Celestial sphere. Elements of the celestial sphere

Celestial sphere

When we observe the sky, all astronomical objects appear to be located on a dome-shaped surface, in the center of which the observer is located.

This imaginary dome forms the upper half of an imaginary sphere called the "celestial sphere."

P – north celestial pole

True horizon

N – north point

S – south point

Celestial meridian

R ' – south celestial pole

Noon Line

Z’ - nadir

The celestial sphere plays a fundamental role in indicating the position of astronomical objects.

Horizontal coordinates

In a horizontal coordinate system, the position of an object is determined relative to the horizon and relative to the direction south (S).

Vertical – height circle

Horizontal coordinates

The position of the star M is determined by its height h (angular distance from the horizon along the great circle - vertical) and azimuth A (angular distance measured to the west from the point south to the vertical).

Height varies: from 0 ° up to +90 ° (above the horizon) from 0 ° up to -90 ° (below the horizon)

Azimuth changes: from 0 ° up to 360 °

Climaxes of celestial bodies

Moving around the axis of the world, the luminaries describe daily parallels.

The culmination is the passage of the luminary through the celestial meridian.

Climaxes of celestial bodies

During the day there are two climaxes: upper and lower

The non-setting luminary has both culminations above the horizon. The non-rising star has both culminations below the horizon.

But for some astronomy problems, the coordinate system must be independent of the observer’s position and time of day. Such a system is called “equatorial”.

Equatorial coordinates

Due to the rotation of the Earth, stars constantly move relative to the horizon and cardinal points, and their coordinates in the horizontal system change.

Celestial equator

Declension

α – right ascension

Vernal equinox point

Declension circle

Equatorial coordinates

Ecliptic - the apparent path of the Sun across the celestial sphere.

Equatorial coordinates

The "declination" of a star is measured by its angular distance north or south of the celestial equator.

"Right ascension" is measured from the vernal equinox to the star's declination circle.

"Right Ascension" varies from 0 ° up to 360 ° or from 0 to 24 hours.

Ecliptic

The Earth's rotation axis is tilted approximately 23.5° relative to the perpendicular to the ecliptic plane.

The intersection of this plane with the celestial sphere gives a circle - the ecliptic, the apparent path of the Sun over a year.

Ecliptic

Every year in June, the Sun rises high in the sky in the Northern Hemisphere, where the days become long and the nights short.

Moving to the opposite side of the orbit in December, in our north, the days become short and the nights become long.

Ecliptic

The Sun travels through the entire ecliptic in a year, moving 1 ° , having visited each of the 12 zodiac constellations for a month.

Celestial sphere

When we observe the sky, all astronomical objects appear to be located on a dome-shaped surface, in the center of which the observer is located.

This imaginary dome forms the upper half of an imaginary sphere called the "celestial sphere."

Elements of the celestial sphere

P – north celestial pole

True horizon

N – north point

S – south point

Celestial meridian

R ' – south celestial pole

Noon Line

Z’ - nadir

The celestial sphere plays a fundamental role in indicating the position of astronomical objects.

Horizontal coordinates

In a horizontal coordinate system, the position of an object is determined relative to the horizon and relative to the direction south (S).

Vertical – height circle

Horizontal coordinates

The position of the star M is determined by its height h (angular distance from the horizon along the great circle - vertical) and azimuth A (angular distance measured to the west from the point south to the vertical).

Height varies: from 0 ° up to +90 ° (above the horizon) from 0 ° up to -90 ° (below the horizon)

Azimuth changes: from 0 ° up to 360 °

Climaxes of celestial bodies

Moving around the axis of the world, the luminaries describe daily parallels.

The culmination is the passage of the luminary through the celestial meridian.

Climaxes of celestial bodies

During the day there are two climaxes: upper and lower

The non-setting luminary has both culminations above the horizon. The non-rising star has both culminations below the horizon.

But for some astronomy problems, the coordinate system must be independent of the observer’s position and time of day. Such a system is called “equatorial”.

Equatorial coordinates

Due to the rotation of the Earth, stars constantly move relative to the horizon and cardinal points, and their coordinates in the horizontal system change.

Celestial equator

Declension

α – right ascension

Vernal equinox point

Declension circle

Equatorial coordinates

Ecliptic - the apparent path of the Sun across the celestial sphere.

Equatorial coordinates

The "declination" of a star is measured by its angular distance north or south of the celestial equator.

"Right ascension" is measured from the vernal equinox to the star's declination circle.

"Right Ascension" varies from 0 ° up to 360 ° or from 0 to 24 hours.

Ecliptic

The Earth's rotation axis is tilted approximately 23.5° relative to the perpendicular to the ecliptic plane.

The intersection of this plane with the celestial sphere gives a circle - the ecliptic, the apparent path of the Sun over a year.

Ecliptic

Every year in June, the Sun rises high in the sky in the Northern Hemisphere, where the days become long and the nights short.

Moving to the opposite side of the orbit in December, in our north, the days become short and the nights become long.

Ecliptic

The Sun travels through the entire ecliptic in a year, moving 1 ° , having visited each of the 12 zodiac constellations for a month.

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Slide captions:

Celestial sphere 02/19/2018 1

Celestial Sphere When we observe the sky, all astronomical objects appear to be located on a dome-shaped surface, at the center of which is the observer. This imaginary dome forms the upper half of an imaginary sphere called the "celestial sphere." 02/19/2018 2

Elements of the celestial sphere 02/19/2018 3

Z - zenith Z' - nadir True horizon N - north point S - south point P - north celestial pole P ' - south celestial pole Celestial meridian Midday line Axis of the world 02/19/2018 4

Horizontal Coordinates The celestial sphere plays a fundamental role in indicating the position of astronomical objects. In a horizontal coordinate system, the position of an object is determined relative to the horizon and relative to the direction south (S). 02/19/2018 5 The position of the star M is given by its height h (angular distance from the horizon along the great circle - vertical) and azimuth A (angular distance measured to the west from the point south to the vertical).

Z Z' N S P P' M h Vertical - height circle A 02/19/2018 6 Height varies: from 0 ° to +90 ° (above the horizon) from 0 ° to -90 ° (below the horizon) Azimuth varies: from 0 ° to 360 °

Climaxes of celestial bodies Climax is the passage of a luminary through the celestial meridian. Moving around the axis of the world, the luminaries describe daily parallels. 02/19/2018 7 During the day, two climaxes occur: upper and lower. For a non-setting luminary, both climaxes are above the horizon. The non-rising star has both climaxes below the horizon

Equatorial coordinates Due to the rotation of the Earth, stars constantly move relative to the horizon and cardinal points, and their coordinates in the horizontal system change. But for some astronomy problems, the coordinate system must be independent of the observer’s position and time of day. Such a system is called “equatorial”. 02/19/2018 8

Ecliptic The intersection of this plane with the celestial sphere gives a circle - the ecliptic, the apparent path of the Sun over a year. The Earth's rotation axis is tilted approximately 23.5° relative to the perpendicular to the ecliptic plane. 02/19/2018 9

Equatorial coordinates The ecliptic is the apparent path of the Sun along the celestial sphere. On March 21, the ecliptic crosses the celestial equator at the vernal equinox. 02/19/2018 10 The Sun travels through the entire ecliptic in a year, moving 1° per day, having been in each of the 12 zodiacal constellations for a month.

P P’ Celestial equator W E N S Declination circle ɤ Vernal equinox point - declination α α - right ascension 02/19/2018 11

Equatorial coordinates “Right Ascension” is measured from the vernal equinox to the star’s declination circle. The "declination" of a star is measured by its angular distance north or south of the celestial equator. . "Right Ascension" varies from 0° to 360° or from 0 to 24 hours. 02/19/2018 12

The height of the luminary at the upper culmination at δ

The height of the luminary at the upper culmination at δ > φ h max = 90° + φ – δ δ Polaris Horizon Celestial equator φ – geographic latitude δ – declination of the luminary Celestial Pole

Exercise No. 1. The geographic latitude of Kyiv is 50°. At what altitude in this city does the upper culmination of the star Antares occur, the declination of which is -26°? Make a corresponding drawing. We build a drawing, taking into account that the height of the celestial pole above the horizon is equal to the geographic latitude: h р = φ, φ =50 °, h р = 50°  NOP=  ZOQ the declination of the star is negative, which means it is located south of the celestial equator. 2) Find the height of the upper culmination of the star h = 90° – φ + δ h = 90°– 50°– 26° = 14° φ = 50° φ = 50° δ = -26° Celestial equator Horizon Polar star Celestial pole O

Ecliptic Every year in June, the Sun rises high in the sky in the Northern Hemisphere, where the days become long and the nights short. Moving to the opposite side of the orbit in December, in our north, the days become short and the nights become long. June 22 – summer solstice December 22 – winter solstice March 21 – vernal equinox September 23 – autumn equinox 02/19/2018 16

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Astronomy is the science of the Universe, studying the structure, origin and development of celestial bodies and systems.

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1. Aristotle in the 4th century. BC e. believed that the Earth was in the center of the world, and the Sun, Moon, and stars were attached to transparent crystal spheres and revolved around it. Observing lunar eclipses, he concluded that the Earth has a spherical shape. The earthly world, according to Aristotle, consists of earth, air, water and fire. The heavenly world consists of a special substance - plenea, a kind of ether.

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2. In the II century. n. e. The Alexandrian astronomer Ptolemy, based on the ideas of Aristotle and other scientists, created a geocentric system of the world. According to Ptolemy's theory, the number of celestial spheres is 55. The geocentric system of the world could not explain the movement of the planets and a number of other observed phenomena.

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3. N. Copernicus in 1543 published the book “On the Revolution of the Heavenly Circles,” in which he showed that the movement of celestial bodies can be easily explained on the basis of the heliocentric system of the world, according to which the Sun is at the center of the world. Copernicus and his students made calculations of the future positions of celestial bodies, which turned out to be quite accurate. The teachings of Copernicus were rejected by the Catholic Church, which saw in it a contradiction with the Bible, which stated that man is at the center of the Universe.

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4. Giordano Bruno added a number of new ideas to the teachings of Copernicus. According to Bruno, there are many solar-like systems in the Universe. Planets revolve around stars. Stars are born and die, so life in the Universe is endless. Giordano Bruno was declared a heretic, hid for several years, and the Inquisition lured him to Italy by deception. Giordano Bruno was demanded to renounce his views, but he continued to insist on the justice of his ideas and on February 17, 1600 he was executed in Rome. This execution not only did not stop the spread of Bruno's ideas, but, on the contrary, aroused great public interest in them.

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5. In 1557, the Danish astronomer Tycho Brahe discovered errors in Copernicus' calculations. In 1577 he calculated the positions of comets. The results he obtained also contradicted Ptolemy’s theory, according to which comets appear in the empty space between the Moon and the Earth. Tycho Brahe created a planetary system and compiled a large catalog of fixed stars. To help with the calculations, he invited Johannes Kepler and set him the task of determining the trajectory of the planets.

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6. After the death of Tycho Brahe, Johannes Kepler continued to work on analyzing the huge amount of observational results that Brahe left him. In 1619, he published a work in which three famous laws (Kepler's laws) were formulated.

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7. On November 10, 1619, in Bavaria, Rene Descartes decided to create analytical geometry and use mathematical methods in philosophy. He expressed the main principle of his philosophy with the following well-known aphorism: “I think, therefore I exist.” Any expressed ideas, according to Descartes, are true if they are clear and definite. He viewed the entire Universe as a mechanism. God created matter and endowed it with movement, after which the world began to develop according to the laws of mechanics. From a world consisting of material particles, Descartes created the Copernican Universe as we observe it. So, by the middle of the 16th century. The universe has gone from closed to open, mostly empty, in which particles move and collide, and between two collisions they move at a constant speed.

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8. In 1632, the Italian scientist Galileo Galilei published the book “Dialogue on the two most important systems of the world - Ptolemaic and Copernican.” In this book, Copernicus's heliocentric system clearly defeated Ptolemy's geocentric system. Galileo himself was a supporter of the heliocentric system, since his observations of the Sun, Moon, Venus and Jupiter using the telescope he created showed the presence of satellites of Jupiter, the existence of phases of Venus similar to the lunar ones, and the fact that the Sun rotates around an axis. All his observations showed that the Earth does not have any special advantages, but behaves in the same way as other planets. Galileo was summoned to the Inquisition, where, under pain of torture and execution, he renounced the “heresy”, strict supervision was established over him, and he could no longer engage in research. (In 1982, Pope John Paul admitted the church's mistake and cleared Galileo of all charges.)

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9. The final triumph of the heliocentric system came after I. Newton’s discovery of the law of universal gravitation. Based on this law, it was possible to derive Kepler's laws and give an accurate description of the movement of celestial bodies.

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10. But, despite the harmony and argumentation of Newton’s theory, there was a phenomenon that confirmed doubts about the daily rotation of the Earth. If the Earth rotated, the position of the stars would have to change. However, there seemed to be no change. The first experimental proof of the Earth's motion around the Sun was made in 1725 by the English astronomer James Bradley. He discovered the displacement of stars. Stars shift from their average position by 20" in the direction of the Earth's velocity vector (the phenomenon of light aberration). In 1837, Russian astronomer V.Ya. Struve measured the annual parallax of the star Vega, which made it possible to determine the Earth's rotation speed. Currently, no one has The fact of the Earth's rotation around its own axis and its rotation around the Sun is doubtful. Based on these facts, many phenomena occurring on Earth are explained.

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11. The most active development of astronomy occurred in the twentieth century. This was facilitated by the creation of high-resolution optical and radio telescopes, as well as the possibility of research from artificial Earth satellites, which made it possible to conduct observations outside the atmosphere. It was in the twentieth century. the world of galaxies was discovered. The study of the spectra of galaxies allowed E. Hubble (1929) to detect the general expansion of the Universe predicted by A.A. Friedman (1922) based on A. Einstein’s theory of gravity. New types of cosmic bodies were discovered: radio galaxies, quasars, pulsars, etc. The foundations of the theory of the evolution of stars and the cosmogony of the Solar System were also developed. The largest achievement of astrophysics of the twentieth century. became relativistic cosmology - the theory of the evolution of the Universe as a whole.

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Otto Yulievich Schmidt (1891 - 1956) - Russian scientist, statesman, one of the organizers of the development of the Northern Sea Route. He was the organizer and leader of many expeditions to the North Pole, in particular, expeditions on the Sedov (1929 - 1930), Sibiryakov (1932), Chelyuskin (1933 - 1934), an air expedition to organize the drifting station SP-1 "(1937). He developed a cosmogonic hypothesis for the formation of solar system bodies as a result of the condensation of a circumsolar gas-dust cloud. Works on higher algebra (group theory). In 1935 O.Yu. Schmidt was elected academician from 1935 to 1942. was vice-president of the USSR Academy of Sciences. In 1937 he was awarded the title Hero of the Soviet Union. In 1932 - 1939 was the head of the Main Northern Sea Route. The enormous merit of O.Yu. Schmidt was the creation of the Great Soviet Encyclopedia, of which he was the founder and editor-in-chief from 1924 to 1942.

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Fred Hoyle (b. 1915) - English astrophysicist. Works on stellar and planetary cosmogony, the theory of the internal structure and evolution of stars, cosmology. Hoyle is the author of many science fiction works.

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Astrometry is the science of measuring space and time. Theoretical astronomy provides methods for determining the orbits of celestial bodies from their apparent positions, and methods for calculating ephemeris from the known elements of their orbits. Celestial mechanics - studies the laws of motion of celestial bodies under the influence of the forces of universal gravity, determines the masses and shape of celestial bodies and the stability of their systems. Astrophysics - studies the structure, physical properties and chemical composition of celestial objects. Stellar astronomy - studies the patterns of spatial distribution and movement of stars, stellar systems and interstellar matter. Cosmogony - examines questions of the origin and evolution of celestial bodies. Cosmology - studies the general laws of the structure and development of the Universe.

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On a dark night we can see about 2500 stars in the sky, which differ in brightness and color. It seems they are attached to the celestial sphere and revolve around the Earth with it. To navigate among them, the sky was divided into 88 constellations. In the 2nd century BC. Hipparchus divided stars according to their brightness into stellar magnitudes; he classified the brightest as stars of the first magnitude, and the faintest, barely visible with the naked eye, as stars of the sixth magnitude. A special place among the constellations is occupied by 12 zodiacal ones, through which the annual path of the Sun passes - the ecliptic.

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Constellations are a set of bright stars connected into shapes named after characters from ancient myths and legends, animals or objects.

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The stars of the constellations are designated by letters of the Greek alphabet. α is the brightest star in the constellation; β - less bright; γ - less bright than β; δ, ε, ζ, etc. In some constellations, the brightest stars have their own names, for example, Vega (α-star in the constellation Lyra), Deneb (α-star in the constellation Cygnus).

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“Space mysteries” - Talk about the need to study such natural phenomena. In 1972, an asteroid measuring 60-80 meters flew towards the earth. The father did not agree for a long time, but finally gave in to the young man’s wishes. Asteroids. The emergence of meteriotes. But Phaeton lost his way among the heavenly constellations. The beautiful legend received real scientific substantiation and assumptions about the origin of asteroids.

“Nebesni tila” - Ostannya quarter. Berezen. The sun is one of the billions of stars in our galaxy. Pegasus is one of the 88 visible stars of the bright sky. Outside the blackout of the Sun near France in 1999. Spring. More Galileo Galilei, waving the Sun behind the help of the telescope, marking the new flame. We should divide our planet into two parts. Presentation “Heavenly Bodies”.

“Points of the celestial sphere” - The equatorial coordinates of the Sun continuously change throughout the year. On the day of the winter solstice, December 22, the declination of the Sun? = -23°27?. The relative position of the celestial equator and the ecliptic. The position of the luminaries on the celestial sphere is determined by equatorial coordinates. The ecliptic is the apparent annual path of the center of the solar disk along the celestial sphere.

"The Origin of Galaxies" - The number of stars and the sizes of galaxies can vary. Elliptical galaxies. The sizes of galaxies range from several thousand to several hundred thousand light years. It is now believed that the cores of some galaxies are quasars. Evolution of galaxies. Our Galaxy is also a barred spiral galaxy.

“Small bodies of the solar system” - Types of small bodies. Meteorites. Asteroids. Comets are among the most spectacular bodies in the solar system. The Earth's surface is constantly bombarded by celestial bodies of various sizes. Asteroids are small bodies of the Solar System. Comets. Comets Asteroids Meteorites. Small bodies. Comets are sources of life.

"Meteor Fall" - However, meteorites are the only extraterrestrial bodies available for direct study. Meteorites fall very often. Meteorite fall. Presentation on Astronomy. Arizona meteorite crater. Threat: Myths or reality. Meteorites fly at speeds from 15 to 80 km/sec. Prepared by Alexander Matveev Team “Reality”.

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