GAPOU NSO "Baraba Medical College"

The annual movement of the Sun across the sky. Ecliptic. Movement and phases of the moon »

Lecturer: Vashurina T. V. Barabinsk, 2019

Objectives of the lesson:

• Learning goals: to form an understanding of the essence of everyday observable and rare astronomical phenomena, familiarization with scientific methods and the history of studying the Universe, gaining an idea of ​​​​the action in the Universe of physical laws discovered in terrestrial conditions, and the unity of the mega-world and the micro-world, awareness of one's place in the Solar system and the Galaxy through the study of concepts : the starry sky, the ecliptic, an explanation of the movement of stars and the Sun observed with the naked eye at various geographical latitudes, the movement and phases of the moon, the use of a star map to search for certain constellations and stars in the sky; formation of one's own position in relation to physical information received from different sources. To contribute to the formation of the ability to organize one's own activities, to choose typical methods and ways of performing exercises (OK2).

Frontal survey Stars and constellations.

Frontal survey Apparent stellar magnitude.

Frontal survey Celestial sphere.

Frontal survey Singular points of the celestial sphere.

Frontal survey Celestial coordinates and star maps.

• The apparent annual motion of the Sun (Table 1, p. 47 of the textbook)
• Daily motion of the Sun at different latitudes.

3. Change in the daily path of the Sun during the year (Fig. 29, 30)

4. Apparent movement and phases of the moon

5. Solar and lunar eclipses

The apparent movement of the Sun along the ecliptic.

Ecliptic- the apparent annual path of the center of the solar disk across the celestial sphere. The movement of the Sun along the ecliptic is caused by the annual movement of the Earth around the Sun. The center of the solar disk crosses the celestial equator twice a year - in March and September .

The annual motion of the Sun reflects the actual revolution of the Earth in orbit, the ecliptic is a trace of the section of the celestial sphere by a plane parallel to the plane of the earth's orbit, which is called the plane of the ecliptic.

Mutual position of the celestial equator and ecliptic

The intersection points of the ecliptic with the celestial equator are called

dots spring and autumn equinoxes.

Through the vernal equinox, the Sun passes from the southern hemisphere of the celestial sphere to the northern (March 21).

Through the point of the autumnal equinox, the Sun passes from the northern hemisphere of the celestial sphere to the southern one (September 23).

At the summer solstice on June 22, the Sun has its maximum declination. δ = +23°26 .

δ = -23°26.

The days of the solstice, like the days of the equinox, can change.

This is due to the fact that there are not 365 days in a year, but a little more.

The solstices are 90° apart from the equinoxes.

The equatorial coordinates of the Sun change throughout the year.

δ = -23°26´.

On the day of the spring equinox on March 21 and the autumnal equinox on September 23, the declination of the Sun is δ = 0°.

In ancient Mesopotamia, the division of the ecliptic with the constellations surrounding it into 12 parts arose, i.e. Belt of the Zodiac

The shift of the vernal equinox occurs towards the annual movement of the Sun by about 50" per year.

The constellations through which the ecliptic passes are called ecliptic constellations.

In each zodiac constellation, the Sun spends about a month, 9 degrees

The apparent annual path of the Sun passes through thirteen constellations, starting from the vernal equinox:

Aries, Taurus, Gemini, Cancer, Leo, Virgo, Libra, Scorpio, Ophiuchus, Sagittarius, Capricorn, Aquarius, Pisces.

According to ancient tradition, only twelve of them are called zodiac.

Constellation Ophiuchus to the zodiac constellations do not count .

The movement of the earth around the sun and

the apparent annual motion of the Sun along the ecliptic

Basic Earth Movements

Movement around the sun elliptical ( close to circular e=0.0167) with an average speed of 29.8 km/s.

The radius of the Earth's orbit -149.6 million km - is taken as one astronomical unit.

The orbital period is 365.256 days or one year.

Rotation around an axis Change of time of day. The axis of rotation all the time // to itself and is inclined to the plane of the orbit at an angle of 66°34".

As a result, the seasons change.

The direction of the moon's movement from west to east, for an observer from the Earth, the moon moves 13.2 degrees per day

• When the Moon is turned to the Earth with its dark, invisible side, this is called a new moon. During the full moon, the entire surface of the moon is illuminated so that it appears to us as round.

• The Moon moves around the Earth at an average speed of 1.02 km/s in an approximately elliptical orbit in a counterclockwise direction, as viewed from the Moon's orbit from the North Pole of the World.
• The semi-major axis of the Moon's orbit is 384,400 km. The period of the moon's revolution around the earth is sidereal month - equals 27.32166 days,
• The moon rotates around an axis inclined to the plane of the ecliptic at an angle of 88 0 28 ’ , with a period equal to the sidereal month, as a result of which it is always turned to the Earth by the same side.
• The planes of the equator of the Moon, the ecliptic and the lunar orbit always intersect in one straight line.

Changes in the appearance of the moon are called phases of the moon.

moon phase the part of the lunar disk that is visible in sunlight is called

Rice. 31 textbooks, p.50

The moon is visible only in the part where the sun's rays fall or the rays reflected by the Earth. This explains the phases of the moon.

appears bright narrow

the crescent of the young moon.

• Every month, the Moon, moving in its orbit, passes between the Earth and the Sun. It is turned to us by the dark side, at this time there is a new moon.
• 1-2 days after that in the western part of the sky

• After 7 days, the first quarter begins, when exactly half of the disk is illuminated.
• In the following days, the terminator becomes convex and after 14-15 days the full moon occurs.
• On the 22nd day, the last quarter is observed. The angular distance of the Moon from the Sun decreases, it again becomes a sickle, and after 29.5 days a new moon occurs again.

The interval between two successive new moons is called synodic (or sidereal) month , having an average duration of 29.5 days. If the new moon occurs near one of the nodes of the lunar orbit, a solar eclipse occurs.

A full moon near the node is accompanied by a lunar eclipse.

Problem solving

• Astronomy. Multi-level independent work with examples of problem solving
• L. A. Kirik p. 13, No. 1-5.

Questions for consolidation:

• Why does the midday height of the sun change throughout the year?
• In what direction is the apparent annual movement of the Sun relative to the stars?

Questions for consolidation:

• What is the range of the angular distance of the Moon from the Sun?
• How to determine the approximate angular distance from the Sun by the phase of the Moon?

Questions for consolidation:

• By what approximate amount does the right ascension of the moon change in a week?
• What observations need to be made to notice the movement of the Moon around the Earth?

Questions for consolidation:

• What observations prove that there is a change of day and night on the Moon?
• Why is the moon's ash light weaker than the glow of the rest of the moon, visible shortly after the new moon?

Independent work

Run time: 5 minutes

• Criteria for evaluation:
• for 3 correct answers - "3" points;
• for 4 correct answers - "4" points;
• for 5 correct answers - "5" points.

Mutual check Criteria for evaluation: for 3 correct answers - "3" points; for 4 correct answers - "4" points; for 5 correct answers - "5" points.

Job number

Answers

TASK FOR INDEPENDENT EXTRACURRICULAR WORK OF STUDENTS

• Vorontsov - Velyaminov B.A., Astronomy. A basic level of. Grade 11: textbook / B.A. Vorontsov - Velyaminov, E.K. Strout. 5th ed., revision. M.: Bustard, 2018. - 238 p.: silt, 8 sheets of color. incl. - (Russian textbook) p. 31-37 read, learn the synopsis. Make observations with the naked eye of the brightest stars and constellations.
• Topics of reports (optional at the request of the student):
• "On the history of the emergence of the names of constellations and stars";
• "Calendar history";
• "Storage and transmission of accurate time".

• Criteria for evaluation:
• the student learned the abstract - "3" points;
• the student read the paragraphs and learned the abstract, did not answer an additional question on the topic - "4" points;
• the student has learned the abstract, owns the information from the textbook, answered an additional question on the topic - "5" points.
• The student prepared a message that meets the requirements, answered an additional question - "5" points.

THANK YOU BEHIND ATTENTION!

List of sources used

• Astronomy Multi-level independent work with examples of problem solving L. A. Kirik [Electronic resource]/ Medic-03 // Access mode file:///D:/movies%20%20physics/med%20college/Development%20events/ASTRONOMY/Astronomy/Kirik%20Independent%20and%20test%20work%20%20Astronomy.pdf
• Vorontsov - Velyaminov B.A., Astronomy. A basic level of. Grade 11: textbook / B.A. Vorontsov - Velyaminov, E.K. Strout. 5th ed., revision. M.: Bustard, 2018. - 238 p.: silt, 8 sheets of color. incl.- (Russian textbook)
• Lectures on astronomy Lesson 2. [Electronic resource] / Infofiz // Access mode http://infofiz.ru/index.php/mirastr/astronomlk/501-lk2astr
• Test on the topic “Motion and phases of the moon” Electronic resource] / Z nanio // Access mode https://znanio.ru/media/test_po_astronomii_dvizhenie_i_fazy_luny-123294/144809

The ecliptic is the circle of the celestial sphere,
along which the apparent annual motion of the Sun takes place.

Zodiac constellations - constellations through which the ecliptic passes
(from the Greek "zoon" - animal)
Each zodiacal
constellation Sun
crosses approximately
per month.
It is traditionally believed that the zodiac
constellations 12, although in fact the ecliptic
also crosses the constellation Ophiuchus,
(located between Scorpio and Sagittarius).

In a day, the Earth travels about 1/365th of its orbit.
As a result, the Sun moves about 1° in the sky every day.
The amount of time it takes for the sun to make a full circle
on the celestial sphere, called the year.

In the days of spring and autumn
equinoxes (March 21 and 23
September) The sun is on
celestial equator and has
declination 0°.
Both hemispheres of the earth
illuminated the same way: the border
day and night passes right through
poles, and day equals night in
all points on earth.

The axis of rotation of the Earth is inclined to the plane of its orbit by 66°34´.
The earth's equator has an inclination of 23°26' with respect to the plane of the orbit,
therefore, the inclination of the ecliptic to the celestial equator is 23°26´.
On the day of the summer solstice
(June 22) Earth turned to
Sun with its North
hemisphere. Summer is here
at the North Pole -
polar day, and the rest
hemisphere days
longer than the night.
The sun rises above
the plane of the earth (and
celestial) equator at 23°26´.

The axis of rotation of the Earth is inclined to the plane of its orbit by 66°34´.
The earth's equator has an inclination of 23°26' with respect to the plane of the orbit,
therefore, the inclination of the ecliptic to the celestial equator is 23°26´.
On the winter solstice
(December 22) when the Northern
hemisphere is illuminated worse
all, the sun is below
celestial equator at an angle
23°26´.

Summer and winter solstice.
Spring and autumn equinoxes.

Depending on the position of the Sun on the ecliptic, its height above
horizon at noon - the moment of the upper climax.
Having measured the noon height of the Sun and knowing its declination on that day,
the geographic latitude of the observation point can be calculated.

By measuring the noon
the height of the sun and knowing it
declination on this day,
can be calculated
geographical latitude
places of observation.
h = 90° – ϕ + δ
ϕ = 90°– h + δ

The daily movement of the Sun during the equinoxes and solstices
at the Earth's pole, at its equator and at mid-latitudes

Exercise 5 (p. 33)
No. 3. On what day of the year were the observations made, if the height
Sun at a geographical latitude of 49° was equal to 17°30´? .
h = 90° – ϕ + δ
δ = h - 90° + ϕ
δ = 17°30´ - 90° + 49° = 23.5°
δ = 23.5° on the day of the solstice.
Since the height of the sun is
geographic latitude 49°
was only 17°30´, then this
winter solstice -
21 December

Homework
16.
2) Exercise 5 (p. 33):
No. 4. The midday altitude of the Sun is 30° and its declination is -19°. Define geographic
latitude of the observation site.
No. 5. Determine the noon height of the Sun in Arkhangelsk (geographic latitude 65 °) and
Ashgabat (geographical latitude 38°) on the days of the summer and winter solstices.
What are the differences in the altitude of the Sun:
a) on the same day in these cities;
b) in each of the cities on the solstices?
What conclusions can be drawn from the obtained results?

Vorontsov-Velyaminov B.A. Astronomy. A basic level of. 11 cells : textbook / B.A. Vorontsov-Velyaminov, E.K.Straut. - M.: Bustard, 2013. - 238s
CD-ROM "Library of electronic visual aids" Astronomy, grades 9-10 ". OOO "Physikon" 2003
https://www.e-education.psu.edu/astro801/sites/www.e-education.psu.edu.astro801/files/image/Lesson%201/astro10_fig1_9.jpg
http://mila.kcbux.ru/Raznoe/Zdorove/Luna/image/luna_002-002.jpg
http://4.bp.blogspot.com/_Tehl6OlvZEo/TIajvkflvBI/AAAAAAAAAmo/32xxNYazm_U/s1600/12036066_zodiak_big.jpg
http://textarchive.ru/images/821/1640452/m30d62e6d.jpg
http://textarchive.ru/images/821/1640452/69ebe903.jpg
http://textarchive.ru/images/821/1640452/m5247ce6d.jpg
http://textarchive.ru/images/821/1640452/m3bcf1b43.jpg
http://tepka.ru/fizika_8/130.jpg
http://ok-t.ru/studopedia/baza12/2151320998969.files/image005.jpg
http://www.childrenpedia.org/1/15.files/image009.jpg

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Slides captions:

Earth Movement

Question 1 The reason for the daily rotation of the celestial sphere is: A) The proper motion of the stars; B) The rotation of the Earth around its axis; C) the movement of the earth around the sun; D) The movement of the Sun around the center of the Galaxy.

Question 2 The North Pole of the world at present: A) is very close to the star α Ursa Major; B) is located near the brightest star in the entire sky - Sirius; C) is very close to the North Star; D) is located in the constellation Lyra near the star Vega.

Question 3 The constellation Ursa Major makes a complete revolution around the North Star in a time equal to A) one night; B) one day; B) one month D) one year.

Question 4 In what place on Earth does the daily movement of stars occur parallel to the horizon plane? A) at the equator B) at mid-latitudes of the northern hemisphere; B) at the poles D) at mid-latitudes of the southern hemisphere of the Earth.

Question 5 Where can all the constellations be observed on Earth? A) at the equator B) at mid-latitudes of the northern hemisphere; B) at the poles D) at mid-latitudes of the southern hemisphere of the Earth.

The motion of the Earth around the Sun and the apparent annual motion of the Sun along the ecliptic

The visible annual path of the Sun passes through thirteen constellations: Aries, Taurus, Gemini, Cancer, Leo, Virgo, Libra, Scorpio, Ophiuchus, Sagittarius, Capricorn, Aquarius, Pisces. According to ancient tradition, only twelve of them are called zodiacal. The constellation Ophiuchus is not considered a zodiac constellation.

The Sun spends about a month in each zodiac constellation.

Summer Solstice - June 22 Winter Solstice - December 22 Spring Equinox - March 21 Autumn Equinox - September 23

Reason for the change of seasons

Cosmic phenomena Celestial phenomena arising from these cosmic phenomena Rotation of the Earth around its axis 1) the shape of the Earth; 2) daily rotation of the celestial sphere around the axis of the world from east to west; the rising and setting of the luminaries; 3) change of day and night; 4) ebbs and flows. Rotation of the Earth around the Sun 1) annual change in the appearance of the starry sky (apparent movement of heavenly bodies from west to east); 2) the annual movement of the Sun along the ecliptic from west to east; 3) change in the midday height of the Sun above the horizon during the year; a) change in the length of daylight hours during the year; b) polar day and polar night at high latitudes of the planet; 4) change of seasons

On the topic: methodological developments, presentations and notes

Presentation for the lesson "The scent of the sun in the art of symbolism"

Explanatory note Modern school education provides for the formation of students' general educational skills and ...

The annual movement of the Sun. Ecliptic, Movement and phases of the Moon. Eclipses of the Sun and Moon

The material represents the methodological development of a combined lesson on the topic "annual motion of the Sun. Ecliptic. Motion and phases of the Moon. Eclipses of the Sun and Moon". The task of the lesson is to correct ...

Page 1 of 4

Name of sections and topics		Watch volume	Level of development
	The apparent annual motion of the Sun. Ecliptic. Apparent movement and phases of the moon. Eclipses of the Sun and Moon. Reproduction of definitions of terms and concepts (culmination of the Sun, ecliptic). Explanation of the movements of the Sun observed with the naked eye at different geographical latitudes, the movement and phases of the Moon, the causes of eclipses of the Moon and the Sun.
Time and calendar.	Time and calendar. Precise time and determination of geographic longitude. Reproduction of definitions of terms and concepts (local, zone, summer and winter time). Explanation of the need to introduce leap years and a new calendar style.	1	2

Topic 2.2. The annual movement of the Sun across the sky. Ecliptic. Movement and phases of the moon.

2.2.1. The apparent annual motion of the Sun. Ecliptic.

Even in ancient times, observing the Sun, people discovered that its midday height changes throughout the year, as does the appearance of the starry sky: at midnight, stars of different constellations are visible above the southern part of the horizon at different times of the year - those that are visible in summer are not visible in winter and vice versa. Based on these observations, it was concluded that the Sun moves across the sky, moving from one constellation to another, and completes a complete revolution during the year. The circle of the celestial sphere, along which the apparent annual movement of the Sun occurs, was called ecliptic.

(ancient Greek ἔκλειψις - ‘eclipse’) - a large circle of the celestial sphere, along which the apparent annual movement of the Sun occurs.

The constellations along which the ecliptic passes are called zodiacal(from the Greek word "zoon" - animal). Each zodiac constellation the Sun crosses in about a month. In the XX century. one more was added to their number - Ophiuchus.

As you already know, the movement of the Sun against the background of stars is an apparent phenomenon. It occurs due to the annual revolution of the Earth around the Sun.

Therefore, the ecliptic is that circle of the celestial sphere, along which it intersects with the plane of the earth's orbit. In a day, the Earth travels about 1/365th of its orbit. As a result, the Sun moves about 1° in the sky every day. The period of time during which it goes around a full circle in the celestial sphere is called year.

From the course of geography, you know that the axis of rotation of the Earth is inclined to the plane of its orbit at an angle of 66 ° 30. Therefore, the earth's equator has an inclination of 23 ° 30 with respect to the plane of the orbit. This is the inclination of the ecliptic to the celestial equator, which it crosses at two points: the spring and autumn equinoxes.

These days (usually March 21 and September 23) the Sun is at the celestial equator and has a declination of 0°. Both hemispheres of the Earth are illuminated by the Sun in the same way: the boundary of day and night passes exactly through the poles, and day is equal to night at all points on the Earth. On the day of the summer solstice (June 22), the Earth is turned towards the Sun with its Northern Hemisphere. Here it is summer, at the North Pole - a polar day, and in the rest of the hemisphere the days are longer than the night. On the day of the summer solstice, the Sun rises above the plane of the earth's (and celestial) equator by 23°30".

♈ - vernal equinox point. March 21 (day equals night).
Sun coordinates: α ¤=0h, δ ¤=0о
The designation has been preserved since the time of Hipparchus, when this point was in the constellation ARIES → now it is in the constellation FISH, In 2602 it will move into the constellation AQUARIUS.

♋ is the summer solstice. June 22 (the longest day and the shortest night).
Sun coordinates: α¤=6h, ¤=+23o26"
The designation of the constellation Cancer has been preserved since the time of Hipparchus, when this point was in the constellation of Gemini, then it was in the constellation of Cancer, and since 1988 it moved into the constellation of Taurus.

♎ is the day of the autumnal equinox. September 23 (day equals night).
Sun coordinates: α ¤=12h, δ t size="2" ¤=0o
The designation of the constellation Libra was preserved as the designation of the symbol of justice under the emperor Augustus (63 BC - 14 AD), now in the constellation Virgo, and in 2442 it will move to the constellation Leo.

♑ - winter solstice. December 22 (the shortest day and the longest night).
Sun coordinates: α¤=18h, δ¤=-23о26"
The designation of the constellation Capricorn has been preserved since the time of Hipparchus, when this point was in the constellation of Capricorn, now in the constellation of Sagittarius, and in 2272 it will move into the constellation of Ophiuchus.

Depending on the position of the Sun on the ecliptic, its height above the horizon changes at noon - the moment of the upper climax. By measuring the noon altitude of the Sun and knowing its declination on that day, one can calculate the geographic latitude of the observation site. This method has long been used to determine the location of the observer on land and at sea.

The daily paths of the Sun on the days of the equinoxes and solstices at the Earth's pole, at its equator and at mid-latitudes are shown in the figure.

slide 1

Visible Movements of Celestial Bodies Cosmos is all that is, that has ever been, and will ever be. Carl Sagan.

slide 2

Since ancient times, people have observed in the sky such phenomena as the apparent rotation of the starry sky, the change in the phases of the moon, the rising and setting of heavenly bodies, the apparent movement of the Sun across the sky during the day, solar eclipses, the change in the height of the Sun above the horizon during the year, lunar eclipses. It was clear that all these phenomena are connected, first of all, with the movement of celestial bodies, the nature of which people tried to describe with the help of simple visual observations, the correct understanding and explanation of which took shape over the centuries.

slide 3

The first written references to celestial bodies originated in ancient Egypt and Sumer. The ancients distinguished three types of bodies in the firmament of heaven: stars, planets and "tailed stars". The differences come just from observations: Stars remain motionless relative to other stars for quite a long time. Therefore, it was believed that the stars were "fixed" on the celestial sphere. As we now know, due to the rotation of the Earth, each star "draws" a circle in the sky.

slide 4

The planets, on the contrary, move across the sky, and their movement can be seen with the naked eye for an hour or two. Even in Sumer, 5 planets were found and identified: Mercury,

slide 5

slide 6

Slide 7

Slide 8

Slide 9

slide 10

slide 11

"Tailed" stars of the comet. Appeared infrequently, symbolized troubles.

slide 12

Configuration - the characteristic relative position of the planet, the Sun and the Earth. The ecliptic is a large circle of the celestial sphere, along which the apparent annual movement of the Sun occurs. Accordingly, the plane of the ecliptic is the plane of rotation of the Earth around the Sun. The lower (inner) planets move in orbit faster than the Earth, and the upper (outer) planets are slower. Let us introduce the concepts of specific physical quantities that characterize the motion of the planets and allow us to make some calculations:

slide 13

Perihelion (ancient Greek περί "peri" - around, near, near, other Greek ηλιος "helios" - the Sun) is the closest point to the Sun in the orbit of a planet or other celestial body of the solar system. The antonym of perihelion is apohelion (aphelion) - the most distant point of the orbit from the Sun. The imaginary line between aphelion and perihelion is called the line of apsides. Sidereal (T - stellar) - the period of time during which the planet makes a complete revolution around the Sun in its orbit relative to the stars. Synodic (S) - the time interval between two successive identical planetary configurations

slide 14

The three laws of planetary motion relative to the sun were empirically derived by the German astronomer Johannes Kepler at the beginning of the 17th century. This was made possible thanks to many years of observations by the Danish astronomer Tycho Brahe.

slide 15

slide 16

slide 17

slide 18

The most simply visible movement of the planets and the Sun is described in the frame of reference associated with the Sun. This approach was called the heliocentric system of the world and was proposed by the Polish astronomer Nicolaus Copernicus (1473-1543).

slide 19

In ancient times and up to Copernicus, it was believed that the Earth is located at the center of the Universe and all celestial bodies revolve along complex trajectories around it. This system of the world is called the geocentric system of the world.

slide 20

The complex apparent motion of the planets in the celestial sphere is due to the revolution of the planets of the solar system around the sun. The very word "planet" in ancient Greek means "wandering" or "tramp". The trajectory of a celestial body is called its orbit. The velocities of the planets in their orbits decrease with the distance of the planets from the Sun. The nature of the movement of the planet depends on which group it belongs to. Therefore, in relation to the orbit and conditions of visibility from the Earth, the planets are divided into internal (Mercury, Venus) and external (Mars, Saturn, Jupiter, Uranus, Neptune, Pluto), or, respectively, in relation to the Earth's orbit, into lower and upper.

slide 21

Since, during observations from the Earth, the movement of the planets around the Sun is also superimposed on the movement of the Earth in its orbit, the planets move across the sky from east to west (direct movement), then from west to east (reverse movement). Moments of direction change are called stops. If you put this path on the map, you get a loop. The size of the loop is the smaller, the greater the distance between the planet and the Earth. The planets describe loops, and not just move back and forth in a single line, solely due to the fact that the planes of their orbits do not coincide with the plane of the ecliptic. Such a complex loop-like character was first noticed and described using the example of the apparent motion of Venus.

slide 22

slide 23

It is a known fact that the movement of certain planets can be observed from the Earth at a strictly defined time of the year, this is due to their position over time in the starry sky. The configurations of the inner and outer planets are different: for the lower planets these are conjunctions and elongations (the largest angular deviation of the planet's orbit from the orbit of the Sun), for the upper planets these are quadratures, conjunctions and oppositions. For the Earth-Moon-Sun system, a new moon occurs in the lower conjunction, and a full moon occurs in the upper one.

slide 24

For the upper (external) connection - the planet behind the Sun, on the straight line Sun-Earth (M 1). opposition - a planet behind the Earth from the Sun - the best time to observe the outer planets, it is completely illuminated by the Sun (M 3). quadrature western - the planet is observed in the western side (M 4). eastern - observed in the eastern side (M 2).