- Elongation (from the Late Latin word elongatio, meaning “moving away”) is a term used in astronomy that has multiple definitions.
Related concepts
The pole of the ecliptic refers to a point on the celestial sphere that intersects with the perpendicular to the ecliptic plane. It serves as the pole for the ecliptic system of celestial coordinates.
Opposition, also known as opposition, is a position of a celestial body in the solar system where the difference between its ecliptic longitude and the Sun’s longitude is 180 degrees. In other words, this body is located along the “Sun – Earth” line and can be observed from Earth in the opposite direction from the Sun. Opposition can only occur for planets and other bodies that are farther away from the Sun than Earth.
A contrail is a faint blurry light spot that can be seen in the night sky. Typically, it appears as a diffuse light spot with a diameter of around 10 degrees in the ecliptic plane, and it is visible from the opposite side of the Sun (at an elongation of 180 degrees).
Extraterrestrial skies refer to the view of space from the surface of a celestial body other than Earth. This view can differ from what we observe from Earth’s surface due to various factors. One of the most significant factors is the composition and density of the atmosphere on the celestial body. The color of the sky can vary based on these factors, and the presence or absence of clouds. Additionally, other astronomical objects like stars, satellites, planets, and rings may also be visible from the surface of the celestial body.
References in literature
Asteroids of the Atira type ((163693) Atira) have been mentioned in various literary works. These asteroids have orbits that are completely contained within the Earth’s orbit. They are often observed at elongations from the Sun that do not exceed 90 degrees. Currently, only two confirmed Atira-type asteroids have been officially numbered.
Similarly, the mistakes in the theory of Venus have been corrected by an extra sphere. If P1P2 = 45°, the maximum elongation is 47°40?, which is very close to the accurate value. Additionally, the varying speed of the planet in the four parts of the synodic orbit is also explained. In the diagram shown above, it can be observed that the transition from one triple point to another takes up one quarter of the period, while the reverse transition takes another quarter. The remaining time is occupied by the slow movement through the small loops at the end of the diagram. Regarding Mercury, the theory proposed by Eudoxus was already quite accurate, and the introduction of an extra sphere only served to enhance it.
If we look at the molecular origins of the tree of life, we find that the oldest organisms are thermophilic archaea – prokaryotes that inhabit hot springs, often with high levels of acidity. (By the way, “archaea” and “archaea” are homonyms, highlighting the ancient nature of the concepts they represent.) Methane-producing archaea, which are closely related, also thrive in temperatures ranging from 40-85 °C, and their methane production increases as the temperature rises. Additionally, the reconstructed ancestral proteins from the elongation factor group, which play a role in sequentially attaching amino acids to the protein being synthesized on the organelle-ribosome (in other words, elongating the protein molecule), are capable of withstanding high temperatures (45-80 °C and even exceeding 80 °C). Since both bacteria and archaea possess these components, it is likely that they inherited them from a common Early Archean ancestor, which had a heat-resistant elongation protein.
Further related concepts
Orbital intersection point – one of the two points where a celestial body’s orbit intersects a reference plane, such as the ecliptic plane for the planets of the solar system and the Moon. These points are also known as orbital nodes. In the equatorial coordinate system, these points are projected onto the celestial sphere, allowing for easier tracking of celestial objects. Due to the presence of two orbital intersection points, a distinction is made between ascending and descending nodes.
Stellar time, denoted as s, represents the angular distance of the vernal equinox. Astronomers rely on star time to determine the specific direction to point the telescope for observing a desired celestial object.
Astronomical refraction, also known as atmospheric refraction, refers to the bending of light rays from celestial bodies as they pass through the Earth’s atmosphere, leading to a change in their apparent position in the sky.
Synodic Circumference Period, derived from the Greek word “σύνοδος” meaning conjunction, represents the time duration between two consecutive conjunctions of the Moon or any planet in the solar system with the Sun, as observed from Earth. The conjunctions of the planets with the Sun must occur in a specific linear order, which is particularly important for the inner planets. For instance, consecutive upper conjunctions occur when a planet passes behind the Sun.
The tilt of the axis of rotation refers to the angle at which the axis of rotation of a celestial body deviates from being perpendicular to the plane of its orbit. Essentially, it is the angle between the equator of the celestial body and its orbit.
Nereid, which was discovered by Gerard Kuiper on May 1, 1949, is a moon of Neptune. It is named after the Nereids, who were sea nymphs in Greek mythology. Nereid has a diameter of 340 kilometers and it is the third largest moon of Neptune. Its orbit has one of the highest eccentricities among the moons in the solar system (0.75), which means that its distance from Neptune varies between 1.4 million km and 9.6 million km, with an average distance of 5.5 million kilometers. The significant eccentricity of its orbit has led to speculation that Nereid may actually be an asteroid.
The phases of Venus are the different changes in brightness that can be seen on the surface of the planet, similar to the phases of the Moon. Galileo Galilei was the first to observe these changes in 1610. While Venus had been seen with the naked eye before, there was no definitive historical record of its phases until the invention of the telescope.
Near-solar comets, also known as sun-struck comets or sungrazers, are comets that come very close to the Sun at their closest point, known as perihelion. Some of these comets come within just a few thousand kilometers of the Sun’s surface. Smaller near-solar comets may completely vaporize during this close approach, while larger comets can survive multiple perihelion passes. However, the intense vaporization and tidal forces often cause the comet to disintegrate.
The Earth Similarity Index (ESI) is a measure of the potential habitability of a planet or moon. It was developed by a team of international scientists including astronomers, planetologists, biologists, and chemists.
A co-orbital orbit is one of the six types of orbits that asteroids and small celestial bodies (SCs) can have around the Sun in relation to the planets of our solar system. In the diagram above, you can see this type of orbit depicted in the top right corner. The orange dot represents the Sun, and the thick yellow circle represents the orbit of a planet, with its closest and farthest points from the Sun marked by the perihelion and aphelion. An asteroid following a co-orbital orbit closely follows the same path as a planet, neither getting closer nor moving further away from it. Examples of groups of asteroids that exhibit this type of orbit include the Trojans and the Greeks.
A transit, also known as an astronomical transit, refers to a fascinating phenomenon in astronomy where one celestial body passes in front of another celestial body, resulting in the obstruction of a portion of the latter body. This event can be observed from a specific vantage point.
The Roche limit signifies the radius of a satellite’s circular orbit around a celestial body. At this particular distance, the gravitational forces exerted by the central body and the satellite’s self-gravity become equal, giving rise to tidal forces.
Analemma, derived from the Greek term “ανάλημμα” meaning “basis” or “foundation,” represents a curve that connects successive positions of the central star within a planetary system (such as the Sun in our case) in the sky of a specific planet. These positions occur at the same time of day throughout the year.
Radiant (from the Latin word radians, genitive Latin radiantis – radiating) is a region on the celestial sphere that appears to be the origin of meteors, which are observed when the Earth intersects a group of meteoric bodies that are moving in a shared orbit around the Sun.
The Local Interstellar Cloud (LIC) is a cloud of interstellar matter (about 30 light-years in size) that the Solar System is currently traversing.
A multiple orbit planet is an exoplanet that does not orbit a single star, like Earth orbits the Sun, but instead orbits around two or more stars. The planet’s path is determined by the gravitational pull of all the stars it orbits. As of January 23, 2012, there have been twelve confirmed cases of multiple orbital planets, including PSR B1620-26, HW Virgo, Kepler-16, Kepler-34, Kepler-35, Ross 458, NY Virgo, UZ Furnace, RR Rex, HU Aquarius, DP Leo, and NN Snake.
A plutoid is a type of dwarf planet found in our solar system. Plutoids are celestial bodies that.
An occultation is an astronomical event where one celestial body passes in front of another from the perspective of an observer, causing part of the celestial body to be obscured.
The Minor Planet Center has introduced the uncertainty parameter U to provide a quantitative measure of the uncertainty associated with the calculated perturbed orbit for a minor planet. This parameter is represented on a logarithmic scale ranging from 0 to 9, indicating the uncertainty arc of the average anomaly of a minor planet after 10 years of orbital observation. On the JPL Small-Body Database Browser website, the uncertainty parameter is also referred to as the condition code. However, it is advised not to rely solely on the U value.
The Hill sphere is positioned between the Lagrangian points L1 and L2, which are situated along the line connecting the centers of the two celestial bodies. In this particular direction, the gravitational influence exerted by the smaller body is at its minimum, resulting in a limitation on the size of the Hill sphere. Beyond this distance, the orbit of any additional body revolving around the smaller body will extend partially outside the Hill sphere, leading to an increasing disruption caused by the tidal forces exerted by the larger central body. Ultimately, the smaller body will lose control over the additional body’s orbit.
A comet’s tail is a elongated plume consisting of dust and gas emitted from cometary matter. It forms as the comet approaches the Sun and becomes visible due to the scattering of sunlight upon it. The tail is typically oriented away from the Sun.
The Kreutz comets are a group of comets that orbit near the Sun and are named after astronomer Heinrich Kreutz, who first discovered their connection. It is believed that these comets are fragments of a larger comet that broke apart several centuries ago.
The Pole of the World refers to a specific point on the celestial sphere where the stars appear to move in a daily motion due to the Earth’s rotation on its axis. The North Pole of the World aligns with the geographical north and is located in the constellation of the Little Bear, with Polaris as its closest star. The South Pole of the World aligns with the geographical south and is located in the constellation Octanthus. Over time, the Earth’s axis undergoes a precession, causing the poles of the world to shift by approximately 20″ per year.
The osculating orbit of an object in space (at a given moment of time) is a gravitational Keplerian orbit, such as an ellipse or another section of a cone, relative to a central body. This orbit represents the path that the object would follow in the absence of any further perturbations, such as those caused by the nonsphericity of the central body, the gravitational influence of third bodies, or non-gravitational forces.
The galactic plane is the plane in which the majority of the mass of a disk galaxy is concentrated. The directions perpendicular to the galactic plane indicate the poles of the galaxy. The terms “galactic plane” and “galaxy poles” are commonly used to describe the plane and poles of the Milky Way.
Synchronous rotation, also known as tidal capture, refers to the phenomenon where a satellite’s rotational period around its axis matches its orbital period around the central body. This results in the satellite always facing the central body on the same side, as it completes one rotation around its axis in the same amount of time it takes to orbit around its partner. Tidal entrapment occurs during mutual motion and is commonly observed in large natural satellites of planets in the solar system.
Planetary equilibrium temperature, on the other hand, is a theoretical concept that represents the temperature a planet would have if it were a completely black body solely heated by the star it orbits. This model does not take into account the presence or absence of an atmosphere, including the greenhouse effect. Instead, it considers the theoretical temperature radiated from the planet’s surface, assuming it behaves as a black body.
The coordinate system of the ecliptic, also known as ecliptic coordinates:49, is a celestial coordinate system where the ecliptic plane serves as the main plane and the ecliptic pole serves as the pole. This system is utilized in studying the movement of celestial bodies within the solar system, particularly the orbital planes of those bodies that are known to be in close proximity to the ecliptic plane. It is also used in observing the apparent motion of the Sun across the sky throughout the year:30.
A hot Neptune is a type of exoplanet that falls within the category of planets with masses similar to Uranus or Neptune, and are located in close proximity to their respective stars (always at a distance less than 1 astronomical unit). A hot Neptune consists of a core and a dense atmosphere that surrounds it, occupying the majority of the planet’s overall size.
Planemo (short for planetary mass object) refers to astronomical entities that have a mass that meets the criteria for being classified as a “planet” – that is, they are larger than asteroids but smaller than nuclear-active brown dwarfs or other stars. This term was coined to describe objects that do not fit the traditional definition of planets.
The repetitive (retrograde) movement of planets is the observed motion of planets against the backdrop of stars in the celestial sphere. This motion appears to be from east to west, which is opposite to the motion of the Sun (annual) and the Moon.
The Earth’s orbit is the path that the Earth follows as it orbits around the Sun. It has an average distance of approximately 149.6 million kilometers (152.1 million km at aphelion; 147.09 million km at perihelion).
The limb (derived from the Latin word “limbus” meaning boundary, edge, limit) refers to the visible edge of the disk of the Moon, Sun, or planet as projected onto the celestial sphere.
A solar day is defined as the period of time during which a celestial body completes one rotation around its axis with respect to the center of the Sun. More precisely, it is the time interval between two consecutive culminations (passages through the meridian) of the Sun’s center, either upper or lower, in a specific location on Earth (or any other celestial body).
The Goldfish (Latin name Doradus) is a constellation located in the southern hemisphere of the celestial sphere. It covers an expansive area of 179.2 square degrees and is visible to the naked eye thanks to its 32 prominent stars.
The main belt comets are celestial objects that orbit the Sun within the main asteroid belt and display comet-like activity during specific portions of their orbit.
The snow line, a term utilized in astronomy and planetology, signifies the distance from a star at which temperatures drop sufficiently for volatile compounds like water, ammonia, methane, molecular nitrogen, and chlorine to solidify within a protoplanetary system.
Sub-brown dwarfs, also known as brown subdwarfs, are celestial objects that have a mass below the threshold of brown dwarfs. These formations, which are often considered as planets, have a mass less than 0.012 solar masses or approximately 12.57 Jupiter masses, although there is no defined lower limit. Interestingly, sub-brown dwarfs form in a manner similar to stars, through the collapse of a gas cloud, rather than through the accretion or core collapse of circumstellar disk material like planets. This scientific phenomenon showcases the fascinating diversity of celestial bodies in our universe.
In other news, on May 29th, we can observe Mercury at its greatest westerly elongation. For those who are interested in the happenings of the sky, this is an exciting event to look out for. While it may not directly impact our earthly lives, it offers a glimpse into the wonders of the cosmos and serves as a reminder of the vastness and beauty of our universe.
1. What does the term “elongation” mean?
Elongation refers to the apparent distance of a planet, comet, or asteroid from the Sun in the Earth’s sky. Another way to define it is the angle between the directions to the centers of two celestial bodies as observed from Earth.
During opposition, a planet’s elongation approaches 180°, although it rarely reaches this value. This is because planetary orbits are inclined to the ecliptic, making it rare for the Earth to be exactly aligned in a straight line between the planet and the Sun. Conversely, when a celestial body passes in front of the solar disk, its elongation approaches zero.
2. What is the significance of Mercury’s elongation?
Elongation is a measure that can be applied to any planet in the solar system at any given moment. However, it is primarily discussed in relation to Venus and Mercury. These two planets are unique in that they can be observed against the backdrop of our Sun and are never positioned more than a certain angular distance away from it, determined by the size of their orbits.
Mercury, with its small orbit, spends a significant portion of time being too close to the Sun to be easily seen through a telescope. This is why the period of maximum elongation is considered the ideal time to observe it.
3. What are the distinctions between eastern and western elongation?
The disparities between eastern and western elongation are precisely as their names imply. During western elongation, the planet is positioned to the west of the Sun, whereas during eastern elongation, it is moving away from the Sun to the east.
Moreover, in the case of Mercury and Venus, this distinction also determines their visibility. During eastern elongation, they can be observed in the evening shortly after sunset, approximately above the location where the Sun has just set. On the other hand, during western elongation, you should search for them early in the morning, above the part of the horizon where the Sun is expected to rise.
On May 29, there will be a significant event happening with Mercury – it will reach its maximum westerly elongation. This means that it will be in the best position for observation. However, it’s important to keep in mind that planets generally move close to the ecliptic, and currently, Mercury is positioned in a way that it rises very slowly in the morning from the Sunrise point in the southern direction. As a result, even though Mercury is west of the Sun, it will only appear above the horizon a few minutes before sunrise, making it extremely challenging to see.
In our latitudes, it is also challenging to observe Mercury’s eastern elongations in the fall, especially when the “low” zodiacal constellations like Scorpio and Sagittarius are at their highest point in the evenings. However, the spring evening elongation of Mercury, which occurred on April 11, was more convenient for observations. Even though the angular distance between Mercury and the Sun was just over 19 degrees, it still provided a good opportunity to observe the smallest planet.
5. How will the maximum elongation of Mercury impact events on Earth?
Mercury completes one orbit around the Sun in just 88 Earth days, allowing it to reach its maximum elongation – both east and west – up to seven times per year. This occurrence, however, is not considered unique.
The maximum elongation of Mercury does not make it special or bring it closer to Earth or the Sun. It is merely a specific alignment of the three celestial bodies. As a result, there is no need to be concerned about any potential influence on earthly events.
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I am a news editor and an author of articles. For the past 10 years, I have been dedicated to popularizing science in Ukrainian. I hold a degree in Technical Sciences and have previously taught civil engineers. However, in recent years, my focus has shifted towards educating the general public about various scientific topics. One subject that has always held a special place in my heart is space. Throughout my work, I strive to uphold the principle of honoring the scientists behind significant discoveries and the engineers responsible for developing space technology.
ELONGATION – (Latin elongatio, “removal”) – the maximum distance from the Sun that the lower planets (Mercury and Venus) reach as observed from Earth: when they reach their eastern elongation (their longitude is greater than that of the Sun), they switch from direct motion to retrograde (see), and when they reach their western elongation (the Sun’s longitude is greater than that of the planet), they return to direct motion. The maximum elongation of Mercury is approximately 28, and Venus is approximately 48.
Discover the definition of ELONGATION in various dictionaries:
ELONGATION
In the Dictionary of Synonyms ASIS.V.N. Trishin.2013, elongation is described as a noun with one synonym, which is distance (34).
ELONGATION
In French, ELONGATION has two meanings. Firstly, it refers to the furthest point on an arc that a pendulum can reach during its oscillations. Secondly, in astronomy, it represents the angle that measures the distance between a planet and the sun.
ELONGATION is the apparent angular distance of a planet from the Sun. If the elongation is equal to zero, the planet is said to be in conjunction with the Sun. The conjunction is referred to as a conjunction.
Definition of ELONGATION
Elongation, also known as g. élongation f. in French and Elongation in German, is derived from the Latin word ex of and longus long. In astronomy, it refers to the apparent angular distance of a planet from the Sun. According to the International Scientific Vocabulary (SIS) in 1954, elongation is defined as watch.
ELONGATION
1) The spelling of the word: elongation2) The emphasis in the word: elongation3) The division of the word into syllables (word transposition): elongation4) The phonetic transcription: watch
ELONGATION
Elongation refers to a stage in the biosynthesis of nucleic acid molecules (during transcription) or proteins (during translation).
It can also refer to the position of a star culminating between the world pole and the zenith when its azimuth is at its greatest or least. Planetary elongation is the position of a lower planet (Mercury or Venus) at the moment when its ecliptic longitude differs maximally from the longitude of the Sun (angular distance of the planet from the Sun). Synonyms for elongation include distance. Watch.
ELONGATION
g.; astr.elongation- eastern elongation- western elongation- elongation of an astronomical object- elongation of a star- elongation of a planet.
ELONGATION
Elongation (derived from the Latin word “elongatio” meaning removal) refers to the position of a star when it is maximally distant in azimuth from the southern point, culminating between the celestial pole and the zenith. The term also applies to the position of a lower planet (Mercury or Venus) when its ecliptic longitude differs the most from that of the Sun.
ELONGATION
Iol Inya Inga Inga Ilona Igo Igla Elongation Eon Gon Goacin Glina Gaoliang Aon England Alin Ail Agonia Agonia Yana Aloe Ala Anglo Anya Galo Galo Golia Gol Golica Gonia Gal Yaga. watch
ELONGATION
The term “elongation” refers to the position of a star when it is at its maximum distance in azimuth from the point of south, culminating between the pole of the world and the zenith. When it comes to planets, elongation refers to the position of a lower planet (such as Mercury or Venus) when its ecliptic longitude is maximally different from that of the Sun.
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ELONGATION
The emphasis is on the word: elongation. The stress falls on the letter: a. Undeleted vowels in the word: elongation.
ELONGATION
– (derived from Late Latin elongatio – removal) – the position of a star (reaching its highest point between the celestial pole and the zenith) when it is farthest in azimuth from the southern point. Elongation of a planet refers to the position of a lower planet (such as Mercury or Venus) when its ecliptic longitude is maximally different from the Sun’s longitude. observe
ELONGATION
The elongation refers to the elongation of a pendulum or a planet in the field of astronomy.
ELONGATION
It is a noun that is used in the feminine gender and in the singular form. In the field of astronomy, elongation is a term that is commonly used.
ELONGATION
In terms of measurement, elongation can be expressed as distance. It is measured in units such as R, D, and Pr.
ELONGATION
Elongation, derived from the Latin word “e(x) of + longus longus,” has two main definitions in astronomy. Firstly, it refers to the apparent angular distance of a planet from the sun. Secondly, it is the greatest distance from the meridian plane for a circumpolar star.
ELONGATION
Elongation is the act of lengthening something. It can refer to physical objects, such as elongating a piece of fabric or stretching a rubber band. It can also refer to abstract concepts, such as elongating a conversation or prolonging a process. Elongation is a word that can be used in various contexts and has multiple meanings. When we elongate something, we are making it longer or extending its duration. So, whether it’s elongating a piece of material or elongating a discussion, the concept of elongation involves stretching or lengthening to some degree.
ELONGATION
elongation, -iSynonyms: distance
EXTENSION
extension, -iSynonyms: distance
LONGITUDINAL STRETCH
〔名词〕 elongation rateSynonyms: distance
STRETCH
stretch g.elongationSynonyms: distance
LENGTHENING
EXPANSION
Initial form – Elongation, singular, feminine, nominative case, inanimate.
ELONGATION
In astronomy and physics, elongation refers to the angular separation between a celestial object and the Sun, as observed from Earth. There are two types of elongation: eastern elongation and western elongation. Synonyms for elongation include distance and separation.
Related terms
The pole of the ecliptic is a point on the celestial sphere where the perpendicular to the ecliptic plane intersects. It is a key component of the ecliptic system of celestial coordinates.
A contrail, also known as a condensation trail, is a faint blurred light spot visible in the night sky. It typically appears as a diffuse light spot with a diameter of approximately 10 degrees in the ecliptic plane. Contrails are observed from the opposite side of the Sun, which corresponds to an elongation of 180 degrees.
Extraterrestrial Skies – The view of the cosmos from the surface of a celestial body other than Earth. This perspective can differ from what is observed from Earth’s surface due to various factors. The primary determinant is the atmosphere of the celestial body, or lack thereof. The hue of the sky is influenced by the density and chemical makeup of the atmosphere. The presence and color of clouds can also vary. Additionally, other celestial objects visible from the surface, such as stars, satellites, planets, and rings, can contribute to the overall view.
In the realm of celestial mechanics, the Lidov or Lidov-Kozai mechanism, effect, or resonance pertains to the periodic alteration of the eccentricity and inclination ratio of an orbit under the gravitational influence of one or more massive bodies. The pericenter argument experiences libration, oscillating around a constant value.
Atira asteroids (also known as (163693) Atira) are a unique type of asteroids. These asteroids have orbits that are completely contained within the orbit of Earth. They can be found at elongations from the Sun that do not exceed 90 degrees. Currently, there are only two confirmed Atira asteroids that have been officially numbered.
Moreover, the Venus theory has been rectified by an additional sphere, effectively eliminating any errors. In cases where P1P2 is equal to 45 degrees, the maximum elongation reaches 47 degrees and 40 minutes, which is remarkably close to the actual value. This additional sphere also accounts for the varying speed of the planet during the four stages of its synodic orbit. As depicted in the above curve, the transition from one triple point to another consumes one-quarter of the entire period, while the reverse transition occupies another quarter. The remaining time is dedicated to the slow movement through the small loops at the curve’s end. Regarding Mercury, Eudoxus’ theory was already fairly accurate, and the inclusion of an extra sphere only served to enhance its precision.
Additional related concepts
Orbital crossing point – one of the two opposite points on the celestial sphere where the path of a celestial object intersects with a predetermined plane serving as a frame of reference. This point is also projected onto the celestial sphere in a geocentric manner. For the planets and the Moon within the solar system, this plane is known as the ecliptic plane. The equatorial coordinate system, along with the celestial equator plane, is commonly used to track ISSs. As there are two of these points, a distinction is made between them.
The motions of the Sun and planets in the sky only show their visible movements, which are apparent to observers on Earth. It is important to note that these movements on the celestial sphere are not directly related to the Earth’s daily rotation, as the rotation of the celestial sphere itself replicates this motion.
Astronomical refraction, also known as atmospheric refraction, refers to the bending of light rays from celestial luminaries as they pass through Earth’s atmosphere. This bending causes a change in their apparent position in the sky.
The tilt of the axis of rotation refers to the deviation angle of a celestial body’s rotation axis from the perpendicular to the plane of its orbit. In simpler terms, it is the angle between the equator plane of the celestial body and its orbit.
Nereid, which comes from Greek mythology and means “sea nymphs,” is a moon that orbits Neptune. It was discovered by Gerard Kuiper on May 1, 1949. With a diameter of 340 km, Nereid is the third largest moon of Neptune. Its orbit has one of the highest eccentricities among all moons in the solar system, measuring at 0.75. Its distance from Neptune ranges from 1.4 million km to 9.6 million km, with an average of 5.5 million kilometers. The significant eccentricity of its orbit suggests that Nereid may have originated from an asteroid.
The phases of Venus are the different changes in brightness that can be seen on the surface of the planet, similar to the phases of the Moon. The first recorded observations of the phases of Venus were made by Galileo Galilei in 1610. Venus had been observed many times without the aid of a telescope, but there was no definitive historical record of its phases until the invention of the telescope.
Near-solar comets, also known as sun-struck comets or sungrazing comets, are comets that come very close to the Sun at perihelion, sometimes getting as close as a few thousand kilometers from its surface. Smaller near-solar comets may completely vaporize during this close approach to the Sun, while larger comets may survive multiple perihelion passes. However, the intense vaporization of the comet’s nucleus and the tidal forces often cause the comet to disintegrate.
The Earth Similarity Index (ESI) was created by a team of international scientists including astronomers, planetologists, biologists, and chemists. This index is used to determine the potential for life on a planet or moon.
A co-orbital orbit is one of the six types of orbits that asteroids and SCs (small celestial bodies) can have in relation to the planets in our solar system. The image above shows this type of orbit in the top right corner. The orange dot represents the Sun, and the thick yellow circle represents the planet’s orbit, which is limited by its closest and farthest distance from the Sun. An asteroid in a co-orbital orbit follows a similar path as a planet, maintaining a consistent distance from it. Examples of groups of asteroids in co-orbital orbits include the Trojans and the Greeks.
A transit, also known as an astronomical transit, refers to an astronomical event where one celestial body passes in front of another from the perspective of an observer at a specific location, causing a partial obscuration of the latter body.
The Roche limit denotes the radius of the orbit followed by a satellite revolving around a celestial body, at which the tidal forces generated by the central body’s gravity are in equilibrium with the satellite’s self-gravity.
Radiant, derived from the Latin word “radians” meaning radiating, designates a specific area on the celestial sphere that appears to be the origin of meteors. These meteors become visible when the Earth intersects with a group of meteoric bodies orbiting the Sun in a general orbit.
The Local Interstellar Cloud (LIC) denotes an interstellar cloud, approximately 30 light-years in size, that the Solar System is presently traversing.
The initial trimester (Latin: Luna crescens dimidiata) is the period of the Moon in which precisely half of its apparent part is illuminated, and, unlike the final trimester, the proportion of the illuminated part at this moment grows (i.e., the Moon transitions from new moon to full moon). During this phase, the Moon is in the eastern quadrature, meaning the angular distance between the Moon and the Sun is 90°. The Moon is positioned to the east of the Sun, and the western section of the Moon’s visible surface is lit up.
A plutoid is a kind of small planet in our solar system. Plutoids refer to celestial objects that belong to this category.
An occultation is a fascinating event in astronomy where one celestial body passes directly in front of another celestial body, causing a partial or complete blockage of the view.
The uncertainty parameter, also known as the U value, is a parameter created by the Minor Planet Center to measure and describe the level of uncertainty in the calculated perturbed orbit of a minor planet. It is represented on a logarithmic scale from 0 to 9, indicating the uncertainty arc of the average anomaly of a minor planet after 10 years of orbital observation. On the JPL Small-Body Database Browser website, the uncertainty parameter is also referred to as the condition code. However, it is not recommended to solely rely on the U value for analysis or decision-making.
The Hill sphere is a region of gravitational influence located between the Lagrangian points L1 and L2, which are positioned on the line connecting the centers of two celestial bodies. The Hill sphere is characterized by its small size in this particular direction, limiting the area of gravitational influence exerted by the subordinate body. As a result, any third body orbiting around the subordinate body beyond this distance will partially pass outside the Hill sphere. Consequently, the tidal forces exerted by the central body will increasingly perturb the orbit of the third body. Ultimately, the subordinate body loses its influence.
A comet’s tail is a elongated plume of dust and gas composed of cometary matter. It forms when a comet approaches the Sun and becomes visible due to the scattering of sunlight on it. Typically, the comet’s tail is directed away from the Sun.
Near-solar comets known as the Kreutz family are named after astronomer Heinrich Kreutz, who first discovered their connection. It is believed that they all originated from a single large comet that fragmented several centuries ago.
The Pole of the World is a point on the celestial sphere where the stars appear to move due to the Earth’s rotation on its axis. The North Pole of the World aligns with the geographic north, while the South Pole aligns with the geographic south. The North Pole of the World is located in the constellation Ursa Minor, with Polaris being the closest star. The South Pole of the World is located in the constellation Octans. Due to the Earth’s axis precession, the positions of the poles of the world shift by approximately 20 arcseconds per year.
Stellar days refer to the time it takes for a celestial body to complete one rotation around its axis in relation to distant stars. This is measured in an inertial frame of reference, typically associated with distant stars. For example, on Earth, a stellar day is the time it takes for the Earth to complete one full revolution around its axis with respect to distant stars.
An osculating orbit is the gravitational Keplerian orbit of an object in space at a specific moment in time. This orbit is typically an ellipse or another section of a cone, relative to a central body. It represents the hypothetical path that the object would follow based on its current position and velocity, assuming no further perturbations or influences such as the nonsphericity of the central body, gravitational effects from other celestial bodies, or non-gravitational forces.
Synchronous rotation, also known as tidal capture, refers to the situation when a satellite orbits around its axis at the same rate as it orbits around the central body. As a result, the satellite always keeps the same side facing the central body. This phenomenon is commonly observed in many large natural satellites within the solar system.
Planetary equilibrium temperature, on the other hand, is a theoretical temperature that a planet would have if it were a completely black body and only heated by the star it orbits. In this model, the presence or absence of an atmosphere and the greenhouse effect are not taken into account. The theoretical blackbody temperature is assumed to be radiated from the planet’s surface.
Hot Neptune is a type of exoplanet that comprises of planets with masses similar to Uranus or Neptune that orbit very close to their star (always within a distance of less than 1 astronomical unit). The mass of a hot Neptune is made up of a central core and a dense atmosphere that occupies the majority of the planet’s volume.
The repetitive (retrograde) movement of the planets – when observed from Earth, the planets appear to move against the backdrop of the stars in the celestial sphere from west to east, which is opposite to the motion of the Sun (annual) and the Moon.
The orbit of the Earth – the path followed by the Earth as it revolves around the Sun, with an average distance of approximately 149.6 million kilometers (152.1 million km at its farthest point, known as aphelion; 147.09 million km at its closest point, known as perihelion).
The limb, derived from the Latin word “limbus” meaning boundary, edge, or limit, refers to the visible boundary of the disk of the Moon, Sun, or planet as projected onto the celestial sphere.
A solar day is the duration of time in which a celestial body completes one rotation around its axis relative to the center of the Sun. More precisely, it is the time interval between two culminations (passages through the meridian) of the center of the Sun in a specific location on Earth (or another celestial body).
Half-body refers to a region that is partially illuminated, lying between areas of complete darkness and full brightness. In the field of optics, this phenomenon occurs when an opaque object casts a shadow and a penumbra is formed due to the illumination from a light source that has dimensions comparable to both the object and the distance between them. The penumbra represents the outer portion of the shadowed area, where only a fraction of the light source is visible. This is distinct from the full shadow, where the source is completely obscured.
The Goldfish, known as Dorado in Latin, is a constellation located in the southern hemisphere of the celestial sphere. Covering an expanse of 179.2 square degrees in the sky, it boasts 32 stars that can be seen with the naked eye.
Comets in the main asteroid belt are celestial bodies that revolve around the Sun within the region of the primary asteroid belt, and during a specific phase of their orbit, they exhibit cometary behavior.
The snow line is a feature of the protoplanetary system of a star observed in astronomy and planetology. It is the distance from the star at which the temperature drops to a level that allows basic volatile compounds like water, ammonia, methane, molecular nitrogen, and chlorine to solidify.
Sub-brown dwarfs, also known as brown subdwarfs, are cold formations that exist below the mass limit of brown dwarfs. These formations are often classified as planets due to their similarities in mass. Sub-brown dwarfs have a mass that is less than 0.012 solar masses or 12.57 Jupiter masses, although there is no defined lower limit. Interestingly, the formation process of sub-brown dwarfs is more akin to that of stars rather than planets. They are created through the collapse of a gas cloud, rather than through accretion or core collapse of circumstellar disk material. This scientific phenomenon showcases the diverse nature of celestial bodies.
Elongation is a term used in astronomy to describe the angular distance between the Sun and a planet (or Moon) as observed from Earth. It is also utilized to measure the angular distance between two points on the celestial sphere. The concept of elongation plays a key role in understanding the positions and movements of celestial objects in relation to one another.
The maximum angles of deviation for Mercury and Venus do not surpass 28 and 47 degrees, respectively.
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To put it in simpler terms, elongation is the angle between a planet and the Sun or between a planet and its satellite, as seen from Earth. You might argue that this is not very straightforward. Firstly, what exactly does geocentric angle mean? Secondly, why create a specialized term for angles?
Geocentric means that the vertex of the angle is on Earth.
Elongation refers to the measurement of the angle between a planet and the Sun in the sky as observed from Earth. This concept is often used in astronomy. For instance, imagine yourself as an observational astronomer gazing at the night sky. As the Sun sets in the western horizon, you may notice a planet like Jupiter positioned towards the southern direction. In this scenario, you can determine that the angle between the Sun and Jupiter in the sky is 90 degrees. Consequently, this measurement can also be referred to as the elongation of Jupiter, which is also 90 degrees.
The elongation of a planet is defined as the angular separation between the Sun and the planet in the sky, with you standing on Earth at the apex of that angle. This angle varies for different planets in the solar system, so the angle between Jupiter and the Sun measured simultaneously will differ from your measurement.
What is the purpose of determining elongation in the first place?
Astronomers in the past were deeply intrigued by the peculiar movements of the planets. They observed that the planets did not move in a uniform manner against the backdrop of the stars, sometimes accelerating and other times decelerating. Additionally, on occasions, the planets would come to a halt and then reverse their direction. Particularly, planets like Mars, Jupiter, and Saturn would create intricate loops in their paths relative to the stars!
To comprehend these phenomena, astronomers needed to find a way to measure the planets’ speed in relation to the stars. But how does one measure this without knowing the distances to the planets? The solution was to measure the angular velocity of the planets because angles are independent of distance and provide a reliable metric for comparison.
Mercury departs from our daytime sky by a maximum of 28°, while Venus does so by a maximum of 48°. In other words, Mercury reaches a maximum elongation of 28 degrees, while Venus reaches a maximum elongation of 48 degrees.
The elongation of Venus reaches a maximum of nearly 48 degrees. Source: David Jefferey
Differences between Eastern and Western Elongation
Elongations (referring to Mercury and Venus) can occur in the east or west.
Since Mercury and Venus are always located near the Sun, they can only be observed in the evening or morning sky. (They can sometimes be seen at midnight or during the deep night in northern Russia, above the Arctic Circle, although this is not always the case!)
In the evenings, Mercury and Venus are visible when they appear to the left of the Sun. Left corresponds to east. This is why these elongations are referred to as eastern elongations..
The morning elongations are referred to as western elongations. During these elongations, Mercury and Venus can be found to the right of the Sun, specifically in the western direction.
STRETCHING OF CELESTIAL BODIES
Star 1 exhibits both an eastern elongation and a western elongation in the diagram. On the other hand, star 2 does not display any elongations.
During the initial month of summer, individuals will have the chance to witness the “hard-to-find celestial body” known as Mercury without the aid of any optical instruments shortly after the sun has set. Continue reading to discover the methods, timing, and locations for observing the smallest planet within the solar system.
How and where can you observe Mercury?
Mercury is set to reach its maximum eastern elongation, or its greatest distance from the Sun, on Thursday, June 4, 2020. However, it will also be favorably positioned for viewing in the evening sky on both June 4 and June 3. During its maximum elongation, Mercury will be 24 degrees away from the Sun. It should be visible to the naked eye approximately 40-60 minutes after sunset. This small planet, the smallest in our solar system, will have an apparent stellar magnitude of 0.4. It will appear relatively low in the sky above the western horizon and will be situated between two prominent stars, Capella and Procyon.
If you wish to observe the disk of the planet, you will require a telescope of medium power. When utilizing a telescope, you will be able to view Mercury’s disk, which is illuminated to less than half (approximately 40%).
Who has the ability to observe the “hard-to-find planet”?
Mercury, at its maximum eastern elongation on June 4, 2020, will be most visible in the Northern Hemisphere. For observers situated in the Southern Hemisphere, the conditions for sighting the planet will not be ideal. Among all the planets visible to the naked eye, Mercury is typically the most challenging to spot throughout the majority of the year. If you have the chance to observe Mercury on June 3-4, seize it, as each subsequent day will see the “elusive planet” becoming fainter in the evening sky.
What does elongation mean?
Elongation refers to the position of a planet when its angular distance from the Sun is at its maximum for observers on Earth. In other words, an observer on Earth is situated at the point where this angle is the greatest.
Mercury and Venus have the potential for maximum elongation since they are located closer to the Sun than Earth and never stray too far from it in the sky. As a result, Mercury has a maximum angle of 28 degrees, while Venus has a maximum angle of 48 degrees.
Being at or near maximum elongation provides ideal conditions for observing a planet. When a planet reaches its farthest point from the Sun, it becomes easily visible in the sky without the need for binoculars or telescopes.
Eastern and Western Elongation
The concept of elongation can be divided into two categories: eastern elongation and western elongation. Due to their proximity to the Sun, Mercury and Venus can only be observed in the evening or morning sky, never in the middle of the night.
When Mercury and Venus are positioned to the left (or east) of the Sun, they are visible in the evening sky. This specific elongation is referred to as the eastern elongation. During or around this time, the planet becomes visible shortly after sunset.
On the other hand, when Mercury and Venus are positioned to the right (or west) of the Sun, they are visible in the morning sky. This particular elongation is known as the western elongation. During or around this time, Mercury and Venus become visible shortly before dawn.
We hope you have clear skies and successful observations!
The evening sky in March is illuminated by Venus, the brightest planet in our solar system. On Tuesday, March 24, 2020, the conditions for observing Venus will be optimal. To catch a glimpse of this celestial phenomenon, let’s explore the best methods and timing for observing the “evening star”.
Understanding the Significance of Venus’ Maximum Eastern Elongation
On the evening of March 24th, astronomers and stargazers will have the opportunity to witness a fascinating celestial event – Venus’ maximum eastern elongation. Known as the third brightest celestial object, Venus will reach its farthest point from the Sun in the sky, forming an angle of 46°. As a result, observers will be able to enjoy the best visibility of Venus in the evening sky.
Occurrences like this take place approximately every eighteen months, either in the morning or evening sky, depending on Venus’ position relative to the Sun. When Venus is positioned to the east of the Sun, it becomes visible during the evening hours. Conversely, when Venus is situated to the west of the Sun, it can be observed in the predawn sky.
The best conditions for observing the planets occur when they are near elongations. On March 24, after sunset, Venus will be so brilliantly visible above the western horizon that there will be no need for any optical instruments to see it. The planet will shine with a brightness of -4.4 stars. To ensure you don’t miss the beautiful sight of Venus, use the Star Walk 2 astronomy app to determine the exact time the planet rises and sets in the sky above your location, and be prepared to observe. The days leading up to and following Venus’ maximum elongation are also ideal for observing the planet in the evening sky. Those with exceptional eyesight may even catch a glimpse of Venus during daylight hours. For everyone else, Venus will be the brightest star in the sky after sunset.
On the night of March 24, people in the Northern Hemisphere will have the exciting opportunity to witness the magnificent beauty of Venus, while those in the Southern Hemisphere may not have the most optimal conditions to observe the planet. When Venus is elongated near the vernal equinox, it stays visible in the sky for a longer period after sunset, maximizing its visibility. However, when the elongation coincides with the autumnal equinox (which happened on March 20 this year in the Southern Hemisphere), the planet can still be seen in the sky, but the visibility conditions are not as favorable.
