back in 1997 near the L1 Lagrange point. It is at this point that solar and earth's gravity are in balance. On board this machine there are devices that continuously monitor the flow of solar winds so that people can explore information about directional plasma particles in real time, limited to the territory of the L1 sector.
Recently, the solar wind caused a geomagnetic storm on Earth. Intense flows emerged from the coronary hole in the solar atmosphere. Such holes can form in the luminary even in cases where there is a complete absence of active zones.
Today, a coronal hole has formed on the Sun.. Streams of plasma particles with a high distribution density reached the planet by mid-June, which caused the development of geomagnetic storms.

The atmosphere of the Sun is 90% hydrogen. The part farthest from the surface is called the solar corona, and is clearly visible during total solar eclipses. The temperature of the corona reaches 1.5-2 million K, and the corona gas is completely ionized. At this plasma temperature, the thermal speed of protons is about 100 km/s, and that of electrons is several thousand kilometers per second. To overcome solar gravity, an initial speed of 618 km/s is sufficient, the second cosmic speed of the Sun. Therefore, plasma is constantly leaking from the solar corona into space. This flow of protons and electrons is called the solar wind.

Having overcome the gravity of the Sun, solar wind particles fly along straight trajectories. The speed of each particle almost does not change with distance, but it can be different. This speed depends mainly on the state of the solar surface, on the “weather” on the Sun. On average it is equal to v ≈ 470 km/s. The solar wind travels the distance to Earth in 3-4 days. In this case, the density of particles in it decreases in inverse proportion to the square of the distance to the Sun. At a distance equal to the radius of the earth's orbit, 1 cm 3 on average there are 4 protons and 4 electrons.

The solar wind reduces the mass of our star - the Sun - by 10 9 kg per second. Although this number seems large on an earthly scale, in reality it is small: the loss of solar mass can only be noticed over times thousands of times greater than the modern age of the Sun, which is approximately 5 billion years.

The interaction of the solar wind with the magnetic field is interesting and unusual. It is known that charged particles usually move in a magnetic field H in a circle or along helical lines. This is true, however, only when the magnetic field is strong enough. More precisely, for charged particles to move in a circle, it is necessary that the energy density of the magnetic field H 2 /8π be greater than the kinetic energy density of the moving plasma ρv 2 /2. In the solar wind the situation is the opposite: the magnetic field is weak. Therefore, charged particles move in straight lines, and the magnetic field is not constant, it moves along with the flow of particles, as if carried away by this flow to the periphery of the Solar system. The direction of the magnetic field throughout interplanetary space remains the same as it was on the surface of the Sun at the moment the solar wind plasma emerged.

When traveling along the equator of the Sun, the magnetic field usually changes its direction 4 times. The sun rotates: points on the equator complete a revolution in T = 27 days. Therefore, the interplanetary magnetic field is directed in spirals (see figure), and the entire pattern of this figure rotates following the rotation of the solar surface. The angle of rotation of the Sun changes as φ = 2π/T. The distance from the Sun increases with the speed of the solar wind: r = vt. Hence the equation of the spirals in Fig. has the form: φ = 2πr/vT. At a distance of the earth's orbit (r = 1.5 10 11 m), the angle of inclination of the magnetic field to the radius vector is, as can be easily verified, 50°. On average, this angle is measured by spacecraft, but not very close to the Earth. Near the planets, the magnetic field is structured differently (see Magnetosphere).