Uranus Size and Uranus Distance from the Sun

Uranus Size and Uranus Distance from the Sun

Today, through incessant research and endless efforts, humans have gone far ahead of the moon in their struggle to conquer stars and planets. As a result, they have been able to make great strides in this field. This endless series of human achievements are a testament to immense research and development in the field of science and engineering.

Today, man has gained access to the moon, and many other planets, and new information about the planets are being obtained every day. All these achievements would have been inconceivable had there been no progress in Science, and engineering in particular. 

In this journey of unprecedented advancements, man has always strived to obtain valuable information about many planets by observing them deeply and thanks to these efforts, he has discovered many planets so far.  We will try to provide all possible information about these planets. In this regard today we will take a detailed look at the planet Uranus.

It is contended that the disparities between the ice giants and the gas giants arise from their construction history. The Solar System is theorized to have been created from a revolving disk of gas and dust known as the presolar nebula. Largely of the nebula’s gas, mainly hydrogen and helium, formed the Sun, and the dust particles accumulated jointly to form the first protoplanets. As the planets evolved, some of them ultimately accumulated sufficient matter for their gravity to hold on to the nebula’s residue gas.

Planetary engineering is the expansion and utilization of technology for the purpose of affecting the environment of a planet. Planetary engineering confines an assortment of methods such as terraforming, seeding, and geoengineering.


Uranus tends to be the seventh planet from the Sun and it has the third biggest diameter in our solar system. It was the foremost planet discovered with the assistance of a telescope, Uranus was found in 1781 by astronomer William Herschel, although he initially believed it was either a comet or a star.

It was two years later that the entity was universally reckoned as a new planet, in part because of investigations by astronomer Johann Elert Bode. Herschel attempted unsuccessfully to name his finding GeorgiumSidus after King George III. Rather, the scientific community acknowledged Bode’s recommendation to name it Uranus, the Greek god of the sky, as indicated by Bode.​

Uranus is approximately four times broader than Earth. If Earth were a big apple, Uranus would have been just the size of a basketball.

Uranus encircles our Sun, a star, and is the seventh planet from the Sun located at a distance of about 1.8 billion miles (2.9 billion kilometers).

Uranus takes about 17 hours to revolve once (a Uranian day), and about 84 Earth years to finish off an orbit of the Sun (a Uranian year).

Uranus is an ice colossus. Most of its mass is a hot, thick, and dense fluid of “icy” materials – water, methane, and ammonia – above a tiny stony, or rocky core.

Uranus has an environment composed mainly of molecular hydrogen and atomic helium, with a slight amount of methane.

Uranus tends to have 27 known moons, and they are named after personalities from the works of William Shakespeare and Alexander Pope.

Uranus tends to have 13 detected rings. The inner rings are thin, narrow, and dark and the exterior rings are brilliantly colored.

Voyager 2 has so far been the only spacecraft to fly by Uranus. No spacecraft has circumnavigated this remote planet to study it at its size and up close.

As we know it, Uranus cannot support life.

Like Venus, Uranus revolves east to west. But Uranus is unusual in that it revolves on its side.

Uranus has the third biggest diameter in our solar system, due to which Uranus is very cold and windy. The ice colossus is encircled by 13 vague rings and 27 small moons as it revolves at an almost 90-degree angle from the plane of its trajectory. This extraordinary angle makes Uranus seem to whirl sideways, circumnavigating the Sun like a rumbling ball.

The first planet detected with the assistance of a telescope, Uranus was found out in 1781 by astronomer William Herschel, though he initially guessed it was either a comet or a star. It was two years subsequently that the object was universally acknowledged as a new planet, in part because of investigations by astronomer Johann Elert Bode.

William Herschel tried abortively to name his finding Georgium Sidus after King George III. Rather, the planet was quoted for Uranus, the Greek god of the sky, as proposed by Johann Bode.

Uranus’ atmosphere is not facilitative to life as we know it. The temperatures, pressures, and materials that depict this planet are largely likely too drastic and volatile for organisms to acclimate to.

Size and  the Distance between Sun and Uranus

With a radius of 15,759.2 miles (25,362 kilometers), Uranus is 4 times wider or broader than Earth. If Earth was the size of a nickel, Uranus would have been nearly as large as a softball.

From an intermediate distance of 1.8 billion miles (2.9 billion kilometers), Uranus is 19.8 astronomical units farther from the Sun. One astronomical unit denotes the distance from the Sun to Earth. From this distance, it takes sunlight 2 hours and 40 minutes to transit from the Sun to Uranus.

One day on Uranus equals about 17 hours (the time it carries for Uranus to revolve or whirl once). And Uranus puts together a complete rotation around the Sun (a year in Uranian time) in nearly 84 Earth years (30,687 Earth days).

Uranus is the solitary planet whose equatorial is virtually at a right angle to its orbit, with a slant of 97.77 degrees – may be the result of a crash with an Earth-sized object long ago. This unusual inclination angle induces the most drastic seasons in the solar system. For almost a quarter of each Uranian year, the Sun shines through straight over each pole, plummeting the other half of the planet into a 21-year-long, dark winter.

Uranus is also one of only two planets that revolve in the opposing direction than most of the planets (Venus is the other one), from east to west.

Uranus has 27 detected moons. Whereas most of the satellites circumnavigating other planets take their names from Greek or Roman myths, Uranus’ moons are outstanding in being named for personalities from the works of William Shakespeare and Alexander Pope.

All of Uranus’ internal moons emerge to be around half water ice and half rock. The arrangement of the exterior moons hangs around unknown, but they have possibly seized asteroids.

Uranus tends to have two clusters of rings. The internal system of nine rings comprises largely narrow, dark grey rings. There are two exterior rings: the innermost one is rubicund like dusty rings elsewhere in the solar system, and the exterior ring is blue similar to Saturn’s E ring.

Based on the increasing distance from the planet, these rings are called Zeta, 6, 5, 4, Alpha, Beta, Eta, Gamma, Delta, Lambda, Epsilon, Nu, and Mu. Some of the bigger rings are encircled by belts of fine dust.

Uranus assumed shape when the remainder of the solar system was created about 4.5 billion years ago – when gravity yanked stirring gas and dust in to become this ice colossus. Similar to its neighbor Neptune, Uranus plausibly formed closer to the Sun and shifted to the outer solar system almost 4 billion years ago, where it is virtually the seventh planet from the Sun.

Uranus is one of two ice colossi in the exterior solar system (the other is Neptune). Most (80% or more) of the planet’s mass is constituted of a hot dense liquid of “icy” materials – water, methane, and ammonia – above a small rocky or stony core. Near the core, it warms up to 9,000 degrees Fahrenheit (4,982 degrees Celsius).

Uranus is somewhat bigger in diameter than its neighbor Neptune, yet tinier in mass. It is the second slighte stthick planet; Saturn is the slightest dense of all.

Uranus obtains its blue-green pigment from methane gas in the environment. Sunlight passes through the environment and is ricocheted back out by Uranus’ cloud tops. Methane gas soaks up the red component of the light, resulting in a blue-green color.

Uranus tends to be the seventh planet from the Sun and its name is a reference to the Greek god of the sky, Uranus (Caelus), who, as per Greek mythology, was the father of Cronus (Saturn), grandfather of Zeus (Jupiter) and great-grandfather of Ares (Mars). It has the third-biggest planetary radius and fourth-biggest planetary mass in the Solar System. Uranus is identical in arrangement to Neptune, and both have preponderated chemical compositions which vary from that of the enormous gas goliath Jupiter and Saturn. For this rationale, scientists frequently categorize Uranus and Neptune as “ice giants” to differentiate them from the other giant planets.

As with gas colossi, ice giants also seem to be lacking a well-defined “solid surface.” Uranus’s atmosphere is analogous to Jupiter’s and Saturn’s in its preliminary composition of hydrogen and helium, but it encompasses more “ices” such as ammonia, water, and methane, along with flickers of other hydrocarbons. It has the coldest planetary environment in the Solar System, with a minimum temperature of 49 K (−224 °C; −371 °F), and has a complicated, layered cloud configuration with water believed to comprise the lowest clouds and methane the topmost coating of clouds. The interior of Uranus is largely formulated of ice and rock.

Similar to the other giant planets, Uranus also has a ring system, a magnetosphere, and innumerable moons. The Uranian system has an unusual composition because its axis of the orbit is leaned sideways, almost into the plane of its solar orbit. Its south and north poles, thus, lie where largely other planets have their equators. In 1986, pictures from Voyager 2 indicated Uranus as a virtually nondescript and featureless planet in visual light, without the cloud bands or storms attributed to the other colossus planets. Voyager 2 stays the only spacecraft to have visited the planet. Investigations from Earth have demonstrated seasonal transition and boosted weather activity as Uranus moved toward its equinox in 2007. Wind speeds can attain 250 meters per second (900 km/h; 560 mph).

Like the classical planets, Uranus is observable to the naked eye, but it was never acknowledged as a planet by ancient spectators because of its sluggish orbit and dimness. Sir William Herschel first scrutinized Uranus on 13 March 1781, leading to its finding as a planet, extending the known limitations of the Solar System for the first time in history and bringing in Uranus to be the first planet categorized as such with the assistance of a telescope.

Uranus had been scrutinized on many occurrences before its acclaim as a planet, but it was commonly wrongly treated as a star. Perhaps the earliest known investigation was by Hipparchos, who in 128 BC might have documented it as a star for his star catalog that was later integrated into Ptolemy’s Almagest. The prematurely substantial sighting was in 1690, when John Flamsteedscrutinized it at least six times, recording it as 34 Tauri. The French astronomer Pierre Charles Le Monnier investigated Uranus at least twelve times between 1750 and 1769, consisting of four successive nights.

Sir William Herschel scrutinized Uranus on 13 March 1781 from the grassland of his house located at 19 New King Street in Bath, Somerset, England (now declared as the Herschel Museum of Astronomy), and originally reported it (on 26 April 1781) as a comet. With a homemade 6.2-inch mirroring telescope, Herschel committed to a series of investigations on the parallax (obvious shifting of the position of an object that happens when an observer changes position) of the fixed stars.

Uranus encircles the Sun once every 84 years, taking an average of seven years to depart through each of the dozen constellations (groups of stars) of the zodiac. In 2033, the planet will have made its third completed rotation around the Sun since being explored in 1781. The planet has been replaced to the juncture of its finding northeast of Zeta Tauri twice since then, on 25 March 1865 and 29 March 1949. Uranus will return to this spot again on 3 April 2033. Its mean distance from the Sun is approximately 20 AU (3 billion km; 2 billion mi). The disparity between its minimum and maximum distance from the Sun is 1.8 AU, bigger than that of any other planet, though not as big as that of the dwarf planet Pluto. The intenseness of sunlight changes conversely with the square of the distance, and so on Uranus (at about 20 times the distance from the Sun described in relation to Earth) it is about 1/400 the intensity or vigor of light on Earth.

The orbital components of Uranus were first computed in 1783 by Pierre-Simon Laplace. With time, disparities began to emerge between the forecasted and explored orbits, and in 1841, John Couch Adams first suggested that the discrepancies might be due to the gravitational pull of an unnoticed planet. In 1845, Urbain Le Verrier started up his own independent investigation into Uranus’s orbit. On 23 September 1846, Johann Gottfried Galle uncovered a new planet, later named Neptune, at nearly the position indicated by Le Verrier.

The orbital duration of the interior of Uranus is 17 hours and 14 minutes. As on all the massive planets, its upper atmosphere encounters powerful winds in the direction of orbit. At some stretches, such as about 60 degrees south, observable characteristics of the atmosphere move much quicker, making a full orbit or rotation in as little as 14 hours.

The Uranian axis of a cycle is roughly similar to the plane of the Solar System, with an axial slant of 97.77° (as defined by prograde rotation. This provides seasonal changes entirely unlike those of the other planets. Near the solstice (either of the two times of the year when the sun is farthest from the equator), one pole faces the Sun constantly and the other faces away, with only a thin strip around the equatorial encountering a rapid day-night cycle, with the Sun low over the horizon. On the other side of Uranus’s trajectory, the direction of the poles towards the Sun is inverted. Each pole gets around 42 years of ongoing sunlight, pursued by 42 years of darkness. Near the time of the equinoxes (either of two times in a year when the sun crosses the celestial equator), the Sun confronts the equator of Uranus providing a duration of day–night cycles similar to those seen on the majority of the other planets.

One consequence of this axis direction is that averaged over the Uranian year, the regions located near the poles of Uranus obtain a greater energy input from the Sun than its tropical regions. Nonetheless, Uranus is hotter at its equatorial than at its poles. The underlying or basic mechanism that provokes this is unknown. The reason for Uranus’s unique axial angle or tilt is also not known with confidence, but the expected anticipation is that during the building of the Solar System, an Earth-sized protoplanet crashed with Uranus, resulting in the tilted direction. Analysis by Jacob Kegerreis of Durham University indicates that the tilt resulted in a rock bigger than the Earth smashing into the planet 3 to 4 billion years ago. Uranus’s south pole was indicated basically directly at the Sun at the time of Voyager 2’s flyby in 1986. The quoting of this pole as “south” employs the definition presently supported by the International Astronomical Union, i.e. that the north pole of a planet or satellite is the pole that points above the constant or unchanging plane of the Solar System, irrespective of the path the planet is whirling. A diverse pattern is sometimes used, in which a body’s south and north poles are elucidated according to the right-hand rule in connection to the direction of rotation.

Uranus’s mass is approximately 14.5 times that of Earth, earning it the least massive of the enormous planets. Its diameter is scarcely bigger than Neptune’s at around four times that of Earth. An ensuing density of 1.27 g/cm3 turns Uranus to be the second least dense planet, after Saturn. This value suggests that it is made mostly of different ices, such as ammonia, water, and methane. The entire mass of ice in Uranus’s internal regions is not accurately known, because diverse figures appear relying on the model chosen; it must be between 9.3 and 13.5 Earth masses. Hydrogen and helium make up only a small portion of the total, with between 0.5 and 1.5 Earth masses. The residue of the non-ice mass (0.5 to 3.7 Earth masses) consists of rocky material.

The typical prototype of Uranus’s configuration is composed of three layers: a rocky (silicate, iron–nickel) core in the center, an icy mantle in the center, and an exterior gaseous hydrogen/helium envelope. The core is moderately small, with a mass of only 0.55 Earth masses and a radius smaller than 20% of Uranus’; the mantle constitutes its bulk, with around 13.4 Earth masses, and the upper environment is somewhat flimsy, weighing about 0.5 Earth masses and expanding for the last 20% of Uranus’s radius.

The intense temperature and pressure deep within Uranus may dissipate the methane molecules, with the carbon atoms thickening into crystals of diamond that rain down through the mantle like hailstones. This sensation is identical to diamond rains that are theorized by scientists to exist on Jupiter, Saturn, and Neptune.

The bulk combinations of Uranus and Neptune are distinct from those of Jupiter and Saturn, with ice overpowering gases, hence explaining their different classification as ice colossi. There may be a coating of ionic water where the water molecules decompose down into a soup of hydrogen and oxygen ions, and deeper down superionic water in which the oxygen crystallizes but the hydrogen ions move voluntarily within the oxygen lattice.

Uranus’s interior heat seems significantly lower than that of the other colossus planets; in astronomical terms, it has a low thermal flux (variability). Why Uranus’s internal temperature is so meager is yet not comprehended. Neptune, which is Uranus’s immediate twin in size and composition, emits 2.61 times as much energy into space as it acquires from the Sun, but Uranus spreads out barely any surplus heat at all.

Though there is no well-illustrated solid surface within Uranus’s internal regions, the exterior portion of Uranus’s gaseous envelope that is approachable to remote sensing is called its atmosphere. Remote-sensing capacity stretches down to around 300 km below the 1 bar (100 kPa) level, with a related pressure of around 100 bar (10 MPa) and a temperature of 320 K (47 °C; 116 °F).

At ultraviolet and visible wavelengths, Uranus’s atmosphere is commonplace in contrast to the other giant planets, even to Neptune, to which it is otherwise nearly similar. When Voyager 2 flew by Uranus in 1986, it explored a total of ten cloud characteristics across the whole planet. One suggested explanation for this shortage of features is that Uranus’s interior heat is significantly lower than that of the other giant planets, as stated formerly Uranus is the chilliest planet in the Solar System.

Engr Fahad

My name is Shahzada Fahad and I am an Electrical Engineer. I have been doing Job in UAE as a site engineer in an Electrical Construction Company. Currently, I am running my own YouTube channel "Electronic Clinic", and managing this Website. My Hobbies are * Watching Movies * Music * Martial Arts * Photography * Travelling * Make Sketches and so on...

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