The path of the Sun

Sunrise and sunset are natural phenomena that occur regularly in our Universe. In reality, the Sun does not actually rise or set, but remains stationary. Contrary to what our ancient ancestors believed, it is not the celestial luminary that revolves around our planet. Instead, it is the Earth, along with the other seven planets, that revolves around the Sun while also rotating on its axis in a west to east direction.

Knowing the direction from which the Sun rises can be helpful for tourists to navigate their surroundings and can even serve as a substitute for a compass. Additionally, there are individuals who enjoy observing the beauty of sunsets. This article provides information on the locations where the Sun sets and rises.

General information

When asked, “On which side does the Sun rise?” most people will give what they consider to be the obvious answer: “The Sun rises in the east.” However, this answer is actually incorrect. The same can be said for the standard response to the question, “Where does the Sun set?” Both answers are only correct for two specific days of the year: September 23 and March 21, also known as the autumn and vernal equinox. On these days, the day and night are divided equally, with 12 hours of each. Therefore, it is true that the Sun rises in the east and sets in the west on these specific days.

During other periods of time, the Sun’s path across the celestial sphere follows a different route, resulting in either a shorter trajectory (which leads to longer nights) or a longer trajectory (which leads to longer days).

Additionally, it is important to mention two significant dates – December 22nd and June 21st. These dates mark the winter and summer solstices, respectively. As their names suggest, these are the days when the Sun is at its highest point in the sky. On the winter solstice, the Sun’s position is in relation to the Southern Hemisphere, while on the summer solstice, it is in relation to the Northern Hemisphere. But what is the reason for this?

The Zodiac

As it moves through the stars, the Sun creates a full circle on the celestial sphere known as the ecliptic. Along this path, the Sun passes through 13 constellations, known as the zodiac belt. These constellations are called zodiacal and have names that are often related to animals. The term “zodiac” is derived from the same root as the word “zoo,” which means “circle of animals” in Russian. Some of the zodiacal constellations bear the names of animals, while others have been given symbolic names based on popular imagination.

Constellations of the zodiac

• In March, the Sun can be found in the constellation of Pisces. All stars in this constellation are faint, not brighter than the 3rd magnitude. The point of the vernal equinox, where the Sun moves from the Southern Hemisphere to the Northern Hemisphere, is located in the constellation of Pisces.
• In April, the Sun moves into the constellation of Aries (Aries is a word that refers to the masculine gender of the word “sheep”). About 2,000 years ago, the point of the vernal equinox was located in this constellation. Due to precession, it has now shifted to the constellation of Pisces.
• In June, the Sun moves into the Gemini constellation. The most prominent stars in this constellation are Pollux and Castor. The point of the summer solstice is located within this constellation.
• During July, the Sun resides in the Cancer constellation. There are no particularly bright stars within this constellation.
• On August 20th, the Sun enters the Leo constellation. This constellation contains several dozen stars, with Regulus and Denebola being the brightest among them.
• In September, the Sun can be found in the Virgo constellation. The brightest star in this constellation is Spica. Additionally, one of the first quasars was discovered in Virgo. The point of the autumnal equinox is also located within this constellation.
• During October, the Sun passes through the Libra constellation. This is a small constellation and only three stars are visible to the naked eye.
• In November, the Sun can be found in the constellation of Scorpius. The most prominent star in this constellation is the reddish Antoros. An interesting fact about the star Zeta Scorpio is that its luminosity is 400,000 times greater than that of the Sun.
• During November, the Sun moves across the constellation of Sagittarius. It is worth noting that the center of our galaxy lies in the direction of this constellation.
• From November to December, the Sun passes through the area of the constellation Serpentor (although it is not officially recognized in astrology, the visible path of the Sun does cross it).
• In January, the Sun can be found in the constellation Capricorn, which does not have any particularly bright stars.
• During February, the Sun is located in the constellation Aquarius.

In ancient times, all zodiac constellations were given symbolic designations that are still in use today. The only exception is the constellation Serpentine, which has no symbol associated with it.

Different Types of Hemispheres and Their Variations

There are a total of four types of hemispheres: Southern Hemisphere, Northern Hemisphere, Western Hemisphere, and Eastern Hemisphere. The Western and Eastern Hemispheres differ primarily in their time zones. When it is daytime in the Western Hemisphere, it is nighttime in the Eastern Hemisphere, and vice versa. This is because the Earth rotates on its axis, exposing different parts to the Sun at different times of the day.

However, our focus lies on the Northern and Southern hemispheres, which exhibit contrasting seasons. In other words, when it’s winter in the Northern Hemisphere, it’s summer in the Southern Hemisphere, and vice versa. Similarly, spring and fall are reversed. These seasonal variations arise from the Earth’s orbit around the Sun and the uneven distribution of sunlight.

Fascinating information

Let’s discover some fascinating information about the Sun, the solitary star in our solar system.

There are a countless number of Earths that can fit inside it.

• If we were to fill the Sun with Earths, we could fit 9,600,000,000 of them inside. However, if we were to compress them and eliminate free space, that number would increase to 1,300,000. The surface area of the Sun is 11,990 times greater than that of the Earth.

It contains 99.86% of the system’s mass.

• The Sun is incredibly close to being a perfect sphere, with the difference between its equatorial and polar diameters being just 10 kilometers.

The temperature at its core reaches a staggering 15 million °C.

Also, check out: Safety guidelines for the subway: tips on how to behave at stations and on trains to avoid any issues.

• Inside the heart of the Sun, this temperature becomes achievable through fusion, a process in which hydrogen is converted into helium. Typically, hot objects undergo expansion, which could lead to the explosion of our star. However, it is kept intact by the immense force of gravity. Meanwhile, the surface temperature of the Sun is relatively “mere” 5780 °C.

Eventually, the Sun will consume the Earth.

• Once the Sun exhausts its hydrogen supply (in approximately 130 million years), it will transition to using helium. This will cause it to expand and engulf the first three planets. This phase is known as the red giant stage.

Eventually, it will shrink to the size of Earth.

• Following the red giant phase, the Sun will collapse and leave behind a compact mass resembling the size of Earth. This is referred to as the white dwarf stage.

It takes approximately eight minutes for the Sun’s rays to reach us.

• The distance between the Sun and the Earth is approximately 150 million kilometers. The speed of light, which is 300,000 kilometers per second, means that it takes about 8 minutes and 20 seconds for light to travel from the Sun to the Earth. However, it’s important to note that the photons of light that reach the Earth’s surface actually took millions of years to travel from the solar core.

The Sun has a velocity of 220 kilometers per second.

• The Sun is located around 24000-26000 light years away from the center of our galaxy. This means that its orbital path takes around 225-250 million years to complete.

The distance between the Earth and the Sun varies throughout the year.

• Due to the Earth’s elliptical orbit, the distance between the Earth and the Sun ranges from approximately 147-152 million kilometers (also known as an astronomical unit).

The Sun is a star that has an average age.

• The age of the Sun is estimated to be around 4.5 billion years, indicating that it has already consumed roughly half of its hydrogen fuel. However, this process will continue for another 5 billion years.

The Sun possesses a powerful magnetic field.

• During periods of magnetic storms, solar flares become more prominent. This phenomenon is observed as the formation of sunspots, where magnetic lines twist and rotate akin to tornadoes on Earth.

The Sun generates the solar wind.

• The solar wind is a constant stream of charged particles that traverses the entire solar system at a speed of 450 kilometers per second. The solar wind emerges from regions where the Sun’s magnetic field extends.
• The term “south” is derived from the Ancient Anglo-Anglian language. It has Gothic and Germanic origins as well. In the past, Sunday used to be referred to as “sunny day” until 700 AD. Translation has also influenced the naming process. The original Greek phrase “heméra helíou” has evolved into the Latin phrase “dies solis”.

Where does the Sun set and where does it rise?

If we consider the Northern Hemisphere, during the summer months, the Sun rises in the direction between north and east, and sets between north and west. In winter, it rises between south and east, and sets between west and south. In the seasons of fall and spring, the Sun rises between the northeast and southeast, and sets between the northwest and southwest. On the days of the fall and spring equinoxes, as mentioned earlier, it rises and sets directly in the east and west, respectively.

In the Southern Hemisphere, the situation is the opposite. This is the reason for the variation in seasons.

For instance, let’s consider the poles where the duration of nights is prolonged to several months, just like the days. In contrast, at the equator, night and day are practically indistinguishable. Consequently, there is a perpetual absence of winter and summer at the equator, with a constant and unchanging illumination.

Is it a fact that fire doesn’t cast a shadow? No, fire does cast a shadow. Although fire is not uniform and consists of layers of flames with different temperatures and colors, it also contains small unburned particles that create a frame around the flames. To make the shadow of fire more visible, a brighter light source should be directed towards the flames to create contrast. Is it true that the Moon revolves around the Earth? The Earth and the Moon actually revolve around each other. The orbits of these two celestial bodies have a common center of mass located about 1,600 kilometers below the Earth’s surface. As a result, the Earth undergoes three different rotations: around its own axis, around the Sun, and around this common center of mass. Feeling confused? Don’t worry, even Newton admitted that thinking about the Moon’s motion made his head spin.

Is it true that in the Southern Hemisphere, does the sun rise in the west? No, in the Southern Hemisphere, the sun rises in the East just like in the Northern Hemisphere. East is the direction in which the planet rotates. However, in the Northern Hemisphere, the sun appears to travel clockwise. From south to west. On the other hand, in the southern hemisphere, it appears to travel from east to west across the northern part of the sky. Consequently, its motion is actually counterclockwise.

Is it true that the Sahara Desert is the driest place on Earth? No, actually the driest place on Earth is Antarctica. It’s hard to believe, but there are parts of this icy continent that haven’t seen rain for two million years. The average annual precipitation in Antarctica is about the same as in the Sahara (25 millimeters per year), but what sets it apart is the presence of the Dry Valleys. Covering 2% of the continent, these valleys are completely devoid of ice and snow, and it never rains there.

Do dolphins really not consume water? Indeed, dolphins do not consume any water. They obtain their hydration from their diet, primarily consisting of squid and fish, and by metabolizing fat in their bodies, thus generating water.

Is it true that the northern blue whale is the largest living organism on the planet? The blue whale holds the title for the largest creature in existence today. However, when it comes to the largest living organism on Earth, that distinction goes to a mushroom. And we’re not talking about any ordinary or uncommon mushroom, but rather a colony of ordinary opiates. The officially recognized largest living organism on the planet can be found in the Malur National Wildlife Refuge in Oregon, spanning an impressive area of 890 hectares. Much of this organism lies beneath the surface, taking the form of a massive network of white fungus that wraps around tree roots, ultimately leading to tree mortality. On occasion, small patches of mushrooms break through the soil, seemingly harmless. In the past, scientists believed they were separate clusters of mushrooms scattered throughout the forest, but recent research has revealed that it is actually a single organism.

Can a cobra be mesmerized by music? This claim is false. The cobra that emerges from the hypnotist’s basket does not actually respond to the sound of the flute, but rather to its shape. Snakes are unable to discern music, despite not being deaf. Snake hearing is attuned to a frequency range of vibrations and sounds that are only produced by larger animals, rendering music meaningless to them. The “mesmerized” cobra, feeling threatened, begins to sway in sync with the movements of the instrument in order to be prepared to defend itself if necessary.

Is it accurate to say that the skin is the largest organ in the human body? Indeed, the skin makes up approximately 20% of the body’s weight. When stretched out, it can cover an area of up to two square meters.

Do humans possess a sixth sense? Absolutely, and it’s not just one additional sense, there are actually at least nine. The familiar five senses include sight, hearing, taste, smell, and touch. However, there are four other senses that are commonly acknowledged. Thermoception refers to the ability to feel warmth on our skin. Equibrioception, on the other hand, is the sense of balance, which relies on the fluid-filled cavities in our inner ear. Nociception is the capacity to perceive pain. Lastly, proprioception is our “body awareness” or understanding of where our body parts are, even when we are unable to see or feel them.

The position of the Sun within our galaxy

The Sun is situated closer to the inner boundary of the Orion arm within the Milky Way. It is located approximately 7.5-8.5 thousand parsecs away from the center of the galaxy. Furthermore, it resides within a localized region known as a “local bubble,” which is a void in the interstellar medium containing luminous gas.

Our solar system is situated within the galactic habitable zone, an area with unique attributes that are conducive to supporting life. The Sun’s movement is directed towards the Vega star in the Lyra constellation and at an angle of 60 degrees relative to the galactic center. In terms of mass, our Sun ranks 40th among the closest 50 star systems.

The Sun’s orbital path is thought to be shaped like an ellipse, but it is influenced by the galactic spiral arms, causing perturbations. It takes approximately 225-250 million years for the Sun to complete one orbit. As of now, the Sun has completed only 20-25 orbits. Below is a map of the Sun’s surface, which you can observe. If you’d like, you can use our online telescopes to view the Sun in real time. And don’t forget to stay updated on the cosmic weather, including magnetic storms and solar flares.

When the star is in the region of the vernal equinox, its right ascension is zero. This value increases each day, eventually reaching 90 degrees, while the declination reaches its maximum of +23 degrees 26 minutes. After that, there is a significant increase in right ascension and a complete decrease in declination. As a result, in the region of the autumnal equinox, the right ascension value is 180 degrees. Then there is a further increase in right ascension, and at the peak of the winter solstice, it reaches 270 degrees. The declination, on the other hand, starts at 23 degrees 26 minutes and continues to increase.

As per information from the Sun and known time

This technique is relatively new and has not yet gained a wide popularity among orienteers. However, its implementation enables you to accurately plot your route by simply having a watch with you. You can utilize either traditional mechanical watches or electronic ones.

The technique is based on the understanding that the celestial body moves along the horizon at a rate of 15 degrees per hour. Additionally, in order to apply this method effectively, you need to be aware of the star’s position every 6 hours, specifically at 6, 12, 18, and 24 hours.

Navigation using the Sun and known time is carried out in the following way:

1. The time remaining before noon or after noon is calculated. This time is considered crucial, as the Sun reaches its highest point in the sky at noon.

2. Once the time and position of the Sun are determined, the angle is calculated relative to the north-south line.

3. In the morning, the calculated angle is adjusted along the path of the Sun’s movement. The observer should be positioned to the left of the Sun, with the north appearing in front and the south behind.

4. After noon, the angle is adjusted in the opposite direction, but the observer should be positioned to the right of the Sun.

The method described is not suitable for navigating in tropical forest zones and on the equator. In these regions, such calculations will result in significant errors, so it is preferable to utilize alternative methods for determining direction, such as using a gnomon.

Observable annual movement of the Sun

The annual motion of the Sun can be explained quite reasonably and logically. There is a specific pattern that can provide a more detailed description of this phenomenon. It demonstrates that based on the Earth’s position, one can observe the Sun moving against the backdrop of varying constellations. This movement is a reflection of the Earth’s orbit around our star, completing a full revolution in one year.

The ecliptic is the great circle on the celestial sphere where the visible annual motion of a star occurs. It derives its name from the Greek word “eclipse” when translated into Russian. This circle is named as such because the phenomenon of an eclipse only occurs when both luminaries are on the same circle. It’s important to note that the plane of the ecliptic aligns perfectly with the plane of the Earth’s orbit.

Furthermore, the Sun’s constant motion along the ecliptic is observed in the same direction as the planets’ constant movement along their orbits (i.e., eastward). Throughout the year, the star sequentially passes through the 12 constellations of the zodiac, which forms the zodiacal belt (including all the well-known zodiac signs).

Due to the fact that the Earth’s orbit is inclined at an angle of 23 degrees 27 minutes to the equatorial plane, the celestial equator is also positioned at an angle to the ecliptic. The value of this angle is the same. However, it is not a constant parameter as the gravitational forces exerted by the Moon and the Sun on the Earth are constantly at work.

Therefore, in 1896, during the approval process of astronomical constant units, it was determined that the inclination should be considered at a value of 23 degrees 27 minutes 8 seconds.

There are numerous techniques available for navigating using the Sun. One can determine their direction by observing the position of a watch hand or the shadow of a gnomon, or simply by tracking the movement of the Sun along the horizon. This skill can prove invaluable, not only for reaching a specific destination, but also for ensuring personal safety.

However, it is important to note that there are certain nuances to consider when orienting oneself based on the Sun. The position of the star varies depending on the time of year and the observer’s location.

During the spring and autumn equinoxes, which fall on March 21 and September 23, the Sun rises exactly in the east and sets exactly in the west. On other days, the star’s position shifts either to the north or south, depending on the time of year.

Sunrise and sunset depending on the time of year

After the vernal equinox, as the Earth moves towards the Sun, the sunrise gradually shifts towards the north each day. On June 21, during the summer solstice, the Sun can be seen rising in the northeast and setting in the northwest. As the year progresses, the Sun’s path starts to shift towards the south, and on the winter solstice (December 22), the sunrise is observed in the southeast and the sunset in the southwest.

These calculations specifically apply to the Northern Hemisphere. If you’re looking for information on the Sun’s position in the Southern Hemisphere, it is completely opposite.

The celestial equator and the ecliptic plane

To provide a more logical and detailed explanation of the Sun’s movement, it is necessary to consider the processes occurring on the celestial equator. The ecliptic intersects with the celestial equator at two specific points known as the equinoxes. These equinoxes occur in March (21) and September (23), corresponding to the days when the length of day and night are equal on Earth.

The solstice points, which are located 90 degrees away from the equinoxes on the ecliptic, play a significant role. These points mark the highest and lowest positions of the Sun in relation to the celestial equator. The summer solstice, occurring on June 22, represents the point where the Sun is at its highest position. On the other hand, the winter solstice, which takes place on December 22, marks the point where the Sun is at its lowest position.

Using the shortest shadow cast by the gnomon

The gnomon is regarded as one of the oldest inventions that enabled the determination of both the north-south direction and the height of the Sun through the shadow it casts. A gnomon can be any vertical object (such as a pillar or column) situated on a flat, open surface.

Moreover, the gnomon serves as the main component of sundials, which are positioned precisely on the cardinal directions. Throughout ancient times, these timekeeping devices have allowed for the accurate measurement of time using the shadow.

Determining the position with a gnomon shadow

Typically, a long object is selected as the gnomon to ensure more precise measurements as the difference in shadow length is easily visible. However, longer shadows can lead to reduced clarity. This is why the top part of the gnomon is sharpened.

When using a gnomon, it is important to keep in mind a few key facts that can help improve accuracy:

1. The shadow cast by the gnomon moves from west to east, in the opposite direction of the sun’s movement.
2. The shortest shadow indicates astronomical noon, while the longest shadows occur during sunrise and sunset.
3. The speed of the gnomon’s shadow changes more rapidly at the beginning and end of the Sun’s path. During midday, the shadow moves at its slowest speed, which is advantageous for taking measurements.

Note:

Orientation with a gnomon should be done in clear, sunny weather. By observing the shortest shadow cast by the instrument, the observer can determine the direction to the north. In the Southern Hemisphere, the shadow will indicate the direction south.

This method not only allows for determining noon without relying on a clock, but also enables the identification of cardinal directions and the planning of a route accordingly.

Coordinates of the Equator

The coordinates of the Sun change unevenly throughout the year due to its erratic movement along the ecliptic, which is also tilted to the equator. Approximately half of the Sun’s visible path occurs in a 186-day period between March 21 and September 23. The remaining half takes 179 days for the rest of the year.

This irregularity is caused by the unequal speed at which the Earth orbits the Sun during its entire orbital period. The Sun is located at one of the foci of the ecliptic. According to Kepler’s second law, the line connecting these celestial objects describes the same area for equal periods of time. Therefore, the Earth experiences rapid movement during the winter season and slower movement during the summer season.

Hence, in the regions where the Sun undergoes its motion, diverse occurrences take place, with certain aspects remaining perplexing to scientists. These phenomena are contingent upon the Sun’s distance from our planet, as well as various other celestial events transpiring in outer space. Researchers continue to investigate this phenomenon, meaning that a conclusive answer to inquiries concerning the Sun’s movement is still pending.

Regarding mechanical clocks and the Sun

The concept behind this technique is that the Sun traverses the sky at half the speed of the hour hand on a mechanical clock. Consequently, if a mechanical clock is available to display the current time, one can determine the direction towards the south by observing the position of the celestial body. Once the southward direction is established, the remaining directions can be deduced.

Mechanical clocks

This rule is only applicable in regions with high latitudes. In low and middle latitudes, using clocks to determine the cardinal directions can lead to significant errors due to the uneven projection of the stars. Therefore, if a traveler becomes disoriented in the forests of such areas, relying on clocks and the position of the Sun can worsen the situation.

By following this method, one can determine the north-south direction. The steps to do so are as follows:

1. Place a mechanical watch horizontally, with the dial facing upwards.
2. Align the clock’s hour hand with the position of the celestial luminary.
3. Take note of the angle between the number “12” on the dial and the hour hand.
4. Divide this angle into two equal parts with a straight line, which will indicate the direction of the south.

In order to perform calculations conveniently and accurately, it is important to remember the following:

Additional information: methods and devices for distress signaling and emergency signaling using signal fires and torches.

• If orienteering is conducted at 6 a.m., the bisector should be divided equally into “9”.
• If the clock indicates 6 o’clock, but it is actually evening, the bisector should be directed towards the “3” division.

Note!

This rule is applicable only in the Northern Hemisphere, where the Sun moves from left to right. Different conditions apply in the opposite hemisphere.

Navigation without Numerals on a Clock

The technique of using the position of the clock’s hands for navigation is widely practiced. Don’t fret if you find yourself with a clock that lacks numerals on its face. It can still serve as a reliable tool for determining cardinal directions and finding your way to a desired destination.

Clocks without numerals are also commonly used. When using electronic clocks, simply knowing the time is not enough. It is necessary to have a depiction of a round dial that is based on the current position of the solar landmark.

For example, at 7 am, the Sun is located in the east. Then, at 13 hours, it is located in the south. And at the end of its rotation, closer to 19 hours, it indicates the western direction. By knowing these key points of the Sun’s position, it is possible to calculate the intermediate directions.

Throughout history, an eclipse of the Sun has consistently evoked a range of emotions in the uninformed, often leading to fear and alarm. Some individuals sought to exploit the event, positioning themselves as fortune tellers and clairvoyants. Not only humans, but animals as well, reacted to the sudden darkness, often perceiving it as the onset of night.

Curious fact: What is the reason behind Mars’ red color? Detailed description, captivating photos and informative video available.

Solar eclipse – diagrams

The scientific explanation of this phenomenon is straightforward: the Moon obstructs the Sun. This occurs only during the new moon phase (when all three celestial objects are approximately aligned, but not always). From the perspective of an observer on Earth, there are different types of solar eclipses:

• “Partial” – where the Moon partially covers the Sun.
• “Total” – where the solar disk is completely obscured.
• “Annular” – where the cone of the shadow cast by the Moon does not reach the Earth’s surface.
• “Total annular” or “hybrid” – where two observers at different locations simultaneously witness the same type of solar eclipse.

Astronomers have made numerous significant findings and gained the ability to observe the Sun’s corona and atmosphere due to the observation of solar eclipses. This is a task that is typically very challenging under normal circumstances. Additionally, solar eclipses are not a common occurrence for us on Earth. They happen approximately 237 times per century.

Based on the Sun’s position

Regrettably, there are instances when an individual traveler or a group of tourists find themselves lost in an unfamiliar area without a compass, map, or knowledge of the emergency azimuth. This is particularly common in the forest.

In such circumstances, one must determine a clear and direct path rather than meandering aimlessly. A helpful method involves using the Sun’s position to navigate through the forest. This allows for a quick arrival at a significant landmark, such as a highway or a river, and subsequently reaching a populated area.

There is a step-by-step process for orienting oneself based on the Sun’s position:

• Begin by calculating the azimuth relative to the solar landmark;
• then, based on the previously calculated data, proceed towards the object designated as the subsequent landmark;
• continue moving from one landmark to another until you reach a familiar or residential area.

Tips!

Keep in mind that the angle is determined in relation to the projection of the bright star, whether it is positioned in front of the observer, to the left or right. However, if the star is situated behind the observer, the azimuth should be relative to the shadow it casts.

Compass usage in determining azimuth

This write-up discusses the daily trajectory of the Sun. To explore the Sun’s yearly trajectory at the same time of day, refer to Analemma. For information on the Sun’s orbit within the galaxy, visit Solar Orbit.

This image captures the annual trajectory of the Sun as observed from Budapest in 2014.

Sun path, also known as day arc, plays a significant role in determining the length of daylight and the amount of sunlight received at a specific latitude during a particular season.

The position of the Sun relative to a location greatly influences the heat gain of buildings and the performance of solar energy systems. Accurate information about the Sun’s path and local climatic conditions is essential for making informed decisions about solar collector size, orientation, landscaping, summer shading, and cost-effective utilization of solar trackers.

Influence of the Earth’s axial tilt

The trajectory of the Sun at any given latitude and time of year can be calculated using fundamental principles of geometry. The Earth’s axis is inclined at an angle of approximately 23.5 degrees in relation to the plane of its orbit around the Sun. This axial tilt results in a 47-degree variation in declination between the solar paths during the solstices, as well as a distinct disparity between summer and winter in each hemisphere.

In the northern hemisphere, the sun during the winter months (November, December, January) rises in the southeast, moves across the sky at a slight angle in the southern direction (over 43° above the southern horizon in the tropics), and finally sets in the southwest. Throughout the day, it remains on the southern (equatorial) side of the house. A vertical window facing south (towards the equator) effectively captures the thermal energy from the sun. On the other hand, in the Southern Hemisphere (May, June, July), the winter sun rises in the northeast, reaches its highest point at a low angle in the north (more than halfway from the horizon in the tropics), and then sets in the northwest. This means that north-facing windows allow a lot of solar thermal energy to enter the house.

At the equinoxes (March 20/21 and September 22/23), the sun rises in the east and sets in the west all over the world, except at the poles. In the northern hemisphere, the highest point of the sun during the equinox is in the southern half of the sky, around halfway from the horizon at mid-latitude. On the other hand, in the southern hemisphere, the highest point of the sun during the equinox is in the northern half of the sky. When observed from the equator, the sun appears to move from left to right in the Northern Hemisphere and from right to left in the Southern Hemisphere.

The variations in solar energy paths based on latitude (and hemisphere) are crucial when it comes to efficiently designing buildings with passive solar panels. This information is essential for determining the optimal design of windows and overhangs for different seasons. Solar designers need to be aware of the specific angles at which the sun’s rays hit each location they are designing for, and how those angles align with the heating and cooling needs of that location throughout the year.

In the United States, NOAA provides accurate data on the seasonal solar paths in terms of elevation and azimuth for different locations. In the Northern Hemisphere, the “equatorial side” of a building is the south-facing side, while in the Southern Hemisphere it is the north-facing side, which experiences the peak of the summer solstice. The solar altitude is highest on December 21st.

When it is solar noon on equinox days, the sun will be directly overhead at the equator, resulting in the vertical stick not casting any shadows. On June 21, which is the summer solstice in the northern hemisphere, the vertical stick located about 23.5 degrees north of the equator in the Tropic of Cancer will also not cast any shadows. However, during other times, the shadow cast at noon will point towards the North Pole. On the other hand, at the Tropic of Capricorn, which is approximately 23.5 degrees south of the equator, the vertical stick will not cast a shadow on December 21, the summer solstice in the southern hemisphere. Similarly, at other times, the noon shadow will point towards the South Pole. If you are located north of the Tropic of Cancer, the noon shadow will always point north. Conversely, if you are located south of the Tropic of Capricorn, the noon shadow will always point south.

The shadows cast by objects at points behind and below the sunrise points will align with the true north and true south directions at solar noon only when the solar declination reaches its maximum positive value (+23.44°) or maximum negative value (-23.44°). Conversely, on the equinox days when the sun is neither inclined towards the north nor the south (0° declination), the solar shadows at noon will point north-northwest north of the equator and southeast south of the equator during the spring equinox (and will point north-northeast north of the equator and SSW south of the equator during the fall equinox).

Duration of daytime

In regions located within the polar circles (to the north and south of the Arctic Circle), there is a period each year when the Sun is not visible for a full 24 hours (during the winter solstice), as well as a period when the Sun is visible for a full 24 hours (during the summer solstice).

For areas situated at mid-latitudes, the duration of daylight hours, as well as the Sun’s altitude and azimuth, change from day to day and from season to season. The difference in length between a long summer day and a short winter day becomes greater as one moves farther away from the equator.

Visualization

The visual representations below depict the various viewpoints from Earth, specifically highlighting the positions of the Sun at different times on the solstice days. During conjunction, two distinct “day arcs” are formed by the suns. These “day arcs” represent the apparent paths that the Sun follows as it moves across the celestial sphere during the course of a day. The longer arc corresponds to the path of the Sun during midsummer, while the shorter arc represents the path during midwinter. The separation between these two arcs is 46.88° (2 × 23.44°), indicating a difference in declination between the solstice suns.

Furthermore, it is worth noting that some “ghost” suns can be observed below the horizon, with a downward angle of up to 18°, signaling the onset of twilight. These visual representations can be applied to both the northern and southern hemispheres of the Earth. For optimal viewing, the hypothetical observer should position themselves near a tree on a small island in the middle of the sea. The green arrows in the images indicate the cardinal directions.

• In the Northern Hemisphere, the left side represents the north. The sun rises in the east (indicated by the arrow pointing far), reaches its highest point in the south (on the right side) when moving to the right, and sets in the west (indicated by the arrow pointing near). During mid-summer, the positions of rising and setting are shifted to the north, while during mid-winter, they are shifted to the south.
• In the Southern Hemisphere, the left side represents the south. The sun rises in the east (indicated by the arrow pointing near), reaches its highest point in the north (on the right side) as it moves to the left, and sets in the west (indicated by the arrow pointing far). During mid-summer, the positions of rising and setting are shifted to the south, while during mid-winter, they are shifted to the north.

The following cases are illustrated:

• When observed from a latitude of 20°, the arc of the solstice day follows a specific pattern. During winter, the sun reaches its highest point at an altitude of 46.56°, while in summer, it reaches an altitude of 93.44°. However, when the angle exceeds 90°, it means that the highest point occurs at an altitude of 86.56° in the opposite cardinal direction. For instance, in the southern hemisphere, during winter, the Sun remains in the north, but during the peak of summer, it can reach its zenith in the south. While summer days are longer than winter days, the difference is not more than approximately two and a half hours. Throughout the year, the Sun’s daily path is steep near the horizon, resulting in twilight lasting only about an hour and 20 minutes in the morning and evening.
• When observed from a latitude of 50°, the path of the sun on the day of the solstice is interesting. On the winter solstice, the sun only rises to a maximum of 16.56° above the horizon at noon, whereas on the summer solstice it reaches 63.44°. This leads to a significant difference in daylight hours between summer and winter, with just over 8 hours on the winter solstice and over 16 hours on the summer solstice. Additionally, there is also a difference in the direction of sunrise and sunset. At midnight (around 1 a.m. during daylight saving time in the summer), the summer sun is 16.56° below the horizon, resulting in continued astronomical twilight throughout the night. This phenomenon is known as “gray nights,” as it is not sufficiently dark for astronomers to observe the deep sky. At latitudes above 60°, the sun is even closer to the horizon, only 6.56° away. This means that civil twilight persists for most of the night, with only a brief period of nautical twilight around local midnight. Above 66.56° latitude, there is no sunset at all, giving rise to the phenomenon known as the midnight sun.
• When observed from a latitude of 70°, the trajectory of the Sun on the solstice day appears unique. During local noon, the Sun’s highest point in the sky during the winter is at -3.44°, while in the summer it reaches 43.44°. This means that during the winter, the Sun remains below the horizon, resulting in a phenomenon known as polar night. However, there is still a period of twilight. Conversely, during local midnight in the summer, the Sun reaches its highest point at 3.44°, meaning it does not set and creates a polar day.
• When observed from either pole (90° latitude), the path of the Sun on the solstice day forms an arc. During the summer solstice, the Sun is 23.44 degrees above the horizon, while during the winter solstice it is 23.44 degrees below the horizon, regardless of the time of day. In the summer months, when the Sun rises, it will circle the sky in a clockwise direction from the North Pole and counterclockwise from the South Pole. It will maintain the same angle to the horizon, rendering the distinction between day and night meaningless. Throughout the annual cycle, the elevation of the Sun will gradually change, reaching its highest point at the summer solstice and rising or setting at the equinox. There will be long periods of twilight lasting a few days after the fall equinox and before the spring equinox.

Since ancient times, humans have recognized the vital importance of the Sun for the existence of life on Earth. The Sun was revered and even worshipped, with people often offering human sacrifices to honor it. In an effort to understand the Sun’s behavior, ancient civilizations built observatories to observe and study its movements. They sought answers to seemingly simple questions like why the Sun shines during the day, what the nature of this celestial body is, where it rises and sets, and what objects surround it. The knowledge gained from these observations guided their daily activities and plans.

Scientists were unaware of the fact that the single star in our solar system experiences seasons much like the “wet season” and “dry season”. The activity of the Sun alternates between increasing in the northern and southern hemispheres, lasting for eleven months, and decreasing for the same duration. This cycle, along with the eleven-year cycle of solar activity, directly impacts the lives of humans on Earth. During this time, powerful magnetic fields are ejected from the core of the star, resulting in hazardous solar disturbances for our planet.

It might come as a surprise to some individuals to discover that the Sun is not classified as a planet. The Sun is actually an enormous, luminous sphere composed of gases, where ongoing thermonuclear reactions occur, emitting energy that produces both light and heat. Notably, there is no other star within our solar system that resembles the Sun, and as a result, it exerts its gravitational pull on all smaller objects located within its sphere of influence, causing them to orbit the Sun along a specific path.

In space, the Solar System is not alone, but rather a part of the Milky Way, a vast galaxy that comprises numerous star systems. The Sun is situated approximately 26,000 light years away from the center of the Milky Way, resulting in a one revolution around it every 200 million years. However, the Sun also rotates around its own axis, completing a full revolution in approximately one month. These figures are approximations due to the complexities of the Sun being a plasma ball with different rotational speeds for its components. For instance, near the equator, the Sun completes a revolution in 25 days, while at the poles, it takes an additional 11 days.

Out of all the stars currently identified, our celestial body ranks fourth in terms of brightness (it shines even brighter during periods of solar activity compared to when it is in decline). The Sun, a massive ball of gaseous matter, is naturally white in color. However, due to the absorption of short-wavelength waves by our atmosphere and the scattering of sunlight at the Earth’s surface, the Sun’s light appears yellowish in color. On a clear day with a blue sky, one can observe the true white color of the Sun.

Some fascinating information about the setting and rising of the sun 9327 4.23 19

As the sole star in our solar system, the Sun serves as the exclusive source of illumination (excluding faraway stars). Despite both the Sun and the Moon being the largest and most prominent celestial bodies in our planet’s atmosphere, they possess significant differences. While the Sun emits its own light, our planet’s satellite, the Moon, lacks this capability and instead reflects the Sun’s light (thus, we can observe the Sun during the night when the Moon is illuminated by it in the sky).

The Atmosphere of the Sun

Due to the extremely high temperature of the upper layers of the Sun, which exceeds 6,000 degrees Celsius, it is not a solid object. At such extreme temperatures, even stones and metals would transform into a gaseous state. These recent conclusions were reached by scientists, who had previously speculated that the light and heat emitted by the Sun were the result of combustion.

As astronomers continued to observe the Sun, it became increasingly clear that its surface had been heated to its limit for billions of years, ruling out the possibility of any burning. According to one current hypothesis, the Sun undergoes processes similar to those of an atomic bomb, where matter transforms into energy. As a result of these thermonuclear reactions, approximately 73.5% of the Sun’s composition, which is hydrogen, is transformed into helium, accounting for nearly 25%.

Regarding the internal structure, the star is composed of gas and is connected to a planet, with the exception of having a core.

The central part

This is where all the thermonuclear reactions take place, producing heat and energy, which then pass through all the subsequent layers of the Sun and are emitted as sunlight and kinetic energy. The solar core stretches from the center of the Sun to a distance of 173,000 km (approximately 0.2 solar radius). Interestingly, the star rotates much more rapidly around its axis in the core compared to the upper layers.

Radiative transfer zone

Photon interactions in the radiative transfer zone occur when photons emitted from the core collide with plasma particles, consisting of neutral atoms as well as charged particles like ions and electrons. During these collisions, energy is exchanged between the photons and the plasma particles. The density and temperature of the plasma decrease towards the outer boundary, resulting in numerous collisions. The high number of collisions in this zone can cause photons to take up to a million years to pass through, despite the decreasing plasma density and temperature.

Tachocline

The tachocline is a narrow region located between the radiative zone and the convective zone of the sun. It is within this thin layer that the magnetic field of the sun is formed. The plasma flows in this region pull the force lines of the electromagnetic field, causing the magnetic field to intensify. It is believed that the plasma undergoes significant changes in its structure within the tachocline.

Convective region

In the vicinity of the sun’s surface, the temperature and density of matter are not adequate for the efficient transport of the sun’s energy solely through re-radiation. Consequently, in this region, the plasma initiates a rotational motion, creating vortices that transfer energy to the surface. As one moves towards the outer boundary of the region, the temperature decreases and the gas density diminishes. Simultaneously, the particles in the photosphere directly above the convective region, having been cooled at the surface, enter into the convective zone.

Photosphere

The photosphere, also known as the solar surface, is the brightest part of the Sun that is visible from Earth. Although the Sun is made up of gas and does not have a solid surface, the photosphere is considered to be a part of its atmosphere.

Compared to the enormous radius of the star, which is approximately 700,000 kilometers, the photosphere is a relatively thin layer ranging from 100 to 400 kilometers in thickness.

This region is where light, kinetic energy, and thermal energy are emitted during solar activity. The lower plasma temperature in the photosphere, combined with intense magnetic radiation, is responsible for the formation of sunspots, which are known to cause solar flares.

Even though solar flares have a short duration, the amount of energy released during this time is extremely high. This energy manifests itself in various forms, such as charged particles, ultraviolet, optical, X-ray, or gamma rays, as well as plasma currents. On our planet, these plasma currents cause magnetic storms that have a negative impact on human health.

The gas in this region of the star is relatively sparse and rotates in an uneven manner. Near the equator, it takes 24 days for a complete turnover, while at the poles it takes thirty days. The upper layers of the photosphere have the lowest recorded temperatures, resulting in only one out of 10 thousand hydrogen atoms being charged ions. Despite this, even in this area, the plasma is sufficiently ionized.

Chromosphere

The chromosphere is the outermost layer of the Sun, extending up to 2 thousand kilometers. Within this region, temperatures rise dramatically and hydrogen and other elements become highly ionized. Due to its low density, the chromosphere is difficult to observe from Earth, but becomes visible during a solar eclipse when the Moon obscures the brighter photosphere, causing the chromosphere to emit a red glow.

The corona, which can be observed during a total solar eclipse, is the outermost layer of the Sun and is characterized by its intense heat and radiant halo-like appearance. However, due to its extremely low density and brightness, it is not visible at other times.

The Sun is composed of prominences, which are columns of glowing gas that can reach heights of up to 40,000 kilometers. It also experiences energetic eruptions that shoot out into space at high speeds, creating the solar wind. This solar wind consists of charged particles and is responsible for various natural phenomena on Earth, such as the northern lights. It is worth mentioning that the solar wind itself is highly dangerous, and if our planet did not have an atmosphere, it would pose a threat to all forms of life.

The Duration of One Earth Year

As our planet orbits around the Sun, it maintains a steady speed of approximately 30 km / s. The complete revolution takes one Earth year, during which the Earth covers a distance of over 930 million kilometers. The closest point between the Earth and the Sun is about 147 million kilometers, while the farthest point is approximately 152 million kilometers away.

Throughout the year, the apparent movement of the Sun as observed from Earth changes, following a trajectory that resembles a figure eight. This path stretches along the Earth’s axis from north to south, with a slope of forty-seven degrees.

During the summer months in the northern hemisphere, the Earth is tilted towards the Sun, resulting in the Sun’s rays hitting the surface of the Earth with maximum intensity. However, in winter, the Sun’s path in the sky is much lower, causing the Sun’s rays to hit the Earth at a sharper angle. As a result, the Earth is heated less effectively.

The average temperature is determined when autumn or spring arrives and the Sun is positioned equidistant from the poles. During this time, the length of both day and night is approximately equal, resulting in transitional climatic conditions between winter and summer on Earth.

These changes begin to occur in winter, following the winter solstice, when the Sun’s trajectory in the sky shifts and it starts to rise.

Consequently, as spring approaches, the Sun moves closer to the vernal equinox, causing the duration of day and night to become equal. On June 21, the summer solstice, the solar disk reaches its highest point above the horizon during summer.

Earth Day

When observing the sky as an Earth dweller seeking to understand why the Sun shines during the day and where it emerges, one will quickly notice that the Sun ascends in the east and sets in the west.

This is due to the fact that our planet not only orbits around the Sun, but also spins on its axis, completing a full rotation in 24 hours. From a space perspective, it can be observed that Earth, like most of the Sun’s planets, rotates counterclockwise, from west to east. However, when standing on Earth and observing the Sun’s appearance in the morning, everything appears in reverse, leading to the perception that the Sun rises in the east.

The Influence of the Sun on Earth

The relationship between the Sun and Earth is so interconnected that the significance of the largest star in the sky cannot be overstated. Primarily, our planet took shape around the Sun, leading to the emergence of life. Additionally, the Sun’s radiant energy provides warmth to the Earth, while its rays illuminate the planet, shaping its climate by cooling it at night and warming it again upon sunrise. Furthermore, the Sun plays a vital role in the development of Earth’s atmosphere, providing the necessary conditions for life to exist. Without the Sun’s rays, the atmosphere would resemble a liquid nitrogen ocean, surrounding frozen blocks of ice and land.

< p > Everything you need to know about the planet Mars 9327 4.79 7 7 < /p > < p > The Sun and the Moon, the Earth and the Sun, the air and water currents, the biomass that surrounds us, are readily accessible, renewable sources of energy that can be conveniently harnessed (they are located on the surface, requiring no extraction from the planet’s core, and do not produce radioactive or hazardous waste). < /p >

The International Day of the Sun was established in the mid-90s as a way to raise public awareness about the potential of renewable energy sources. Each year on May 3rd, various events including seminars, exhibitions, and conferences are held across Europe to demonstrate the positive impact of harnessing the power of the sun and educate people on how to accurately determine sunrise and sunset times.

For instance, during the Day of the Sun event, attendees have the opportunity to participate in unique multimedia presentations and observe massive magnetic disturbances and diverse displays of solar activity through a telescope. On this occasion, visitors can also witness a range of physical experiments and demonstrations that vividly showcase the immense power of our Sun as an energy source. It is not uncommon for visitors to have the chance to create their own sundial and put it to the test during the Day of the Sun event.

Greetings to all. I am here to share with you a fascinating tale about a unique service that allows you to:

* Locate a Google Street View spot near your place of residence and observe the sun’s journey across the sky throughout the year. This is done by taking into account the geographical coordinates and aligning them with your surroundings, such as buildings and vegetation (based on the data collected during the last visit of a Google car to your area);

* Virtually explore different parts of the world where Google StreetView coverage is available in order to study the sun’s movements. This includes observing the vertical sunrise and sunset in equatorial countries, the counterclockwise trajectory of the sun and inverted analemmas in the southern hemisphere, as well as experiencing polar nights and days, among other phenomena.

I didn’t prepare a detailed script this time, so the narration is more concise. Feel free to adjust the playback speed to 1.25 or higher.

14.9K posts 45.3K subscribers

Guidelines for the Community

What guidelines can be implemented here, apart from the guidelines established by peekaboo itself 🙂

Hold on, what has been altered? I have been familiar with this service for a couple of years now. And there is a video on the identical channel from “Oct. 31. 2015”

Is there really water on the Sun? What is the explanation for its existence?

The Sun, a massive ball of hydrogen-helium plasma, contains a variety of elements that are heated to extremely high temperatures. Surprisingly, water, an unexpected component, has been discovered on the Sun after years of intense scientific discussion.

Water can be found throughout the entire solar system. Some of the water molecules are even older than our own sun and all other celestial objects. They originated from a massive cloud of gas and dust, which eventually gave birth to the various entities we observe in our corner of outer space. Given that the Sun’s mass is over 99 times greater than the rest of the matter in our solar system, it’s not surprising that the Sun absorbed some of this moisture during its formation. The question now is whether these molecules managed to remain as water or if the intense heat of the Sun caused them to separate into hydrogen and oxygen.

The Sun’s surface has an average temperature of approximately 5500 degrees Celsius, which is quite high. However, it is important to note that the term “average” is used here for a reason. The Sun has dark spots on its surface, which appear darker in contrast to the lighter spots because they are cooler. These dark spots have a temperature of “only” 3,500 degrees Celsius. This temperature is still too hot for any form of biological life, but it is possible for water molecules to maintain their structure at this temperature.

Nonetheless, despite the theoretical possibility of vapor existing on a star’s surface, there is no concrete evidence confirming its actual presence. Scientists have persistently endeavored to establish its existence on the Sun, but their attempts have thus far been inconclusive. One possible method of verification is through spectroscopy, which involves analyzing the wavelengths of light emitted by the star. Each element emits a distinct signature, but the situation with water is slightly more intricate.

It may seem absurd and contrary to common sense, but it is indeed true that there is water on the surface of a scorching fireball. This seemingly amusing fact can have significant implications for the study of other star systems. For decades, astronomers have been analyzing the composition of exoplanet atmospheres by observing the spectrum when these celestial bodies pass in front of their star. Unsurprisingly, water has been the most sought-after element in these observations. However, the discovery of water must now come with a caveat, as it appears that steam can exist on the surface of the star itself.

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The arrangement of the movement of the celestial bodies in the solar system

A sophisticated depiction of the true nature of the universe.

What is the definition of plutoids?

Following the removal of Pluto from the list of planets, the International Astronomical Union sought to compensate for this change by introducing a new classification for trans-Neptunian objects that would be named after Pluto.

These objects, known as plutoids, include dwarf planets that orbit the Sun at a distance greater than Neptune’s orbit. They must also be in hydrostatic equilibrium and have not cleared their orbital path of other objects. Initially, the designation of plutoids was given to Pluto itself and Erida. Later, Makemake and Haumea were added to this group. Quavar, Sedna, and several other objects are currently being considered as potential plutoids.

Sun in Multispectral, August 1, 2023.

The image was captured using multiple telescopes, each equipped with narrow-band light filters that highlight specific wavelengths.
The H-alpha (656 nm) filter was used for the red channel,
the Continuum (540 nm) filter for the green channel,
and the CaK (393 nm) filter for the blue channel.
The complete list of equipment used, as well as high-quality images, can be found at this link.
The photograph was taken in the courtyard of Anapa.

Astrophotography of the Year: The Magnetic Field of the Sun

This photograph depicts the phenomenon of the magnetic field pulling in sections of the chromosphere following a significant flare. The magnetic field lines can be seen tracing along the surface of the sun in this particular instance.

Sunday, July 31st, 2023

The Chromosphere (at a wavelength of 656.28 nm):

At a wavelength of 540 nm, we can observe the photosphere of the Sun.

The photosphere of the sun can be observed at a wavelength of 393.3 nm.

Extra: Observe the Sun’s movement between July 26 and 31

July 30, 2023, Sunday

The Chromosphere (at a wavelength of 656.28 nm):

The layer of the sun known as the photosphere, which emits light at a wavelength of 540 nanometers, is captured in this stunning image.

Sunday, July 29th, 2023, 10:25 in the morning

Equipment:
-Telescope Celestron 102 SLT
-Mount Celestron Nexstar SE
-Lacerta wedge by Herschel
-Light filter Baader Solar Continuum (540 nm wavelength, in the green region of the spectrum)
-ND3 light filter
-ZWO ASI 183MC astronomical camera.
Click here to view the image in full size.
Location: Yard in Anapa.

Sunday, July 27th, 2023

Chromosphere (wavelength 656.28 nm):

The Sun’s photosphere (at a wavelength of 540 nm):

Photosphere (wavelength 393.3 nm):

Sunday, July 26th, 2023

The chromosphere (at a wavelength of 656.28 nm):

The photosphere of the sun can be observed at a wavelength of 540 nm.

The photosphere, with a wavelength of 393.3 nm, is captured in this image:

A breathtaking image of the analemma

Analemma – The path that the sun traces in the sky over the course of a year when its position is recorded at the same time every day.

Earth and Mars

The planets Earth and Mars are fascinating celestial bodies in our solar system. Earth is the third planet from the Sun, while Mars is the fourth. Both planets have distinct characteristics and are of great interest to scientists and space enthusiasts.

Earth is often referred to as the “Blue Planet” due to its abundant water resources and the presence of life. It is the only known planet to support life, with a diverse range of ecosystems and a breathable atmosphere. Earth has a solid surface and is composed of various layers, including the crust, mantle, and core. It has a moderate climate that allows for the existence of liquid water, making it a suitable home for a wide variety of organisms.

On the other hand, Mars is often referred to as the “Red Planet” due to its reddish appearance. It is a rocky planet with a thin atmosphere, composed mainly of carbon dioxide. Mars has a colder and drier climate compared to Earth, with a surface covered in dust and rocky terrain. Despite these harsh conditions, scientists have discovered evidence of liquid water in the past and believe that Mars may have once supported life.

Both Earth and Mars have similarities in terms of their geological features. They both have volcanoes, mountains, and valleys, although the scale and size vary significantly. Earth has the highest mountain, Mount Everest, while Mars has Olympus Mons, the largest volcano in the solar system. Both planets also have polar ice caps, although Mars’ ice caps are primarily composed of frozen carbon dioxide.

In terms of exploration, Earth has been extensively studied and explored by humans. Mars, on the other hand, has been the subject of numerous space missions and robotic explorations. These missions have provided valuable data and insights into the planet’s geology, atmosphere, and potential for supporting life.

In conclusion, Earth and Mars are two captivating planets with distinct characteristics and features. While Earth is known for its abundance of life and diverse ecosystems, Mars is a barren planet with potential evidence of a past habitable environment. Further exploration and research will continue to deepen our understanding of these two fascinating celestial bodies.

The Kallanish stones provide a stunning backdrop for the Sun’s analemma.

An analemma is the path that the Sun traces in the sky throughout the year, as its position is recorded at the same time every day.

The Callanish Stones, which are approximately 5,000 years old, are Scotland’s most renowned prehistoric site. While their exact purpose remains a mystery, many believe that they served as an ancient astronomical observatory or calendar.

During the summer solstice, the Sun reaches its highest point in the elongated figure-eight shape of the analemma, while during the winter solstice, it occupies the lowest point.

The unique shape of the analemma is determined by the Earth’s orbit being elliptical and the planet’s axis of rotation being inclined to it.

As a result, the analemma on Mars would have a completely different appearance, resembling a drop rather than a figure eight.

This photo was captured by the Mars Pathfinder probe in 1997.

The constellation Orion is located in which galaxy?

Hello everyone. Yesterday, someone posted a photo of an analemma (the sun’s path across the sky, if recorded at the same time of day during the year) in an unidentified location.

I have come across this image before, and it didn’t raise any doubts in my mind because it appeared to be authentic. Therefore, I didn’t feel the need to investigate further. However, there has been recent speculation about its authenticity, with some suggesting that it may be a manipulated or photoshopped image. As a result, I was drawn to this post and decided to conduct a small investigation.

To begin with, I utilized a Google search to trace the origin of the image. It turns out that the photo was taken by a Hungarian photographer named György Soponyai and was originally posted on Flickr:

The next question arises as to whether the 8-hour analemma is too high and completely visible above the horizon. This is a valid inquiry because, for instance, in Moscow around New Year’s Day at 8 o’clock, the sun has not yet risen, it only rises at 9 o’clock.

All these variations in hours are typically explained by the time zone and the specific location of the point in relation to the middle of the time zone. Let’s examine the situation in this particular case.

Considering that we are discussing a major European city, it immediately occurred to me that it might be possible to find an actual landscape captured by the Google car (Google Street View service), and thus, we could observe the real location of analogs here.

As they say, “Done and done.” First, I located the desired point in Google Maps, inputted its coordinates into daybit.ru/sun, and observed the following:

When comparing this photograph to the original one, it becomes evident that there is only one possible candidate for the desired analemma depicted here. The top portion of the analemma (representing June 22) aligns with the same building as in the initial photo, while the bottom portion (representing December 22) is positioned just above the bridge, slightly to the right of the first lantern. The previous analemma (on the left) is already partially below the horizon, while the next one (on the right) is positioned too high.

The only thing left is to comprehend the reason behind its designation as 8 o’clock. To achieve this, Budapest must be situated in the UTC+1 time zone. As it turns out, during winter time (standard time), Budapest follows UTC+1, while during summer time it follows UTC+2 (thus, the summer portion of this analemma corresponds to 09:00). Interestingly, the European Union appears to be on the verge of eliminating the seasonal adjustment of clocks, leaving us uncertain about what time this analemma will be referred to in Hungary in the future.

In conclusion, the mini-investigation has verified that the Budapest analemma is indeed accurate, and I have created a separate post since the google-maps calculation coincided with the original source – I felt compelled to share this magnificence with all of you. )

Snapshot of the analemma

The analemma represents the trajectory that the sun traces throughout the year when its position is fixed at a specific time.

Sun clock

Greetings to all. Since I created a video discussing the movement of the sun across the sky, I have been planning to write a comprehensive article about sundials. Finally, after three years, I am able to fulfill this plan.

In this piece, I have diligently compiled all the essential information I have gathered about sundials in over a decade:

* I will reference the analemma belt mentioned in my previous video, as every sundial is a projection of this belt;

* I will cover the main types of sundials: scaphis, horizontal sundials, analemmatic (which are based on the principles of equatorial sundials), vertical, and equatorial sundials;

* I will discuss the spatial orientation of the gnomon (the “stick” that casts a shadow);

* Can a vertical pole be utilized as a gnomon, and what would be the potential inaccuracies?

* How can a basic horizontal sundial be constructed (e.g., in your country house)?

* What inaccuracies arise when measuring time with a sundial: their source and extent.

Certain concepts in the video are briefly mentioned without verbal explanations, so feel free to pause the video to examine the text and markup on the slide.

Analemma for Google Earth

This brief video demonstrates how you can calculate the sun’s position anywhere on the planet at any given date and time using the pre-calculated analemma for Google Earth (kml-file). In other words, it’s almost like a manual process. This video is a continuation of the previous one titled “Sun Altitude Isolines” which can be found at https://pikabu.ru/story/izolinii_vyisotyi_solntsa_razyasnyay.

Having watched the video myself, I felt that the content was quite condensed and could benefit from a more serene and meditative approach. I welcome any feedback. )

The inaugural image of the analemma, 1979

The analemma is the path that the sun traces throughout the year, when observed at a fixed time (excluding the seasonal shift).

It all began with a conversation about a renowned photograph of the analemma:

In addition to the dots, there are three lines present in the photograph. Two of these lines correspond to the solstice days – the shorter line represents the winter solstice, while the longer line represents the summer solstice. The middle line, however, is considered to be “erroneous” as it is believed to represent the equinox, but it does not. Upon closer examination, it is evident that the crossing point in the analemma is positioned “above” the equinox days [1]. To ensure the accuracy of the photo’s description, I sought out the original source. I am pleased to confirm that I have found it and have verified its authenticity [2].

An article was published in the June 1979 issue of Sky & Telescope discussing the analemma. The author, Dennis di Cicco, shared his experience with the technical aspects of this phenomenon.

As someone who personally developed a program to determine the Sun’s position in the mid-2000s, I found the following excerpt quite intriguing:

By acquiring a programmable calculator (a Hewlett-Packard HP-67), I was able to write multiple programs. These programs utilized the direct sunrise and declination data from various dates to calculate the observation’s altitude and azimuth from a specific window. This allowed for an accurate depiction of the analemma’s appearance, considering the presence of trees and buildings to the east.

Curiosity got the better of me, and I decided to explore this impressive piece of technology from the 70s:

In the article, the writer details his experience with a digital alarm clock that he spent a total of three months modifying to incorporate an automatic shutter release mechanism.

Initially, the author’s first attempt, which took place between February 1977 and February 1978, was unsuccessful due to an error in the camera’s tilt. As a result, the upper portion of the analemma was not captured within the frame as intended:

A second photograph had to be captured over the course of a year, spanning from 1978 to 1979. Each week, a picture was taken, with the exception of days with unfavorable weather conditions, in which case the photograph was taken on the following day. The precise time for each shot was determined using the WWV radio station, a shortwave radio station that began operating in America in 1920 and emitted highly accurate time signals. All of the photographs were taken automatically, and half of them were taken when no individuals were present at the location.

The elongated lines in the photograph were captured using a solar filter with a density of 6.0. This filter was specifically designed so that the film would not be overexposed during the approximately two-minute period in which the solar disk shifted by its own diameter.

The subsequent content provides a distinct depiction of the central axis, which is the basis for my ongoing investigation. In the article, the writer asserts that this axis, which corresponds to the intersection point of the figure-eight analemma, ought to have been captured in either mid-April or late August. [3] The writer hypothesized that if the capture had been made in April, when the tree had not yet developed dense foliage, the photograph would have depicted the sun appearing to pass in front of the tree. It is worth noting that the winter axis (the shortest one, on the right) bears a striking resemblance to this scenario.

The background image was taken in September, when the sun was positioned outside of the frame (as evidenced by the shadow cast by the pipe). The neutral filter was swapped with a polarizing filter in order to intensify the darkness of the sky.

The weather always seemed to be attempting to ruin things, especially in January 1979 when it was very overcast. However, we were fortunate. Additionally, during the winter, I had to use a hair dryer to thaw the frozen windowpane behind which the camera was positioned.

There was another issue – power outages. These outages could have caused the timer to malfunction, resulting in either not working at all or taking the picture at an unplanned time. One such power failure occurred in May 1978, and there was no way to confirm if the picture turned out fine. The author made the decision to proceed. From what I understand, some “extra” sunlight outside of the analemma had to be retouched.

The diagram below displays the important dates:

All photographs of the sun were captured at 0830 EST.

Lastly, an image that illustrates the reason behind the unique appearance of the morning analemma to an observer: