Terrestrial planets presentation. Presentation on the topic "Terrestrial planets". Mars is the fourth planet from the sun

Slide 1

Terrestrial planets

Performed by student HB-5 Shiryaeva Sofia

Slide 2

According to their own physical characteristics The planets of the solar system are divided into terrestrial planets and giant planets

The terrestrial planets include: Mercury, Venus, Earth and Mars

Slide 3

general characteristics dynamic properties of terrestrial planets

The similarity of the terrestrial planets does not exclude significant differences in mass, size and other characteristics

GENERAL CHARACTERISTICS OF THE TERRESTRIAL PLANETS

Slide 4

Mercury

Slide 5

Mercury is the “second moon”! When the Mariner 10 spacecraft transmitted the first close-up images of Mercury, astronomers threw up their hands: there was a second Moon in front of them!

Mercury is very similar to the Moon. In the history of both celestial bodies There was a period when lava flowed to the surface in streams.

Slide 6

Mercury is the planet closest to the Sun out of the 9 main planets of the solar system, and, in accordance with Kepler's 3rd law, has the shortest period of revolution around the Sun (88 Earth days). And the highest average orbital speed (48 km/s).

Mercury is located close to the Sun. Mercury's maximum elongation is only 28 degrees, making it very difficult to observe. Mercury has no satellites.

Slide 7

The surface of Mercury in photographs taken at close range is replete with craters (US MESSENGER spacecraft)

This reticulated topography is the territory of the Caloris Basin. Pantheon Fossae or the Depression of the Pantheon is its center. The relief of the basin became this way due to the fall of a giant meteorite. The pool is the result of the outflow of lava from the bowels of the planet after a collision.

The shadows in the photo give the craters an additional resemblance to the cartoon character. The diameter of Mickey's "head" is 105 kilometers.

Slide 9

Data on the atmosphere of Mercury indicates only its strong rarefaction. Because the critical speed is too low and the temperature too high for Mercury to retain an atmosphere. However, in 1985, with the help spectral analysis an extremely thin layer of sodium atmosphere was discovered. Obviously, atoms of this metal are released from the surface when it is bombarded by streams of particles flying from the Sun.

Mercury is located very close to the Sun and captures sunny wind by its gravity. A helium atom captured by Mercury remains in the atmosphere for an average of 200 days.

Slide 10

Mercury has a weak magnetic field, which has been discovered spacecraft Mariner 10.

The high density and presence of a magnetic field indicate that Mercury must have a dense metallic core. The core accounts for 80% of Mercury's mass.

The radius of the core is 1800 km (75% of the radius of the planet).

Slide 11

Surface temperatures in Mercury's polar regions, which are never illuminated by the Sun, can hover around -210°C. There may be water ice present. The maximum surface temperature of Mercury recorded by sensors is + 410 °C. Temperature differences on the day side due to the change of seasons caused by the elongation of the orbit reach 100 °C.

Slide 12

Slide 13

Venus is the second terrestrial planet after Mercury in terms of distance from the Sun (108 million km). Its orbit has the shape of an almost perfect circle. Venus orbits the Sun in 224.7 Earth days at a speed of 35 km/sec.

All planets (except Uranus) rotate around their axis counterclockwise (when viewed from the North Pole), while Venus rotates in the opposite direction - clockwise.

The rotation axis of Venus is almost perpendicular to the orbital plane, so there are no seasons - one day is similar to another, has the same duration and the same weather.

Slide 14

The weather uniformity is further enhanced by the specificity of the Venusian atmosphere - its strong greenhouse effect.

The existence of the Venusian atmosphere was first discovered in 1976 by M.V. Lomonosov during observations of its passage across the solar disk.

Studies of the reflected spectrum of Venus using telescopes have shown that the atmosphere is very different from the atmosphere of Earth.

Slide 15

The main components of Venus's clouds are droplets of sulfuric acid and solid sulfur particles. Using probes, it was discovered that below the clouds the atmosphere contains approximately 0.1 to 0.4% percent water vapor and 60 parts per million free oxygen. The presence of these components indicates that Venus may once have had water, but the planet has now lost it.

Image in ultraviolet rays, obtained from the Pioneer-Venus interplanetary station, demonstrates the planet’s atmosphere, densely filled with clouds, lighter in the polar regions (at the top and bottom of the image)

Slide 16

Near the surface of Venus, it was possible to measure wind speeds of approximately 13 km/h. They are relatively weak, however they can move small particles of sand or the like. At higher altitudes there are stronger winds. At an altitude of 45 km, wind movements at a speed of 175 km/h were observed, and strong vertical air movements were also detected. Probes conducting research on Venus brought data that was deciphered as evidence of the presence of lightning.

The sky on Venus is a bright yellow-green hue.

Slide 17

The surface of Venus has many features similar to those of Earth. Most of the planet is dominated by relatively low-lying planes characterized by excessive volcanic structures, but there are also large highland areas with mountain ranges, volcanoes, and fissure systems. The largest highland area, called Aphrodite's Land, is in the equatorial region of Venus. Its size is approximately equal to the size of Africa.

Slide 18

According to the most plausible hypothesis, the Venusian core has not yet begun to solidify and therefore convective jets are not born there, swirling due to the rotation of the planet and generating a magnetic field. Otherwise, such a field should still have arisen

Whether Venus has a solid or liquid core is not yet known for sure.

Slide 19

In relation to Venus, we can say that the climate and weather on this planet are one and the same. On Venus, these conditions are practically unchanged throughout the day and year. With an almost perpendicular position of the rotation axis of Venus to the orbital plane (inclination 3), fluctuations in the values ​​of meteorological elements remain almost unchanged during the day (their duration is 234 Earth days). Temperature fluctuations at the surface do not exceed 5-15 C.

Slide 20

Slide 21

The earth has one unique feature - it has life. However, this is not noticeable when looking at the Earth from space. Clouds floating in the atmosphere are clearly visible. Continents can be seen through the gaps in them. Most of the Earth is covered by oceans.

The appearance of life, living matter - the biosphere - on our planet was a consequence of its evolution. In turn, the biosphere had a significant impact on the entire further course of natural processes. So, if there was no life on Earth, chemical composition its atmosphere would be completely different.

Slide 22

It’s not easy to “look” into the depths of the Earth. Even the deepest wells on land barely penetrate the 10-kilometer mark, and under water they manage to penetrate the basalt foundation no more than 1.5 km after passing through the sedimentary cover. Seismic waves come to the rescue.

According to vibration records earth's surface– seismograms – it was established that the interior of the Earth consists of three main parts: the crust, the shell (mantle) and the core.

Slide 23

Opened in 1905 changes in the Earth's magnetic field in space and intensity led to the conclusion that it originates in the depths of the planet. The most likely source of such a field is a liquid iron core. There should be current loops in it, roughly reminiscent of turns of wire in an electromagnet, which generate various components of the geomagnetic field.

In the 30s seismologists have established that the Earth also has an inner, solid core. Modern meaning the depth of the boundary between the inner and outer cores is approximately 5150 km.

Slide 24

Back in 1912, German researcher Alfred Wegener put forward the hypothesis of continental drift.

The first magnetic maps of the Pacific ocean floor off the coast North America, in the area of ​​​​the Juan de Fuca ridge, showed the presence of mirror symmetry. An even more symmetrical pattern is found on both sides of the central ridge in the Atlantic Ocean.

Using the concept of continental drift, known today as "new global tectonics", it is possible to reconstruct mutual arrangement continents in the distant past. It turns out that 200 million years ago it formed a single continent.

In the 50s, when studies of the ocean floor were widely carried out, the hypothesis of large horizontal movements in the lithosphere received new confirmation. A significant role in this was played by the study of the magnetic properties of the rocks that make up the ocean floor.

Slide 25

It is known that our planet was formed about 4.6 billion years ago. During the formation of the Earth from particles of the protoplanetary cloud, its mass gradually increased. The gravitational force increased, and consequently, the speed of particles falling on the planet. Kinetic energy particles turned into heat, and the Earth warmed up more and more. During impacts, craters appeared on it, and the substance ejected from them could no longer overcome gravity and fell back.

The larger the falling bodies, the more they heated the Earth. The impact energy was released not on the surface, but at a depth equal to approximately two diameters of the embedded body. And since the bulk at this stage was supplied to the planet by bodies several hundred kilometers in size, the energy was released in a layer about 1000 km thick. It did not have time to radiate into space, remaining in the bowels of the Earth. As a result, the temperature at depths of 100–1000 km could approach the melting point. Additional boost temperature probably caused the decay of short-lived radioactive isotopes.

Slide 26

Currently, the Earth has an atmosphere with a mass of approximately 5.15 * 10 kg, i.e. less than a millionth of the planet's mass. Near the surface it contains 78.08% nitrogen, 20.05% oxygen, 0.94% inert gases, 0.03% carbon dioxide and in small quantities other gases.

Water covers more than 70% of the surface of the globe, and the average depth of the World Ocean is about 4 km. The mass of the hydrosphere is approximately 1.46 * 10 kg. This is 275 times the mass of the atmosphere, but only 1/4000 of the mass of the entire Earth. The hydrosphere is 94% made up of the waters of the World Ocean, in which salts are dissolved (3.5% on average), as well as a number of gases. Upper layer The ocean contains 140 trillion tons of carbon dioxide and 8 trillion tons of dissolved oxygen. tons

Slide 27

The Moon is the only natural satellite of the Earth. The second brightest object in the earth's sky after the Sun and the fifth largest natural satellite of a planet in the solar system. The average distance between the centers of the Earth and the Moon is 384,467 km (0.002 57 AU).

Visible magnitude full moon in the earth's sky −12.71m. Illumination created full moon near the surface of the Earth in clear weather, it is 0.25 - 1 lux.

The Moon is the only astronomical object outside the Earth that humans have visited.

Slide 29

Slide 30

The orbit of Mars lies approximately one and a half times further than the earth. It is somewhat elliptical, so the planet's distance from the Sun varies from a minimum, at perihelion, 206.7 million km to a maximum, at aphelion, 249.2 million km.

Because Mars is further from the Sun than Earth; Mars takes longer to complete one revolution around the Sun. A year on Mars lasts 687 Earth days. The speed of Mars is approximately 24 km/s, and the planet rotates in the same direction as the Earth - counterclockwise (when viewed from the side north pole planets). A Martian day lasts 24 hours, 37 minutes, 23 seconds, which is very close to the length of an Earth day.

The tilt of the planet's axis is approximately 25 degrees, as a result of which seasonal changes on Mars occur similar to those on Earth. Because of Mars' elliptical orbit, it is summer in the southern hemisphere when the planet is closest to the Sun, and winter in the northern hemisphere.

Slide 31

The main components of the Martian atmosphere are carbon dioxide (95.3%), nitrogen (2.7%), and argon (1.6%). Small amounts of oxygen, carbon monoxide, water vapor, and other substances make up the rest. The average surface pressure of the atmosphere is less than one hundredth the average surface pressure of the Earth's atmosphere, and it varies with time of year and altitude. The Martian atmosphere is subject to diurnal and seasonal sudden changes temperature.

Gravity on Mars is almost 3 times less than on Earth. That is, while walking on this planet, you could jump three times higher than on Earth.

Spacecraft that have visited Mars have confirmed the presence of water in the form of large reserves below the surface and in the form of ice on the surface.

Slide 32

The color of the Martian surface ranges from orange to brown-black. The darker substances are weathered basalt rock, and the lighter ones are iron oxides.

Photographs of the Martian surface obtained American devices, who landed on the surface of Mars as part of the Viking mission, confirm the presence of layers that are carried by winds, and also show rocks and boulders scattered on the surface.

Mars is a huge red desert. The deep canyons of Mars are carved by winds. Volcanoes rise on the surface and impact craters stretch out.

Slide 33

Currently the structure gravitational field Mars has been studied in detail. It indicates a slight deviation from the uniform distribution of density on the planet. The core can have a radius of up to half the radius of the planet. Apparently, it consists of pure iron or an alloy of Fe-FeS (iron-iron sulfide) and possibly hydrogen dissolved in them. Apparently, the core of Mars is partially or completely liquid.

Mars should have a thick crust 70-100 km thick. Between the core and the crust there is a silicate mantle enriched in iron. Red iron oxides present in surface rocks determine the color of the planet. Now Mars continues to cool. Seismic activity planets are weak.

Slide 35

Olympus Mons on Mars is the highest mountain in solar system. Its height is 27 km. This is a volcano. The relatively young lava on its slopes indicates its possible activity.

Valles Marineris is the longest and deepest canyon in the solar system. It stretches along the equator for 4000 km, and its depth reaches 7 kilometers. One of the main versions of the formation of a canyon resembling a scar is a grandiose catastrophe associated with the collision of Mars with a huge cosmic body.

Canyon on Mars - trace of a great cosmic catastrophe on the planet

Slide 36

Deimos (Greek Δείμος “horror”) is one of two satellites of Mars. It was discovered by American astronomer Asaph Hall in 1877

The diameter of Deimos is about 13 km, it orbits at an average distance of 6.96 planet radii (approximately 23,500 km), with an orbital period of 30 hours 17 minutes 55 s.

Deimos, like the Moon, has an angular velocity of motion in orbit equal to angular velocity own rotation, therefore it is always turned to Mars with the same side.

Phobos (ancient Greek φόβος “fear”) is one of two satellites of Mars. It was discovered by American astronomer Asaph Hall in 1877.

The dimensions of Phobos are 27 × 22 × 18 km. Phobos orbits at an average distance of 2.77 Mars radii from the planet's center (9400 km). It makes one revolution in 7 hours 39 minutes 14 seconds, which is about three times faster than the rotation of Mars around its own axis. As a result, in the Martian sky, Phobos rises in the west and sets in the east.

Phobos Deimos

Slide 37

AXIS OF ROTATION OF THE TERRESTRIAL PLANETS

Slide 38

THANK YOU FOR YOUR ATTENTION!

Terrestrial planets
Vikonali 11th grade student
Giniyatullin Vladislav
that
Locust Karina

According to their physical characteristics, the planets of the solar system are divided into terrestrial planets and giant planets
The terrestrial planets include: Mercury, Venus, Earth and Mars

General characteristics of the dynamic properties of terrestrial planets
The similarity of the terrestrial planets does not exclude significant
differences in weight, size and other characteristics
GENERAL CHARACTERISTICS OF THE TERRESTRIAL PLANETS

Mercury

Mercury is the “second moon”!
When the Mariner 10 spacecraft transmitted the first
Close-up shots of Mercury, astronomers
They clasped their hands: in front of them was the second Moon!
Mercury is very similar to the Moon. In the history of both celestial bodies
There was a period when lava flowed to the surface in streams.

Mercury is the planet closest to the Sun out of the 9 main planets of the solar system, and, in accordance with Kepler's 3rd law, has the shortest period of revolution around the Sun (88 Earth days). And the highest average orbital speed (48 km/s).
Mercury is located close to the Sun. Mercury's maximum elongation is only 28 degrees, making it very difficult to observe.
Mercury has no satellites.

The surface of Mercury in photographs taken from close up
distances, replete with craters (American spacecraft MESSENGER)
This reticulated topography is the territory of the Caloris Basin. Pantheon Fossae or Depression of the Pantheon is its center. The relief of the basin became this way due to the fall of a giant meteorite. The pool is the result of the outflow
lava from the bowels of the planet after a collision.
The shadows in the photo give the craters an additional resemblance to the cartoon character. The diameter of Mickey's "head" is 105 kilometers.

Data on the atmosphere of Mercury indicates only its strong rarefaction. Because the critical speed is too low and the temperature too high for Mercury to retain an atmosphere. However, in 1985, using spectral analysis, an extremely thin layer of sodium atmosphere was discovered. Obviously, atoms of this metal are released from the surface when it is bombarded by streams of particles flying from the Sun.
Mercury is located very close to the Sun and captures the solar wind with its gravity.
A helium atom captured by Mercury remains in the atmosphere for an average of 200 days.

Mercury has a weak magnetic field,
which was discovered by the Mariner 10 spacecraft.
High density and availability
magnetic field show that Mercury should have
dense metal core.
The core accounts for
80% of Mercury's mass.
The radius of the core is 1800 km (75% of the radius of the planet).

Surface temperature in
The polar regions of Mercury, which the Sun never illuminates, can remain around -210 °C.
There may be water ice present.
Maximum temperature
surface of Mercury,
registered by sensors, + 410 °C.
Temperature changes
on the day side
due to the change of seasons,
caused by the elongation of the orbit,
reach 100 °C.

Venus is the second terrestrial planet after Mercury in terms of distance from the Sun (108 million km). Its orbit has the shape of an almost perfect circle. Venus orbits the Sun in 224.7 Earth days at a speed of 35 km/sec.
All planets (except Uranus) rotate around their axis counterclockwise (when viewed from the North Pole), while Venus rotates in the opposite direction - clockwise.
The rotation axis of Venus is almost perpendicular to the orbital plane, so there are no seasons - one day is similar to another, has the same duration and the same weather.

The weather uniformity is further enhanced by the specificity of the Venusian atmosphere - its strong greenhouse effect.
The existence of the Venusian atmosphere was first discovered in 1976 by M.V. Lomonosov during observations of its passage across the solar disk.
Studies of the reflected spectrum of Venus using telescopes have shown that the atmosphere is very different from the atmosphere of Earth.

The main components of Venus's clouds are droplets of sulfuric acid and solid sulfur particles. Using probes, it was discovered that below the clouds the atmosphere contains approximately 0.1 to 0.4% percent water vapor and 60 parts per million free oxygen. The presence of these components indicates that Venus may once have had water, but the planet has now lost it.
An ultraviolet image taken from the Pioneer Venus interplanetary station shows the planet's atmosphere densely filled with clouds, lighter in the polar regions (top and bottom of the image).

Near the surface of Venus, it was possible to measure wind speeds of approximately 13 km/h. They are relatively weak, however they can move small particles of sand or the like. At higher altitudes there are stronger winds. At an altitude of 45 km, wind movements at a speed of 175 km/h were observed, and strong vertical air movements were also detected. Probes conducting research on Venus brought data that was deciphered as evidence of the presence of lightning.
The sky on Venus is a bright yellow-green hue.

The surface of Venus has many features similar to those of Earth. Most of the planet is dominated by relatively low-lying planes characterized by excessive volcanic structures, but there are also large highland areas with mountain ranges, volcanoes, and fissure systems. The largest highland area, called Aphrodite's Land, is in the equatorial region of Venus. Its size is approximately equal to the size of Africa.

According to the most plausible hypothesis, the Venusian core has not yet begun to solidify and therefore convective jets are not born there, swirling due to the rotation of the planet and generating a magnetic field. Otherwise, such a field should still have arisen
Whether Venus has a solid or liquid core is not yet known for sure.

In relation to Venus, we can say that the climate and weather on this planet are one and the same. On Venus, these conditions are practically unchanged throughout the day and year. With an almost perpendicular position of the rotation axis of Venus to the orbital plane (inclination 3), fluctuations in the values ​​of meteorological elements remain almost unchanged during the day (their duration is 234 Earth days). Temperature fluctuations at the surface do not exceed 5-15 C.

The earth has one unique feature - it has life. However, this is not noticeable when looking at the Earth from space. Clouds floating in the atmosphere are clearly visible. Continents can be seen through the gaps in them.
Most of the Earth is covered by oceans.
The appearance of life, living matter - the biosphere - on our planet was a consequence of its evolution. In turn, the biosphere had a significant impact on the entire further course of natural processes. So, if there were no life on Earth, the chemical composition of its atmosphere would be completely different.

It’s not easy to “look” into the depths of the Earth. Even the deepest wells on land barely penetrate the 10-kilometer mark, and under water they manage to penetrate the basalt foundation no more than 1.5 km after passing through the sedimentary cover. Seismic waves come to the rescue.
Based on records of vibrations of the earth's surface - seismograms - it was established that the interior of the Earth consists of three main parts: the crust, the shell (mantle) and the core.

Opened in 1905 changes in the Earth's magnetic field in space and intensity led to the conclusion that it originates in the depths of the planet. The most likely source of such a field is a liquid iron core. There should be current loops in it, roughly reminiscent of turns of wire in an electromagnet, which generate various components of the geomagnetic field.
In the 30s seismologists have established that the Earth also has an inner, solid core. The current value of the depth of the boundary between the inner and outer cores is approximately 5150 km.

Back in 1912, German researcher Alfred Wegener put forward the hypothesis of continental drift.
The first magnetic maps of the Pacific floor off the coast of North America, in the area of ​​the Juan de Fuca Ridge, showed the presence of mirror symmetry. An even more symmetrical pattern is found on both sides of the central ridge in the Atlantic Ocean.
Using the concept of continental drift, known today as “new global tectonics,” it is possible to reconstruct the relative positions of continents in the distant past. It turns out that 200 million years ago it formed a single continent.
In the 50s, when studies of the ocean floor were widely carried out, the hypothesis of large horizontal movements in the lithosphere received new confirmation. A significant role in this was played by the study of the magnetic properties of the rocks that make up the ocean floor.

It is known that our planet was formed about 4.6 billion years ago. During the formation of the Earth from particles of the protoplanetary cloud, its mass gradually increased. The gravitational force increased, and consequently, the speed of particles falling on the planet. The kinetic energy of the particles turned into heat, and the Earth warmed up more and more. During impacts, craters appeared on it, and the substance ejected from them could no longer overcome gravity and fell back.
The larger the falling bodies, the more they heated the Earth. The impact energy was released not on the surface, but at a depth equal to approximately two diameters of the embedded body. And since the bulk at this stage was supplied to the planet by bodies several hundred kilometers in size, the energy was released in a layer about 1000 km thick. It did not have time to radiate into space, remaining in the bowels of the Earth. As a result, the temperature at depths of 100–1000 km could approach the melting point. The additional increase in temperature was probably caused by the decay of short-lived radioactive isotopes.

Currently, the Earth has an atmosphere with a mass of approximately 5.15 * 10 kg, i.e. less than a millionth of the planet's mass. Near the surface it contains 78.08% nitrogen, 20.05% oxygen, 0.94% inert gases, 0.03% carbon dioxide and in small quantities other gases.
Water covers more than 70% of the surface of the globe, and the average depth of the World Ocean is about 4 km. The mass of the hydrosphere is approximately 1.46 * 10 kg. This is 275 times the mass of the atmosphere, but only 1/4000 of the mass of the entire Earth. 94% of the hydrosphere is made up of the waters of the World Ocean, in which salts are dissolved (3.5% on average), as well as a number of gases. The top layer of the ocean contains 140 trillion tons of carbon dioxide and 8 trillion tons of dissolved oxygen. tons

The Moon is the only natural satellite of the Earth. The second brightest object in the earth's sky after the Sun and the fifth largest natural satellite of a planet in the solar system. The average distance between the centers of the Earth and the Moon is 384,467 km (0.002 57 AU).
The apparent magnitude of the full Moon in the earth's sky is −12.71m. The illumination created by the full Moon near the Earth's surface in clear weather is 0.25 - 1 lux.
The Moon is the only astronomical object outside the Earth that humans have visited.

The orbit of Mars lies approximately one and a half times further than the earth. It is somewhat elliptical, so the planet's distance from the Sun varies from a minimum, at perihelion, 206.7 million km to a maximum, at aphelion, 249.2 million km.
Because Mars is further from the Sun than Earth; Mars takes longer to complete one revolution around the Sun. A year on Mars lasts 687 Earth days. The speed of movement of Mars is approximately 24 km/s, and the planet rotates in the same direction as the Earth - counterclockwise (when viewed from the north pole of the planet). A Martian day lasts 24 hours, 37 minutes, 23 seconds, which is very close to the length of the earth's day.
The tilt of the planet's axis is approximately 25 degrees, as a result of which seasonal changes on Mars occur similar to those on Earth. Because of Mars' elliptical orbit, it is summer in the southern hemisphere when the planet is closest to the Sun, and winter in the northern hemisphere.

Kreneva Evgenia

The work describes the planets belonging to the Terrestrial group. The conditions on these planets are considered, their common features, as well as the characteristics of each planet.

Download:

Preview:

To use presentation previews, create a Google account and log in to it: https://accounts.google.com

Slide captions:

TERRESTRIAL PLANETS Presentation on astronomy Prepared by 11th grade student Kreneva Evgenia GBOU Secondary School No. 8, Moscow

SOLAR SYSTEM

Terrestrial Planets These are the four planets of the solar system: Mercury, Venus, Earth and Mars. They are also called inner planets, in contrast to the outer planets - giant planets.

Terrestrial planets have a high density and consist mainly of silicates and metals, as well as oxygen, silicon, iron, magnesium, aluminum and others heavy elements. Largest planet terrestrial group - Earth, but it is more than 14 times less massive than the least massive gas planet- Uranus. All terrestrial planets have the following structure: - in the center, a core made of iron with an admixture of nickel, - a mantle, consisting of silicates, - a crust, formed as a result of partial melting of the mantle and also consisting of silicate rocks, but enriched in incompatible elements. Of the terrestrial planets, Mercury does not have a crust, which is explained by its destruction as a result of meteorite bombardment.

MERCURY Is closest to the sun. The existence of this planet was mentioned in ancient Sumerian writings, which date back to the third millennium BC. This planet got its name from the Roman pantheon, Mercury, the patron saint of merchants, who also had his Greek counterpart, Hermes. Mercury completely circles the sun in eighty-eight Earth days. It travels around its axis in less than sixty days, which by Mercury standards is two-thirds of a year. The temperature on the surface of Mercury can vary greatly - from + 430 degrees on the sun side to + 180 degrees on the shadow side. In our solar system, these differences are the strongest.

MERCURY An unusual phenomenon can be observed on Mercury, which is called the Joshua effect. When the sun on Mercury reaches a certain point, it stops and begins to move towards reverse side, and not like on Earth - it must go around the planet in a full circle. Mercury is the smallest planet of the Earth group. It is smaller in size than even the largest satellites of the planets Jupiter and Saturn. The surface of Mercury is similar to the surface of the Moon - all strewn with craters. The only difference with the lunar surface is that Mercury has numerous oblique, jagged slopes that can extend for many hundreds of kilometers. These slopes were formed as a result of compression as the planet cooled.

MERCURY One of the most popular and visible parts of the planet is the so-called Heat Plain. This is a crater that gets its name due to its close location to the "hot longitudes". The crater has a diameter of one thousand three hundred kilometers. Most likely, the celestial body that made this crater in ancient times had a diameter of at least one hundred kilometers. Thanks to gravity, Mercury also captures particles of the solar wind, which in turn create a rather thin atmosphere around Mercury. Moreover, they are replaced every two hundred days. In addition, this planet is the fastest planet in our system. The average speed of its rotation around the sun is about forty-seven and a half kilometers per second, which is twice as fast as the Earth.

VENUS The atmosphere of Venus is quite aggressive, because relative to Earth it has a very high temperature and there are poisonous clouds in the sky. The atmosphere of Venus consists mainly of carbon dioxide. If you find yourself in the atmosphere of this planet, you will experience a pressure of about eighty-five kg per 1 square centimeter. In the Earth's atmosphere the pressure will be eighty-five times less. If you throw a coin in the atmosphere of Venus, it will fall as if in a layer of water. Thus, walking on the surface of this planet is just as difficult as walking on the bottom of the ocean. And if, God forbid, the wind rises on Venus, it will carry you like a sea wave carries a sliver.

VENUS The atmosphere of this planet is 96% carbon dioxide. This is precisely why it is created Greenhouse effect. The planet's surface is heated by the sun, and the resulting heat cannot be dissipated into space because it is reflected by a layer of carbon dioxide. That's why the temperature of this planet is about four hundred and eighty degrees, like an oven.

VENUS The surface of Venus is dotted with thousands of volcanoes. Science fiction writers described Venus as similar to Earth. It was believed that Venus was shrouded in clouds. This means that the surface of this planet should be dotted with swamps. This means that it probably has a very rainy climate, which leads to a lot of cloudiness and a lot of humidity. In reality, everything is completely different - in the early seventies, the union sent spaceships to the surface of Venus, which clarified the situation. It turned out that the surface of this planet is made up of continuous rocky deserts, where there is absolutely no water. Of course, at such a high temperature there could never be any water.

EARTH The Earth ranks fifth in size and mass among major planets, but of the terrestrial planets, it is the largest. Its most important difference from other planets in the solar system is the existence of life on it, which reached its highest, intelligent form with the advent of man. According to modern cosmogonic concepts, the Earth was formed ~4.5 billion years ago by gravitational condensation from gas and dust matter scattered in the circumsolar space, containing all the chemical elements known in nature.

EARTH The formation of the Earth was accompanied by differentiation of matter, which was facilitated by the gradual heating of the earth's interior, mainly due to the heat released during decay radioactive elements(uranium, thorium, potassium, etc.). The result of this differentiation was the division of the Earth into concentrically located layers - geospheres, differing in chemical composition, state of aggregation And physical properties. The Earth's core formed in the center, surrounded by a mantle. From the lightest and most fusible components of the substance released from the mantle during melting processes, the earth's crust located above the mantle arose. The collection of these internal geospheres, bounded by the solid earth's surface, is sometimes called the "solid" Earth.

EARTH “Solid” Earth contains almost the entire mass of the planet. Beyond its boundaries are the external geospheres - water (hydrosphere) and air (atmosphere), which were formed from vapors and gases released from the bowels of the Earth during degassing of the mantle. Differentiation of matter in the Earth's mantle and replenishment with differentiation products earth's crust, water and air envelopes occurred throughout geological history and continue to this day.

MARS This planet is named after the famous god of War in Rome, because the color of this planet is very reminiscent of the color of blood. This planet is also called the “red planet”. It is believed that this color of the planet is associated with iron oxide, which is present in the atmosphere of Mars. Mars is the seventh largest planet in the solar system. It is considered to be the home of the Valles Marineris - a canyon that is much longer and deeper than the famous Grand Canyon in the USA. By the way, there are quite a few mountains on Mars, and the height of these mountains is sometimes much higher than our Everest. Here, by the way, there is also Olympus - the highest and most famous mountain in the entire solar system.

MARS Mars has the largest volcanoes in the solar system. But the atmosphere of this planet is one hundred times less dense than Earth’s. But this is enough to maintain the weather system on the planet - that means wind and clouds. Average temperature Mars boasts a temperature of minus sixty degrees. A year on Mars = 687 Earth days. But a day on Mars is as close as possible to a day on Earth - it is 24 hours, 39 minutes. and 35 sec. Mars has a very thick crust - about fifty kilometers in cross section. Mars also has two moons - Deimos and Phobos.

Thank you for your attention!

Slide 2

According to their physical characteristics, the planets of the solar system are divided into terrestrial planets and giant planets

The terrestrial planets include: Mercury, Venus, Earth and Mars

Slide 3

General characteristics of the terrestrial planets

General characteristics of the dynamic properties of terrestrial planets

The similarity of the terrestrial planets does not exclude significant differences in mass, size and other characteristics

Slide 4

Mercury