"Life with a star" - part 1: solar activity
The night from the 1st to the 2nd of September 1859 marked itself as the largest aurora, in the entire history of astronomical observations - it could be observed throughout the entire territory of the Earth. In the circumpolar regions, with its light it was possible to read, it was so bright - that it woke the miners in the Rocky Mountains . Most telegraphs in Europe and North America are out of order, and on telegraph poles - witnesses observed sparks. Evaluation of the consequences of such an event (if it happens in the modern world, with centralized electrical networks) gives damage values of $ 0.6-2.6 trillion, only for the USA . Such was the most destructive manifestation of space weather at the moment, recorded by mankind.
In the first part of the article - I will describe the phenomena of solar activity that underlie the "space weather" , and for this, in turn, we will need to delve into the structure of the Sun, which looks like this: The solar core - occupies the zone from the center to 0.25 radius of the sun. Here is a zone with a maximum temperature (about 15 million K), pressure (about 250 billion atmospheres), and density (reaching 150 g / cm 3 ). Since the rate of thermonuclear reactions strongly depends on temperature - the main part of the energy release in the Sun, it is in this area. However, even with such indicators - the rate of thermonuclear reactions is not very high (about 275 watts / m 3 ), therefore thermonuclear reactors, such as ITER
- require an order of magnitude greater temperatures in order to have reasonable indicators in terms of volume / power.
The zone of radiative transfer - extends from a depth of 0.25, to about 0.7 of the radius of the sun. It is called so - because the main method of energy transfer in it is the sequential emission and absorption of photons. This is a fairly calm zone in which the main type of movement is rotational: the Sun makes about one revolution in 25.6 days along the equatorial line (for an observer on Earth, taking into account our rotation around the Sun, it goes out approximately 28 days), and 33.5 day at the pole level. The radiant zone, in this case - has approximately averaged (between these two) speeds.
Tahoklin- the transition region located between the radiant and convective zones, its thickness is approximately 0.04 of the radius of the sun. In this area, there is a transition from radiant (quiet) heat transfer to convective (turbulent), and from "solid-state rotation" (when the layers rotate at a uniform frequency) - to the differential (differing in polar and equatorial regions).
The reasons for this transition are as follows: at the border of about 0.7 times the radius of the sun - the gradual drop in temperature and pressure of the solar layers leads to the fact that physical conditions no longer allow plasma atoms to be sustained without electrons (hydrogen atoms once ionized and helium twice). Accordingly, the photo effect begins to act.and the substance ceases to be transparent. Radiant transfer loses its efficiency, and convective heat transfer comes first.
The explanation of the source of the second effect is a much more complex task, and its solution has not been given to scientists for a long time. But in 2013, using the data of the Solar Dynamics Observatory , the connection between convective motion on the Sun (which is chaotic on small scales) and stable, differential rotation of the Sun was also shown : The key factors in understanding the processes occurring on the Sun are:
1) The source of energy for the occurrence of all processes recorded on the Sun is turbulent convection (and its source is the temperature gradient between the solar core, in which thermonuclear reactions take place, and the surface of the Sun through which this energy is emitted).
2) Almost all matter on the Sun (with the exception of a certain fraction of hydrogen in the photosphere) is in a state of plasma . For this reason, energy transfer occurs at the expense of the kinetic energy of convective currents, and at the expense of the electromagnetic field . At the same time, energy can freely transfer from one type to another (plasma movement can generate a magnetic field, and in another case, a magnetic field can accelerate plasma flows).
Convective zone- a zone located at a distance of about 0.7 radius, and directly to the most visible surface. In the absence of other possibilities, heat transfer from this level begins to occur due to the mixing of the layers (that is, convection, which is why this zone itself was named so). It is this zone that is responsible for all the phenomena that are called “solar activity” . The main structure of the convective zone (and the visible "surface" of the Sun) - consists of granules (with a typical diameter of 1000 km, and a lifetime of 8 to 20 minutes), and supergranules
(size of 30 thousand km, and a lifetime of about a day). Granular structure - consists of bright areas (where matter rises from the depths of the Sun) and dark gaps between them (where matter falls, respectively). The vertical speed of a substance is 1-2 km / s, and the depth of the granules is hundreds and thousands of kilometers. Sunspots
These are areas in which strong magnetic fields impede the convective movement of matter. In spite of the name, they can be called “spots” with a big stretch: the temperature inside them is 3000-4500 K. And their visible blackness is explained by the temperature of the surrounding substance (averaging 5780 K), and, accordingly, by a much lower emission of light by “spots” external background. Practically from the beginning of systematic observations of sunspots in 1749 - they became the main evidence for the existence of an 11-year cycle of solar activity (therefore, the one that was running at that moment — it started in 1745) was chosen as the zero cycle:
To be more precise, the cycle has an average duration of about 11.2 years, and varies in the range from 7 to 17 years (the shorter the cycle, the more powerful it is). The growth stage in the cycle takes a shorter period of time (4.6 years, versus 6.7 years - on average, at the recession stage). At the beginning of the cycle spots appear at latitudes of about ± 35-40 °, then shifted to the area of ± 15 ° in the maximum period and the end of the cycle - the majority of them are found at latitudes of ± 5-8 ° (the so-called spörer's law ): This cyclicity in the behavior and number of sunspots — associated with an 11-year cycle of changing the magnetic poles of the Sun (with a full cycle of changing polarity north / south — it takes 22 years, respectively). However, this 22-year period ( the Hale cycle
) - did not receive wide popularity, since besides the change of polarity, it doesn’t practically manifest itself.
The availability of statistics for 400+ years suggested the existence of a century-old solar activity cycle (the so-called Gleissberg cycle - lasting in the range of 70-100 years, with an average value of 87 years). But it was really possible to prove its presence - only with the advent of radiocarbon analysis: the fact is that during periods of solar maximum the solar wind becomes denser and the solar heliosphere expands a bit (this was the basis of reports of Voyager-1 out of the solar system: 1 , 2 , 3 , 4 ), with the flow of galactic cosmic rays- reduced, and with it reduced production of radioactive carbon-14 in the upper atmosphere. Traces of these changes over the past 11 thousand years are found in ice cores and tree rings :
Sunspots are often formed in groups, with the leading spot having the same polarity as the current polarity of the hemisphere, and the back polarity. A group of sunspots can exist from several hours to several months (a long-term, 27-day forecast is based on this — when spots that have made one revolution return to the same position as they are now).
Solar torches- are a kind of “spots per revolution”: in this case, the magnetic field acts as an amplifier of convection, which in turn raises the temperature and luminosity of the “surface” of the Sun.
The protuberances are formations of a bizarre form, in a stable state resembling a torus half , resting on the "surface" of the Sun:
They are due to a magnetic field, which is their source: a flow of matter moving along magnetic lines - rises from the depths of the Sun at the beginning, then describes an arc and falls back on the sun. Such fountains of substance - can exist up to months. They can be huge energy, which can be released in two physical phenomena, which will be discussed below.
The sun, a large prominence and Jupiter with the Earth - on a scale of
solar flares - are gigantic emissions of energy (the largest of which is described at the beginning of this article). During a typical flare, energy can be released on the order of 10 20 J (about 10 gigatons in TNT equivalent), in large - about 10 25 J (about 1 billion megatons). Their source is the reconnection of magnetic fields on the Sun (when two magnetic “rings” are in contact with each other, and drastically change their structure):
Accurate evidence of such a process was obtained quite recently . During a solar flare, energy is emitted throughout the entire spectrum of electromagnetic radiation, most of it is emitted in a hard ultraviolet, as well as x-rays and gamma rays (this is due to the fact that magnetic fields in the process of reconnection heat the plasma to tens of millions of degrees). Only a small part of the energy is released in the visible range of light, so in the usual situation - they are not visible. But in the case of the Carrington event - a flash could be observed even with the naked eye.
The intensity of the flashes is divided into five classes: A, B, C, M, X. Each succeeding class is ten times more powerful than the previous one. Each class is divided into a linear scale from 1.0 to 9.9, the class X does not have an upper limit: at the moment the most powerful flash recorded since 1957 (when extraatmospheric observations began, and the full power over the entire emission spectrum became possible to establish) November 4, 2003 , and according to updated data - had a class X45.
| Flash class | Intensity in gamma rays 0.5-8 Å, W \ m 2 |
|---|---|
| A | up to 10 -7 |
| B | from 10 -7 to 10 -6 |
| C | from 10 -6 to 10 -5 |
| M | from 10 -5 to 10 -4 |
| X | more than 10 -4 |
Coronal ejection model
The latest computer models with high accuracy describe the processes occurring on the Sun - this allows us to hope that soon a period of accurate forecasts for space weather can be obtained not in 3 days - but over a period considerably longer.Comparison of the model with real coronal ejection
The photosphere is the visible "surface" of the sun. It is about 300 km in thickness, and it is in it that most of the visible spectrum is emitted. The density of this layer is from 10 -8 to 10 -9 g \ cm 3 . It is here that the minimum temperature of the Sun is reached (4300 K), but the average temperature of this area is close to 5777 K:
Actually being a continuation of the convective zone - the photosphere is visible (for us) a reflection of those phenomena and the structure that exists in the convective zone ( which is described above).
The chromosphere is a layer about 10 thousand km thick, located between the photosphere and the corona. Here the pressure starts to drop sharply, and the temperature starts to rise again:
Due to the fact that the pressure in this layer is very low - its luminosity (despite the rise in temperature) is hundreds of times less than that of the photosphere. For this reason, it was first discovered due to lunar eclipses (when the light from the photosphere did not interfere with the observation of this layer). It was in this region of the Sun that helium was first discovered.
The chromosphere mainly consists of spicules - objects of oblong shape, having several thousand kilometers in diameter, and about a thousand in depth:
Rising from the photosphere - they transport matter into the upper layers of the Sun. Another component of the chromosphere is fibrils. They are vertical loops of matter, carried away by a magnetic field (by the type of prominences).
Crown- starts from the apparent radius of the Sun, and extends to 10-20 of its diameter. Consists of a very rarefied and unevenly distributed substance, with a temperature in excess of one million kelvin. The source of such a high temperature of the corona, according to the latest data , is chromospheric spicules, which feed it with high-energy particles. The structure of the corona strongly depends on the period of solar activity: at the time of the maxima - it has a spherical shape, at the time of the minima - extended along the equator direction: The solar wind is a stream of highly rarefied solar matter, with a temperature close to the coronal, moving at high speed (in orbit Earth - its speed is 300-400 km / s):
This substance is accelerated by the magnetic fields of the Sun (this is the reason for the high difference in speed between the equator and the poles). The pressure produced by them is 1-6 nPa in the Earth's orbit (depending on the period of the 11-year cycle and the presence of coronal emissions). Through the solar wind - the Sun loses about 10 -14 M C (this is several orders of magnitude less than what it loses due to radiation).
P.S. In the second part of the article - about the space weather, the devices exploring the Sun and services that monitor its condition.