About the planets
We begin to study astronomy in high school. By this time, children already know that there are planets in the solar system, their names, movement and location, and approximate sizes. They are helped in this by photos and videos, which they sometimes watch on TV or on the Internet over the years. However, this knowledge is obtained fragmentarily and incoherently.
In high school, teachers try to collect them into a single system, but without a good base this works poorly.
We suggest that you master the names, movements and number of planets already in early childhood. The fascinating cartoon presented on the site will help us with this. The information that photos and videos provide in it will be useful even for adults. So watch it with the whole family!
For example, do you know the sizes of the planets? And their number?
How many planets are there in the Solar System?
It's easy to count: there are only nine of them.
The ninth planet, Pluto (visible in photos and videos), is the farthest and until recently was actually considered a planet. However, in the 21st century, scientists have proven that it is not a planet. So now the farthest planet is Neptune.
Now to the question: how many planets are there in the Solar System? – you can answer: eight.
The planets move not only around their own axis, but also around the Sun. Thanks to this, the seasons and time of day change on Earth. Movement around the Sun and its axis causes similar changes on other planets. The time taken to move will be different on other planets. For example, Mercury revolves around the Sun for 87 days, and around its axis for 58 days.
Like the movement of the planets, their sizes also differ significantly. The smallest planet in the Solar System is Mercury. The largest planet in the Solar System is Jupiter. This is a large planet surrounded by 4 satellites. You can also see them in the video and photo. The sizes of celestial bodies are measured by their diameter.
The temperature on the surface of planets also fluctuates significantly. Thus, the hottest planet is Mercury (daytime temperatures reach 350 degrees). It is closest to the Sun. And the coldest Neptune is also the farthest.
In the video and photo presentation of “Planets of the Solar System” for children, kids will see not only the movement of planets, but also other celestial bodies: stars, satellites, asteroids, meteorites. They are also in the photo.
Kids will be able to observe the movement of the Moon around the Earth. In the photo, this celestial body is presented more closely, and you can see the relief of the lunar surface. And although children observe it in the sky every day, it would be a good idea for them to study the Moon from a scientific point of view.
This is the basic information that children should know about the planets. In the presentation you will learn a lot more interesting things about the satellites of the planets, about the asteroid ring, about the structure of space in general.
Presentation "Solar System"
#Teaching materials #Presentation #All teachers #School education
SOLAR SYSTEM PRESENTATION MADE BY GVALDIN ALEXANDER
CONTENTS 1 SOLAR SYSTEM 2 LOCATION OF PLANETS 3 SUN 4 SUN-SOURCE OF ENERGY 5 SOLAR ECLIPSE 6 SUNSPOT 7 TERRESTRIAL PLANETS 8 MERCURY 9 GENERAL CHARACTERISTICS OF MERCURY 10 PHYSICAL CHARACTERISTICS STICKS 11 SURFACE OF MERCURY 12 VENUS 13 GENERAL CHARACTERISTICS OF VENUS 14 SURFACE OF VENUS 15 CLIMATE OF VENUS 16 EARTH 17 GENERAL CHARACTERISTICS OF THE EARTH 18 STRUCTURE OF THE EARTH 19 TECTONIC PLATFORMS 20 ROTATION OF THE EARTH 21 MOON 22 MOVEMENT OF THE MOON 23 WATER ON THE MOON 24 MARS 25 CHARACTERISTICS OF MARS 26 JUPITER 27 CHARACTERISTICS OF JUPITER 28 PAIRS AMETERS OF JUPITER 29 THE GREAT RED SPOT 30 SATURN 31 CHARACTERISTICS OF SATURN 32 RINGS 33 URANUS 34 CHARACTERISTICS URANUS 35 NEPTUNE 36 CHARACTERISTICS OF NEPTUNE 37 PLUTO 38 CHARACTERISTICS OF PLUTO
SOLAR SYSTEM The solar system is a planetary system that includes the central star - the Sun - and all the natural space objects orbiting around it. Most of the mass of objects bound to the Sun by gravity is contained in eight relatively solitary planets, which have almost circular orbits and are located within an almost flat disk - the ecliptic plane. The four smaller inner planets: Mercury, Venus, Earth and Mars, also called the terrestrial planets, are composed primarily of silicates and metals. The four outer planets: Jupiter, Saturn, Uranus and Neptune, also called gas giants, are largely composed of hydrogen and helium and are much more massive than the terrestrial planets. The Solar System also has two regions filled with small bodies. The main asteroid belt, located between Mars and Jupiter, is similar in composition to the terrestrial planets, since it also consists of silicates and metals. Beyond Neptune's orbit are trans-Neptunian objects consisting of frozen water, ammonia and methane. In these regions, five individual objects - Ceres, Pluto, Haumea, Makemake and Eris - are large enough to maintain a nearly round shape under the influence of their own gravity, they are called dwarf planets. In addition to the thousands of small bodies in these two regions, other diverse populations of small bodies such as comets, meteoroids, and cosmic dust move throughout the Solar System. Six of the eight planets and three dwarf planets are surrounded by natural satellites. Each of the outer planets is surrounded by rings of dust and other particles. The solar wind (the flow of plasma from the Sun) creates a bubble in the interstellar medium called the heliosphere that extends to the edge of the diffuse disk. The hypothetical Oort cloud, which serves as a source of long-period comets, could extend over a distance of about a thousand times greater than the heliosphere. The solar system is part of the Milky Way galaxy.
LOCATION OF PLANETS
THE SUN The Sun is the central and only star of the Solar System, around which other objects of this system revolve: planets and their satellites, dwarf planets and their satellites, asteroids, meteoroids, comets and cosmic dust. The mass of the Sun is 99.8% of the total mass of the entire solar system. Solar radiation supports life on Earth (photons are necessary for the initial stages of the photosynthesis process) and determines climate. The sun consists of hydrogen (~73% of mass and ~92% of volume), helium (~25% of mass and ~7% of volume[5]) and the following elements, which are included in its composition in small concentrations: iron, nickel, oxygen, nitrogen, silicon, sulfur, magnesium, carbon, neon, calcium and chromium[6]. According to the spectral classification, the Sun belongs to the G2V type (“yellow dwarf”). The surface temperature of the Sun reaches 6000 K, so the Sun shines with almost white light, but due to stronger scattering and absorption of the short-wave part of the spectrum by the Earth's atmosphere, the direct light of the Sun at the surface of our planet acquires a certain yellow tint.
THE SUN IS A SOURCE OF ENERGY Radiation from the Sun is the main source of energy on Earth. Its power is characterized by the solar constant - the amount of energy passing through a unit area area perpendicular to the sun's rays. At a distance of one astronomical unit (that is, in Earth's orbit), this constant is approximately 1370 W/m². Passing through the Earth's atmosphere, solar radiation loses approximately 370 W/m² in energy, and only 1000 W/m² reaches the earth's surface (in clear weather and when the Sun is at its zenith). This energy can be used in various natural and artificial processes. Thus, plants process it into chemical form (oxygen and organic compounds) using photosynthesis. Direct heating by the sun's rays or energy conversion using photocells can be used to generate electricity (solar power plants) or perform other useful work. In the distant past, energy stored in oil and other types of fossil fuels was also obtained through photosynthesis.
SOLAR ECLIPSE A solar eclipse is an astronomical phenomenon in which the Moon covers (eclipses) completely or partially the Sun from an observer on Earth. A solar eclipse is only possible during new moons, when the side of the Moon facing the Earth is not illuminated and the Moon itself is not visible. The Moon's shadow on the earth's surface does not exceed 270 km in diameter and therefore a solar eclipse is observed only in a narrow strip along the path of the shadow. Since the Moon revolves in an elliptical orbit, the distance between the Earth and the Moon at the time of an eclipse can be different; accordingly, the diameter of the lunar shadow spot on the Earth’s surface can vary widely from maximum to zero (when the top of the lunar shadow cone does not reach the Earth’s surface). If the observer is in the shadow, he sees a total solar eclipse in which the Moon completely hides the Sun, the sky darkens, and planets and bright stars may appear on it. Around the solar disk hidden by the Moon, you can observe the solar corona, which is not visible in the normal bright light of the Sun. When an eclipse is observed by a stationary ground-based observer, the total phase lasts no more than a few minutes. The minimum speed of movement of the lunar shadow on the earth's surface is just over 1 km/s. During a total solar eclipse, astronauts in orbit can observe the running shadow of the Moon on the Earth's surface.
SUNSPOTS Sunspots are dark areas on the Sun, the temperature of which is lower by about 1500 K compared to the surrounding areas of the photosphere. They are observed on the solar disk (using optical instruments, and in the case of large sunspots, with the naked eye) in the form of dark spots. Sunspots are areas where strong (up to several thousand gauss) magnetic fields enter the photosphere. The darkening of the photosphere in spots is due to the suppression by the magnetic field of convective movements of matter and, as a consequence, a decrease in the flux of thermal energy transfer in these areas. The number of sunspots (and the associated Wolf number) is one of the main indicators of solar magnetic activity.
TERRESTRIAL PLANETS The four inner planets consist predominantly of heavy elements, have a small number (0-2) of satellites, and have no rings. They are largely composed of refractory minerals such as silicates, which form their mantle and crust; and metals such as iron and nickel that form their core. The three inner planets—Venus, Earth, and Mars—have atmospheres; all have impact craters and tectonic surface features such as rift basins and volcanoes.
MERCURY Mercury is the planet closest to the Sun in the Solar System, orbiting the Sun in 88 Earth days. Mercury is classified as an inner planet because its orbit is closer to the Sun than the main asteroid belt. After Pluto was deprived of its planetary status in 2006, Mercury acquired the title of the smallest planet in the solar system. Mercury's apparent magnitude ranges from −2.0 to 5.5, but it is not easily visible due to its very small angular distance from the Sun (maximum 28.3°). At high latitudes, the planet can never be seen in the dark night sky: Mercury is always hidden in the morning or evening dawn. The optimal time for observing the planet is morning or evening twilight during periods of its elongations (periods of maximum distance of Mercury from the Sun in the sky, occurring several times a year ). It is convenient to observe Mercury at low latitudes and near the equator: this is due to the fact that the duration of twilight there is shortest. In mid-latitudes it is much more difficult to find Mercury and only during the period of the best elongations, and in high latitudes it is impossible at all.
GENERAL CHARACTERISTICS OF MERCURY
PHYSICAL CHARACTERISTICS Mercury is the smallest terrestrial planet. Its radius is only 2439.7 ± 1.0 km, which is less than the radius of Jupiter's moon Ganymede and Saturn's moon Titan. The mass of the planet is 3.3×1023 kg. The average density of Mercury is quite high - 5.43 g/cm³, which is only slightly less than the density of Earth. Considering that the Earth is larger in size, the density value of Mercury indicates an increased content of metals in its depths. The acceleration of gravity on Mercury is 3.70 m/s². The second escape velocity is 4.3 km/s. The proximity to the Sun and the rather slow rotation of the planet, as well as the lack of an atmosphere, lead to the fact that Mercury experiences the most dramatic temperature changes in the Solar System. The average daytime surface temperature is 623 K (349.9 °C), while the nighttime temperature is only 103 K (-170.2 °C). The minimum temperature on Mercury is 90 K (-183.2 °C), and the maximum reached at noon at “hot longitudes” when the planet is near perihelion is 700 K (426.9 °C).
SURFACE OF MERCURY The surface of Mercury is in many ways reminiscent of the Moon - it is dotted with many craters. The density of craters varies in different areas. It is assumed that the more densely dotted areas with craters are more ancient, and the less densely dotted ones are younger, formed when the old surface was flooded with lava. At the same time, large craters are less common on Mercury than on the Moon. The largest crater on Mercury is named after the great German composer Beethoven, its diameter is 625 km. However, the similarity is incomplete - formations are visible on Mercury that are not found on the Moon. An important difference between the mountainous landscapes of Mercury and the Moon is the presence on Mercury of numerous jagged slopes stretching for hundreds of kilometers - scarps. A study of their structure showed that they were formed during compression that accompanied the cooling of the planet, as a result of which the surface of Mercury decreased by 1%. The presence of well-preserved large craters on the surface of Mercury suggests that over the past 3-4 billion years there has been no large-scale movement of sections of the crust, and there was no erosion of the surface; the latter almost completely excludes the possibility of the existence of any significant atmosphere.
VENUS Venus is the second inner planet of the Solar System with an orbital period of 224.7 Earth days. The planet got its name in honor of Venus, the goddess of love from the Roman pantheon. Venus is the third brightest object in the Earth's sky after the Sun and Moon and reaches an apparent magnitude of −4.6. Because Venus is closer to the Sun than Earth, it never appears too far from the Sun: the maximum angular distance between it and the Sun is 47.8°. Venus reaches its maximum brightness shortly before sunrise or some time after sunset, which gives rise to the name it is also called the Evening Star or the Morning Star. Venus is classified as an Earth-like planet and is sometimes called "Earth's sister" because the two planets are similar in size, gravity, and composition. However, the conditions on the two planets are very different. The surface of Venus is hidden by extremely thick clouds of sulfuric acid clouds with high reflective characteristics, which makes it impossible to see the surface in visible light (but its atmosphere is transparent to radio waves, with the help of which the planet's topography was subsequently studied). Disputes about what lies beneath the thick clouds of Venus continued until the twentieth century, until many of the secrets of Venus were revealed by planetary science. Venus has the densest atmosphere of any Earth-like planet, consisting mainly of carbon dioxide. This is explained by the fact that on Venus there is no carbon cycle and no organic life that could process it into biomass.
GENERAL CHARACTERISTICS OF VENUS
SURFACE OF VENUS Exploration of the surface of Venus became possible with the development of radar methods. The most detailed map was compiled by the American Magellan spacecraft, which photographed 98% of the planet's surface. Mapping has revealed extensive elevations on Venus. The largest of them are the Land of Ishtar and the Land of Aphrodite, comparable in size to the earth’s continents. Numerous craters have also been identified on the surface of the planet. They probably formed when Venus's atmosphere was less dense. A significant part of the planet's surface is geologically young (about 500 million years old). 90% of the planet's surface is covered with solidified basaltic lava. In 2009, a map of the southern hemisphere of Venus was published using the Venus Express apparatus. Based on the data from this map, hypotheses arose about the presence of oceans of water and strong tectonic activity on Venus in the past. Several models of the internal structure of Venus have been proposed. According to the most realistic of them, Venus has three shells. The first - the crust - is approximately 16 km thick. Next is the mantle, a silicate shell that extends to a depth of about 3,300 km to the border with the iron core, the mass of which is about a quarter of the total mass of the planet. Since the planet’s own magnetic field is absent, it should be assumed that in the iron core there is no movement of charged particles - an electric current causing a magnetic field, therefore, there is no movement of matter in the core, that is, it is in a solid state. The density in the center of the planet reaches 14 g/cm³. It is interesting that all the details of the relief of Venus bear female names, with the exception of the highest mountain range of the planet, located on Ishtar Earth near the Lakshmi Plateau and named after James Maxwell.
CLIMATE OF VENUS Calculations show that in the absence of an atmosphere the maximum surface temperature of Venus would not exceed 80 °C. In reality, the temperature on the surface of Venus (at the average radius of the planet) is about 750 K (475 °C), and its daily fluctuations are insignificant. The pressure is about 93 atm, the gas density is almost two orders of magnitude higher than in the Earth's atmosphere. The establishment of these facts was a disappointment for many researchers, who believed that on this planet, so similar to ours, conditions were close to those that were on Earth during the Carboniferous period, and therefore, a similar biosphere could exist there. The first temperature determinations seemed to be able to justify such hopes, but refinements (in particular, with the help of landers) showed that, thanks to the greenhouse effect near the surface of Venus, any possibility of the existence of liquid water was excluded. This effect in the planet’s atmosphere, leading to strong heating of the surface, is created by carbon dioxide and water vapor, which intensively absorb infrared (thermal) rays emitted by the heated surface of Venus. Temperature and pressure first fall with increasing altitude. The minimum temperature of 150–170 K (−125…−105 °C) was determined at an altitude of 60–80 km [5], and with further rise the temperature increases, reaching 310–345 K (35–70 °C) at an altitude of 90–120 km C)[6]. The wind, which is very weak at the surface of the planet (no more than 1 m/s), near the equator at an altitude of over 50 km intensifies to 150-300 m/s. Observations from automatic space stations detected thunderstorms in the atmosphere.
EARTH Earth (lat. Terra) is the third planet from the Sun in the Solar System, the largest in diameter, mass and density among the terrestrial planets. Most often referred to as Earth, planet Earth, World. The only currently known body of the Solar System in particular and the Universe in general, inhabited by living beings. Scientific evidence indicates that the Earth formed from the Solar Nebula about 4.54 billion years ago, and shortly thereafter acquired its only natural satellite, the Moon. Life appeared on Earth about 3.5 billion years ago. Since then, the Earth's biosphere has significantly changed the atmosphere and other abiotic factors, causing the quantitative growth of aerobic organisms, as well as the formation of the ozone layer, which, together with the Earth's magnetic field, weakens harmful solar radiation, thereby maintaining conditions for life on Earth. The Earth's crust is divided into several segments, or tectonic plates, that gradually migrate across the surface over periods of many millions of years. Approximately 71% of the planet's surface is covered by sea water, the rest of the surface is occupied by continents and islands. Liquid water, essential for all known life forms, does not exist on the surface of any known planets or planetoids in the Solar System. The Earth's interior is quite active and consists of a thick, relatively solid layer called the mantle, which covers a liquid outer core (which is the source of the Earth's magnetic field) and an inner solid iron core.
GENERAL CHARACTERISTICS OF THE EARTH
STRUCTURE OF THE EARTH The Earth, like other terrestrial planets, has a layered internal structure. It consists of hard silicate shells (crust, extremely viscous mantle), and a metallic core. The outer part of the core is liquid (much less viscous than the mantle), and the inner part is solid. Geological layers of the Earth in depth from the surface: The internal heat of the planet is most likely provided by the radioactive decay of the isotopes potassium-40, uranium-238 and thorium-232. All three elements have a half-life of more than a billion years.] At the center of the planet, the temperature may rise to 7,000 K, and the pressure may reach 360 GPa (3.6 thousand atm). Part of the thermal energy of the core is transferred to the earth's crust through plumes. Plumes lead to the appearance of hot spots and traps.
TECTONIC PLATFORMS According to plate tectonic theory, the outer part of the Earth consists of two layers: the lithosphere, which includes the earth's crust, and the solidified upper part of the mantle. Below the Lithosphere is the asthenosphere, which makes up the inner part of the mantle. The asthenosphere behaves like a superheated and extremely viscous liquid. The lithosphere is divided into tectonic plates, and seems to float on the asthenosphere. The plates are rigid segments that move relative to each other. There are three types of their mutual movement: convergence, divergence, and strike-slip movements along transform faults. Earthquakes, volcanic activity, mountain building, and the formation of ocean basins can occur on faults between tectonic plates.
EARTH'S ROTATION The Earth takes an average of 23 hours 56 minutes and 4.091 seconds (sidereal day) to complete one rotation around the axis connecting the north and south poles. The planet's rotation rate from west to east is approximately 15 degrees per hour (1 degree per 4 minutes, 15′ per minute). This is equivalent to the apparent diameter of the Sun or Moon every two minutes. (The apparent sizes of the Sun and Moon are approximately the same.) The Earth's rotation is unstable, but on a large time scale it slows down. In one century, the Earth rotates 0s.0014 seconds slower than in the previous century. The Earth moves around the Sun in an elliptical orbit at a distance of about 150 million km with an average speed of 29.765 km/sec. The speed ranges from 30.27 km/sec (at perihelion) to 29.27 km/sec (at aphelion]. Moving in orbit, the Earth makes a complete revolution in 365.2564 average solar days (one sidereal year). From Earth, the movement of the Sun relative to the stars is about 1° per day in the easterly direction. The speed of the Earth's orbit is not constant: in July it begins to accelerate (after passing aphelion), and in January it begins to slow down again (after passing perihelion). The Sun and the entire solar system revolve around the center of the Milky Way galaxy in an almost circular orbit at a speed of about 220 km/s.In turn, the Solar system within the Milky Way moves at a speed of about 20 km/s towards a point (apex) located on the border of the constellations Lyra and Hercules, accelerating as the Universe expands. Carried away by the movement of the Sun, the Earth describes a helical line in space.
MOON The Moon (lat. Luna) is the only natural satellite of the Earth. It is the second brightest object in the earth's sky after the Sun and the fifth largest natural satellite of the planets in the solar system. It is also the first (and as of 2010, the only) extraterrestrial object of natural origin visited by humans. The average distance between the centers of the Earth and the Moon is 384,467 km. The apparent magnitude of the full Moon in the earth's sky is −12m.71. The illumination created by the full Moon near the Earth's surface in clear weather is 0.25 lux.
MOTION OF THE MOON As a first approximation, we can assume that the Moon moves in an elliptical orbit with an eccentricity of 0.0549 and a semimajor axis of 384,399 km. The actual motion of the Moon is quite complex; many factors must be taken into account when calculating it, for example, the oblateness of the Earth and the strong influence of the Sun, which attracts the Moon 2.2 times stronger than the Earth. More precisely, the movement of the Moon around the Earth can be represented as a combination of several movements: rotation around the Earth in an elliptical orbit with a period of 27.32 days; precession (plane rotation) of the lunar orbit with a period of 18.6 years (see also saros); rotation of the major axis of the lunar orbit (apse line) with a period of 8.8 years; periodic change in the inclination of the lunar orbit relative to the ecliptic from 4°59′ to 5°19′; periodic change in the size of the lunar orbit: perigee from 356.41 Mm to 369.96 Mm, apogee from 404.18 Mm to 406.74 Mm; the gradual removal of the Moon from the Earth (about 4 cm per year) so that its orbit is a slowly unwinding spiral. This is confirmed by measurements carried out over 25 years. The force that causes the Moon to move away from the Earth is the transfer of angular momentum from the Earth to the Moon through tidal interaction. The gravitational interaction between the Moon and the Earth is not constant; as the distance increases, the strength of the interaction decreases. This leads to the fact that with increasing distance the speed of the Moon's retreat decreases.
WATER ON THE MOON In July 2008, a group of American geologists from the Carnegie Institution and Brown University discovered in soil samples of the Moon traces of water that was released in large quantities from the bowels of the satellite in the early stages of its existence. Later, most of this water evaporated into space. Russian scientists, using the LEND instrument they created and installed on the LRO probe, have identified areas of the Moon that are most rich in hydrogen. Based on this data, NASA selected a site for the LCROSS probe to bombard the Moon. After the experiment, on November 13, 2009, NASA announced the discovery of water in the form of ice in the Cabeus crater near the south pole. According to data transmitted by the Mini-SAR radar installed on the Indian lunar probe Chandrayaan-1, at least 600 million tons of water were discovered in the north pole region, most of which is in the form of ice blocks resting at the bottom of lunar craters. In total, water was found in more than 40 craters, the diameter of which varies from 2 to 15 km. Now scientists no longer have any doubt that the ice found is water ice.
MARS Mars is the fourth most distant planet from the Sun and the seventh largest planet in the Solar System. This planet is named after Mars, the ancient Roman god of war, corresponding to the ancient Greek Ares. Mars is sometimes called the “Red Planet” because of the reddish hue of its surface given by iron(III) oxide. Mars is a terrestrial planet with a thin atmosphere. Features of the surface relief of Mars can be considered impact craters like those on the Moon and volcanoes, valleys, deserts and polar ice caps like those on Earth. The Martian extinct volcano Olympus Mons is the highest mountain in the solar system, and Valles Marineris is the largest canyon. Additionally, in June 2008, three papers published in Nature provided evidence for the largest known impact crater in the solar system in the northern hemisphere of Mars. Its length is 10,600 km and its width is 8,500 km, which is about four times larger than the largest impact crater previously also discovered on Mars, near its south pole. In addition to similar surface topography, Mars has a rotation period and seasonal cycles similar to Earth's, but its climate is much colder and drier than Earth's.
CHARACTERISTICS OF MARS
PHYSICAL CHARACTERISTICS OF MARS Mars is almost half the size of Earth - its equatorial radius is 3396.9 km (53.2% of Earth's). The surface area of Mars is approximately equal to the land area on Earth. The rather rapid rotation of the planet leads to noticeable polar compression - the polar radius of Mars is approximately 21 km less than the equatorial one. The planet's mass is 6.418×1023 kg (11% of the Earth's mass). The acceleration of gravity at the equator is 3.711 m/sec² (0.376 Earth); The first escape velocity is 3.6 km/sec and the second is 5.027 km/sec. Mars rotates around its axis, inclined to the orbital plane at an angle of 24°56′. The planet's rotation period is 24 hours 37 minutes 22.7 seconds. Thus, a Martian year consists of 668.6 Martian solar days (called sols). The tilt of Mars' rotation axis causes the seasons to change. In this case, the elongation of the orbit leads to large differences in their duration. Thus, the northern spring and summer, taken together, last 371 sols, that is, noticeably more than half of the Martian year. At the same time, they occur in a section of Mars’ orbit that is distant from the Sun. Therefore, on Mars, the northern summer is long and cool, and the southern summer is short and hot.
JUPITER Jupiter is the fifth planet from the Sun, and the largest in the Solar System. Jupiter is twice as massive as all the other planets in the solar system combined. Along with Saturn, Uranus and Neptune, Jupiter is classified as a gas giant. The planet has been known to people since ancient times and is reflected in the mythology and religious beliefs of many cultures. Jupiter is composed primarily of hydrogen and helium. Most likely, in the center of the planet there is a rocky core of heavier elements under high pressure. Due to its rapid rotation, Jupiter's shape is an oblate spheroid (it has a significant bulge around its equator). The planet's outer atmosphere is clearly divided into several elongated bands along latitudes, and this leads to storms and storms along their interacting boundaries. A notable result of this is the Great Red Spot, a giant storm that has been known since the 17th century. According to data from the Galileo lander, pressure and temperature increase rapidly as one goes deeper into the atmosphere. Jupiter has a powerful magnetosphere. Jupiter's satellite system consists of at least 63 moons, including 4 large moons, also called "Galilean" moons, which were discovered by Galileo Galilei in 1610. Jupiter's moon Ganymede has a diameter greater than that of Mercury. A global ocean has been discovered beneath the surface of Europa, and Io is known for having the most powerful volcanoes in the solar system. Jupiter has weak planetary rings.
CHARACTERISTICS OF JUPITER
PARAMETERS OF JUPITER Jupiter is the largest planet in the solar system. Its equatorial radius is 71.4 thousand km, which is 11.2 times the radius of the Earth. The Great Red Spot and the Little Red Spot in May 2008 in a photograph taken by the Hubble Telescope. The mass of Jupiter is more than 2 times the total mass of all other planets in the solar system, 318 times the mass of the Earth and only 1000 times less than the mass of the Sun. If Jupiter were about 60 times more massive, it could become a star. The density of Jupiter is approximately equal to the density of the Sun and is significantly inferior to the density of the Earth. The equatorial plane of the planet is close to the plane of its orbit, so there are no seasons on Jupiter. Jupiter rotates around its axis, and not like a rigid body: the angular velocity of rotation decreases from the equator to the poles. At the equator, a day lasts about 9 hours 50 minutes. Jupiter rotates faster than any other planet in the solar system. Due to the rapid rotation, the polar compression of Jupiter is very noticeable: the polar radius is 4.6 thousand km less than the equatorial radius (that is, 6.5%). All we can observe on Jupiter are the clouds of the upper atmosphere. The giant planet consists mainly of gas and does not have the solid surface we are accustomed to. Jupiter releases 2-3 times more energy than it receives from the Sun. This may be explained by the gradual compression of the planet, the sinking of helium and heavier elements, or the processes of radioactive decay in the bowels of the planet. Most of the currently known exoplanets are comparable in mass and size to Jupiter, so its mass (MJ) and radius (RJ) are widely used as convenient units of measurement to indicate their parameters.
GREAT RED SPOT The Great Red Spot (GRS) is an atmospheric feature on Jupiter, the most visible feature on the planet's disk, observed for almost 350 years. The BCP was discovered by Giovanni Cassini in 1665. The feature noted in Robert Hooke's 1664 notes can also be identified as a BCP. Before the Voyager mission, many astronomers believed that the spot was of a solid nature. The BKP is a giant hurricane-anticyclone, measuring 24-40 thousand km in length and 12-14 thousand km in width (significantly larger than the Earth). The size of the spot is constantly changing, the general tendency is to decrease; 100 years ago, the BKP was approximately 2 times larger and much brighter (see the results of observations by A. A. Belopolsky in the 1880s). The Great Red Spot on the planet Jupiter is the largest atmospheric vortex in the solar system. Its dimensions vary and it can reach up to 40,000 km in length and 14,000 km in width. Its length could accommodate 3 Earth-sized planets. This huge vortex has been raging for at least 340 years, since telescopes were powerful enough to view it from Earth, but it may have been around much longer. It rotates counterclockwise at a speed of about 435 km/h. The bright orange color of the spot is apparently due to the presence of sulfur and phosphorus in the atmosphere.
SATURN Saturn is the sixth planet from the Sun and the second largest planet in the Solar System after Jupiter. Saturn, as well as Jupiter, Uranus and Neptune, are classified as gas giants. Saturn is named after the Roman god Saturn, the counterpart of the Greek Kronos (Titan, father of Zeus) and the Babylonian Ninurta. Saturn's symbol is a sickle (Unicode: ♄). Saturn is mostly hydrogen, with some helium and traces of water, methane, ammonia and “rocks.” The inner region is a small core of rock and ice, covered with a thin layer of metallic hydrogen and a gaseous outer layer. The planet's outer atmosphere appears calm and serene, although it occasionally exhibits some long-lasting features. The wind speed on Saturn can reach 1800 km/h in places, which is significantly higher than, for example, on Jupiter. Saturn has a planetary magnetic field that is intermediate in power between the Earth's magnetic field and the powerful field of Jupiter. Saturn's magnetic field extends 1 million km in the direction of the Sun. The shock wave was detected by Voyager 1 at a distance of 26.2 Saturn radii from the planet itself, the magnetopause is located at a distance of 22.9 radii. Saturn has a prominent ring system made up primarily of ice particles and smaller amounts of rock and dust. There are 62 currently known satellites orbiting the planet. Titan is the largest of them, as well as the second largest satellite in the Solar System (after the satellite of Jupiter, Ganymede), which is larger than the planet Mercury and has the only dense atmosphere among the many satellites of the Solar System.
CHARACTERISTICS OF SATURN
RINGS Today we know that all four gaseous giants have rings, but Saturn has the most beautiful and noticeable ones. The rings are located at an angle of approximately 28° to the ecliptic plane. Therefore, from the Earth, depending on the relative position of the planets, they look different: they can be seen both in the form of rings and “edge-on”. As Huygens also assumed, the rings are not a solid solid body, but consist of billions of tiny particles located in circumplanetary orbit. There are three main rings and a fourth, thinner one. Together they reflect more light than the disk of Saturn itself. The three main rings are usually designated by the first letters of the Latin alphabet. Ring B is the central one, the widest and brightest, it is separated from the larger outer ring A by the Cassini gap, almost 4,000 km wide, which contains the thinnest, almost transparent rings. Inside the A ring there is a thin gap called the Encke separating strip. Ring C, located even closer to the planet than B, is almost transparent. Saturn's rings are very thin. With a diameter of about 250,000 km, their thickness does not reach even a kilometer (although there are also peculiar mountains on the surface of the rings[4]). Despite its impressive appearance, the amount of substance that makes up the rings is extremely small. If it were assembled into one monolith, its diameter would not exceed 100 km. The images obtained by the probes show that the rings are actually formed from thousands of rings alternating with slits; the picture resembles the tracks of gramophone records. The particles that make up the rings are mostly several centimeters in size, but occasionally bodies of several meters are found. Very rarely - up to 1-2 km. The particles appear to be composed almost entirely of ice or rocky material covered with ice. There is complete consistency between the planet's rings and satellites. Indeed, some of them, the so-called “shepherd moons,” play a role in keeping the rings in place. Mimas, for example, is “responsible” for the absence of substance in
How to work with a presentation?
The presentation “Planets of the Solar System” is designed for babies from 3 months and contains photos and videos of planets. Here is the movement of celestial bodies around the Sun, their sizes; it tells how many planets there are in the Solar System, which is the hottest and coldest, the largest and smallest, what dwarf planets exist in the Solar System and much more. To ensure your child understands the material well, watch it 2-3 times a day, 5 days a week.
After this, you can print and start playing with the Planet cards. Initially, start with a small amount, take 2 cards and ask the child to show where this or that Planet is. After your child has mastered this information, try introducing more cards.
The Umnitsa company has very good Planet cards, which are called Planets of the Solar System for children. In addition, here you can download cards of the Planets of the Solar System, as well as many games for children from 1 to 8 years old to develop attentiveness, logic, memory, accuracy, creative tasks and much more - space games for free.
The presentation is also suitable for primary and secondary school children as educational material. The presentation can be put on in a natural history lesson while learning about the structure of the cosmos and then carefully study the photographs offered on it, freezing the frames.
In a children's aesthetic center, such information will also not be superfluous. It develops erudition and helps expand the boundaries of children's thinking.
Many parents and educators are afraid to offer their children global topics to study, believing that this is material for study at an older age. In vain. Until the age of 7, a child learns material at maximum speed. Then brain activity begins to slow down, and after 7 years it is much more difficult to study complex material.
There is no need to be afraid that such astronomy lessons will bore children or seem uninteresting. Making them fun is in our hands. The proposed presentation is designed to solve this problem.
Show it to your children as much as they are interested. As soon as you notice your child looking bored, stop and give him a chance to distract himself. The next day, show me another piece. Subsequently, the baby will get carried away and will ask him to give him a presentation. And along with interest will come new knowledge.
External system - for children
This includes the major planets: Jupiter, Saturn, Uranus and Neptune. These are huge worlds with thick gas layers. It is important to explain to the youngest children that almost all of their mass is represented by hydrogen and helium, which is why they resemble the Sun in composition. There is no solid surface beneath these layers, although there may be a rocky core. Around them there are rings of rocks and ice (the most famous are those of Saturn). Of course, Jupiter is the largest planet in the solar system.
Comets are often called dirty snowballs because they are made of ice and rock. When their orbit is directed toward the Sun, some of the ice in the central core turns into gas, which is sprayed into space in the form of a long tail. There are comets with a short periodicity (200 years) that emerge from the Kuiper belt. But with a long periodicity - objects of the Oort cloud.
Jupiter
Saturn
Uranus
Neptune
Pluto
