Presentation on the topic "Mercury". Mercury - planet of the solar system

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Solar system. Planets terrestrial group Mercury Venus Earth Moon Mars

Mercury

Mercury Basic data: Name - Roman god of trade Distance from the Sun - 58 million km m Diameter - 4.8 km Density - 5.4 g/cm 2 Rotation period (1 day) - 59 Earth days Period of revolution around the Sun (1 year ) – 88 Earth days Orbit – ellipse Speed ​​– 47.3 km/s No satellites

Mercury Atmosphere and structure Temperature from -210 to +570 No change of seasons

Features and relief of Mercury

Mercury The earliest known recording of Mercury in the tables of Mul Apin (a collection of Babylonian astrological tables) was made by Assyrian astronomers around the 14th century BC. The Sumerian name UDU.IDIM.GU\U 4 .UD (“jumping planet”) is the god Ninurt, and in later records it is called “Nabu” in honor of the god of wisdom and scribal art. Titles B Ancient Greece– Hermes Ancient Rome– Mercury (Claudius Ptolemy) B Ancient China- Chen-hsing, (Morning Star) In modern Chinese, Korean, Japanese and Vietnamese cultures - “Water Star” In Indian mythology - Budha Model of the movement of Mercury proposed by Ibn al-Shatir History

First telescopic observation by Galileo Galilei early XVII century. Although he observed the phases of Venus, his telescope was not powerful enough to observe the phases of Mercury. In 1631, Pierre Gassendi made the first telescopic observation of the passage of a planet across the solar disk. The moment of passage was previously calculated by Johannes Kepler. In 1639, Giovanni Zupi discovered with a telescope that the orbital phases of Mercury were similar to those of the Moon and Venus. Observations have definitively demonstrated that Mercury orbits the Sun. History of Galileo Galilei Pierre Gassendi Mercury

Research of the US automatic interplanetary probe Mariner -10 was launched on November 3, 1973 and flew up to Mercury on March 29, 1974. Images of Mercury were transmitted by Mariner-10 during three flights with an interval of six months March 1974 September 1974 March 1975 Result: 45% of the planet's surface was explored Mercury

automatic interplanetary apparatus "MESSENGER" Start August 2004 In orbit January 2008 Result - 1231 images, including previously unobserved areas. Mercury research

On January 18, 2008, a ceremony was held in Germany to sign a contract for the production of the BepiColombo spacecraft. BepiColombo will launch in August 2013 using the Russian Soyuz-2-1B launch vehicle with the Fregat-M upper stage from the Kourou cosmodrome in French Guiana . Arrival at Mercury scheduled for August 2019 Mercury Exploration

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

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

terrestrial planets and giant planets

Slide 3

General characteristics dynamic properties of terrestrial planets

General characteristics of the terrestrial planets

The similarity of the terrestrial planets does not exclude significant

differences in weight, size and other characteristics

Slide 4

MERCURY

Slide 5

Mercury is the closest planet to the Sun.

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.

Slide 6

Mercury is located close to the Sun.

The maximum elongation of Mercury is only 28 degrees,

therefore it is very difficult to observe.

The best photos of Mercury from Earth

Transit of Mercury across the solar disk

Slide 7

Comparative sizes of Mercury and other celestial bodies

In size, Mercury can be compared with large

satellites of other planets in the solar system

Slide 8

The surface of Mercury in photographs taken from close up

distances, replete with craters (photos by Mariner 10 spacecraft)

Degas Crater

Copley Crater

Surface of Mercury

Computer processing

photographs of the surface of Mercury

Slide 9

There are fewer dark formations - seas - on Mercury than on the Moon

Computer processing of photographs of the surface of Mercury from the Mariner 10 spacecraft.

The light stripe at the top means there are no photographs of this area.

Slide 10

There are many craters on the surface of Mercury

Surface area of ​​the Northern Hemisphere

Mercury is about 500 km wide

Slide 11

The huge Caloris pool (left),

reaching a diameter of 1300 km,

has a strong resemblance to circular

seas on the Moon.

It was probably formed as a result

collision of Mercury with a large

celestial body at an early stage

geological history of Mercury.

The pool is the result of the outflow

lava from the bowels of the planet after a collision.

Smooth, rounded plains were discovered on the surface of the planet,

received the name pools due to their resemblance to the lunar “seas”.

Slide 12

Mercury makes two revolutions around the Sun in the same time, during which it manages to turn around its axis three times.

A solar day on Mercury lasts 176 Earth days.

those. exactly 2 Mercury years.

The average speed of Mercury's orbit is 47.9 km/s.

Quickly rushing along its orbit, Mercury lazily turns around its axis.

Day and night last 88 days, i.e. equal to the year of the planet.

earthly years and months

Slide 13

Mercury's rotation axis is almost perpendicular to the orbital plane.

The change of seasons on Mercury is not caused by the tilt of the axis,

and by changing the distance to the Sun.

Slide 14

Chemical composition Mercury's atmosphere

Data on the atmosphere of Mercury indicate only its strong rarefaction.

The pressure at the surface of the planet is 500 billion times less than at the surface of the Earth (this is less than in modern vacuum installations on Earth).

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.

Slide 15

Mercury has a weak magnetic field,

which was discovered spacecraft Mariner 10.

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

High density and availability

magnetic field show that Mercury should have

dense metal core.

The core accounts for

80% of Mercury's mass.

Slide 16

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.

View all slides

The oldest evidence of Mercury sightings can be found in Sumerian cuneiform texts dating back to the third millennium BC. e. The planet is named after the god of the Roman pantheon Mercury, an analogue of the Greek Hermes and Babylonian Naboo. The ancient Greeks of Hesiod's time called Mercury "Στίλβων" (Stilbo, the Shining One). Until the 5th century BC. e. The Greeks believed that Mercury, visible in the evening and morning skies, were two different objects. IN Ancient India Mercury was called Buddha () and Roginea. In Chinese, Japanese, Vietnamese and Korean Mercury is called the Water Star () (in accordance with the ideas of the "Five Elements". In Hebrew, the name of Mercury sounds like "Kohav Hama" (כוכב חמה) (" solar planet"). Mercury Hermes Nabu HesiodV century BC. e. Ancient India Chinese Japanese Vietnamese Korean Hebrew

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 × 10 23 kg. The average density of Mercury is quite high at 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. Acceleration free fall on Mercury it is 3.70 m/s². The second escape velocity is 4.3 km/s. Jupiter Ganymede Saturn Titan Earth Acceleration of gravity Comparative sizes of Mercury, Venus, Earth and Mars

Aphelion km 0, a. e.a. e. Perihelion km 0, a. e. Semimajor axis Semimajor axis km 0, a. e. Orbital eccentricity Orbital eccentricity 0, Sidereal period Sidereal period 87.969 days Synodic period Synodic period 115.88 days Orbital speed Orbital speed 47.87 km/s Mean anomaly Mean anomaly 174.795884° Inclination 3.38° (relative to the solar equator) Longitude of the ascending node Longitude of the ascending node 48.330541° Periapsis argument Periapsis argument 29.124279° Number of satellites no satellites

Compression

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 escarpments extending over hundreds of kilometers of 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 34 billion years there has been no large-scale movement of sections of the crust, and there has been no erosion of the surface, the latter almost completely eliminating the possibility of the existence of any significant atmosphere in the history of Mercury. lunarBeethovencrater landscapeserosion The surface resembles the lunar (picture by MESSENGER)

Mercury is the least studied terrestrial planet. Only two devices were sent to study it. The first was Mariner 10, which flew past Mercury three times in years; the closest approach was 320 km. As a result, several thousand images were obtained, covering approximately 45% of the planet's surface. Further research from Earth showed the possibility of the existence of water ice in polar craters. Mariner's

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Planet of the Solar System Mercury Completed by: Surmey Ya. Checked by: Maksimenko A.V.

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Mercury is the planet closest to the Sun in the Solar System, revolving around the Sun every 88 days. Mercury belongs to inner planets, since its orbit is closer to the Sun than the Earth's orbit.

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History and name The oldest evidence of observations of Mercury can be found in Sumerian cuneiform texts dating back to the third millennium BC. e. The planet is named after the god of the Roman pantheon Mercury, an analogue of the Greek Hermes and Babylonian Naboo. The ancient Greeks of Hesiod's time called Mercury "Στίλβων" (Stilbo, the Shining One). Until the 5th century BC. e. The Greeks believed that Mercury, visible in the evening and morning skies, were two different objects. In ancient India, Mercury was called Buddha (बध) and Roginea. In Chinese, Japanese, Vietnamese and Korean, Mercury is called the Water Star (水星) (in accordance with the ideas of the "Five Elements"). In Hebrew, the name of Mercury is "Koha in Hama" (כוכב חמה) ("Solar Planet").

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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. Comparative sizes of Mercury, Venus, Earth and Mars

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Orbital characteristics Aphelion 69,816,927 km 0.46669733 a. e. Perihelion 46,001,210 km 0.30749909 a. e. Semi-major axis 57,909,068 km 0.38709821 a. e. Orbital eccentricity 0.20530294 Sidereal period 87.969 days Synodic period 115.88 days Orbital speed 47.87 km/s Average anomaly 174.795884° Inclination 3.38° (relative to the solar equator) Longitude of the ascending node 48.330541° Periapsis argument 29.124279° Number of satellites none

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Physical characteristics Compression< 0,0006 Средний радиус 2439,7 ± 1,0 км Площадь поверхности 7,48×107 км² 0,108 Земных. Объём 6,083×1010 км³ 0,054 Земных Масса 3,3022×1023 кг 0,055 Земных Средняя плотность 5,427 г/см³ Ускорение свободного падения на экваторе 3,7 м/с² 0,38 g Вторая космическая скорость 4,25 км/с Скорость вращения (на экваторе) 10,892 км/ч Период вращения 58,646 дней (1407,5 часов) Наклон оси вращения 0,01° Прямое восхождение на северном полюсе 18 ч 44 мин 2 с 281.01° Склонение на северном полюсе 61,45° Альбедо 0,119 (Бонд) 0,106 (геом. альбедо)

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Surface 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. The surface resembles the moon (MESSENGER image)

• Mercury, the planet closest to the Sun, is difficult to study because it is mostly lost in its rays. Therefore, the initial ideas about Mercury were largely erroneous.

• Named after the Roman god Mercury, who was considered the messenger of the gods and was the fastest in the world. His most famous attribute is his winged sandals and the golden staff in his hand.

• Images from the Mariner 10 space probe, 1974-1975. showed that the surface of the planet is similar to the moon

• The moon is on the right

Mercury is on the left.

• When Mercury is seen in the sky away from the Sun, then through a telescope, it appears as the Moon in the first or last quarter, i.e. like a semicircle.

• All of Mercury is pitted with the same craters. Like the Moon, and just as dense.
• According to the decision of the International Astronomical Union, craters on Mercury are named after cultural figures: writers, poets, artists, sculptors, composers. / Beethoven, Tolstoy, Shakespeare, Dostoevsky /

• Unlike the Moon, Mercury is characterized by scarps.
• Scarps are long ledges similar to cliffs, but up to 3 km high.

General information about Mercury.

• The period of Mercury's revolution around its axis in relation to the stars is about 59 days!
• The surface temperature of the side of the planet facing the star reaches +427°C
• Due to the lack of atmosphere, the surface in the shade quickly cools to -173 ° C on the night side. .

• The average density of Mercury is 5.4 g/cm

General information about Mercury.

• The mass of Mercury is almost 20 times less than the mass of the Earth.
• Mercury is even smaller than some of the moons of Jupiter and Saturn.
• Mercury has no natural satellites.