formation of the solar system 6 steps

A shock wave from a supernova may have triggered the formation of the Sun by creating relatively dense regions within the cloud, causing these regions to collapse. [43][67], In contrast to the outer planets, the inner planets are not thought to have migrated significantly over the age of the Solar System, because their orbits have remained stable following the period of giant impacts. (4) There are some notable exceptions to these general patterns. the process by which atoms collide and fuse together to form new, more massive elements (releasing a great amount of energy) protostellar disk. [14] Late in the life of these stars, they ejected heavier elements into the interstellar medium. When the Sun's orbit takes it outside the galactic disc, the influence of the galactic tide is weaker; as it re-enters the galactic disc, as it does every 2025million years, it comes under the influence of the far stronger "disc tides", which, according to mathematical models, increase the flux of Oort cloud comets into the Solar System by a factor of 4, leading to a massive increase in the likelihood of a devastating impact. Astronomers feel confident that our Solar System formed by accretion because now they are able to glimpse a similar process occurring in part of the Orion Nebula. [79] The evolution of the outer Solar System also appears to have been influenced by space weathering from the solar wind, micrometeorites, and the neutral components of the interstellar medium. The process was most efficient for Jupiter and Saturn; hence, their compositions are most nearly cosmic. Much less gas was captured by Uranus and Neptune, which is why these two planets have compositions dominated by the icy and rocky building blocks that made up their large cores rather than by hydrogen and helium. Arthur Stanley Eddington's confirmation of Albert Einstein's theory of relativity led to his realisation that the Sun's energy comes from nuclear fusion reactions in its core, fusing hydrogen into helium. Thats why they are called rocky, or terrestrial, planets. As the nebula shrinks, its rotation causes it to flatten into a disk. Eventually, it will have to again resort to the reserves of hydrogen and helium in its outer layers. Source: NASA/JPL-Caltech. (One light-year equals 6 trillion miles.) The Moon will continue to recede from Earth, and Earth's spin will continue to slow gradually. [112], Around 5.4billion years from now, the core of the Sun will become hot enough to trigger hydrogen fusion in its surrounding shell. In some ways, the swarms of moons around these worlds resemble mini versions of our solar system. Chemical Condensation Sequence in the Solar Nebula. [47], At the end of the planetary formation epoch the inner Solar System was populated by 50100 Moon- to Mars-sized protoplanets. The Oort Cloud is made of icy pieces of space debris - some bigger than mountains orbiting our Sun as far as 1.6 light-years away. Astronomy Lecture Notes - Solar System Formation Main goal: Understand the reason for the different sizes, compositions, and orbital and rotational motions of planets (Terrestrial, Jovian) and minor objects (Pluto and similar objects, asteroids, comets), including exceptions to the general patterns. Researchers use AI to discover new planet outside solar system. This shell of material is thick, extending from 5,000 astronomical units to 100,000 astronomical units. Much of the material is concentrated in the hot center, which will ultimately become a star. Nearest to the Sun, only rocky material could withstand the heat when the solar system was young. [1] Studies of ancient meteorites reveal traces of stable daughter nuclei of short-lived isotopes, such as iron-60, that only form in exploding, short-lived stars. [50], One unresolved issue with this model is that it cannot explain how the initial orbits of the proto-terrestrial planets, which would have needed to be highly eccentric to collide, produced the remarkably stable and nearly circular orbits they have today. As an Amazon Associate we earn from qualifying purchases. It will study every phase in the history of our Universe, ranging from the first luminous glows after the Big Bang, to the formation of solar systems capable of supporting life on planets like Earth, to the evolution of our own Solar System. A. There's an invisible monster on the loose, barreling through intergalactic space so fast that if it were in our solar system, it could travel from Earth to the Moon in 14 minutes. A nebula is a cloud of gas and dust in space. (b) The volume of gas at 20C20^{\circ} \mathrm{C}20C and 1.00 bar adsorbed on the surface of 1.50 g of a sample of silica at 0C0^{\circ} \mathrm{C}0C was 1.42cm31.42\ \mathrm{cm}^{3}1.42cm3 at 56.4 kPa and 277cm3277\ \mathrm{cm}^{3}277cm3 at 108 kPa. The Solar System has evolved considerably since its initial formation. [34] Today, the four giant planets comprise just under 99% of all the mass orbiting the Sun. Module 3 Lab 6: Formation of the Solar System Learning Objective: You will explore the processes/steps of solar system formation and identify which process/step leads to the characteristic we see today. The next full moon is the Hunter's Moon; the Travel, Dying Grass, Sanguine, or Blood Moon. Direct link to Cameron Gibelyou's post I think the most basic an, Posted 8 years ago. And since they formed from a rotating disk, the planets all orbit the same way. Textbook content produced by OpenStax is licensed under a Creative Commons Attribution License . There are still leftover remains of the early days though. Our planetary system is called the solar system because we use the word solar to describe things related to our star, after the Latin word for Sun, "solis.". This edge occurs between 80-100 astronomical units. The sun's gravitational pull helped in drawing material from this low-density protostar. Finally the pressure caused by the material was so great that hydrogen atoms began to fuse into helium, releasing a tremendous amount of energy. Still others, such as Earth's Moon, may be the result of giant collisions. Now, think about how a round object spins. Some of the scattered objects, including Pluto, became gravitationally tied to Neptune's orbit, forcing them into mean-motion resonances. Its subsequent development has interwoven a variety of scientific disciplines including astronomy, chemistry, geology, physics, and planetary science. Almost all meteorites (see the Canyon Diablo meteorite) are found to have an age of 4.6billion years, suggesting that the Solar System must be at least this old. As they did, a tiny bit of matter transformed into a whole lot of energy, and a star was born. The next full moon is the Pink Moon also known as the Sprouting Grass, Egg, or Fish Moon. Jupiter is 11 times the size (in diameter) of Earth and more than twice as big as all the other planets combined. The Sun and the planets formed together, 4.6 billion years ago, from a cloud of gas and dust called the solar nebula. Some of the material from the impact was absorbed into the liquefied Earth but some material ricocheted into space, where it settled into orbit and condensed as the Moon. All remaining planets' orbits will expand; if Venus, Earth, and Mars still exist, their orbits will lie roughly at 1.4AU (210millionkm; 130millionmi), 1.9AU (280millionkm; 180millionmi), and 2.8AU (420millionkm; 260millionmi), respectively. Therefore, the Sun's vertical position cannot alone explain such periodic extinctions, and that extinctions instead occur when the Sun passes through the galaxy's spiral arms. Models show that density and temperature variations in the disk governed this rate of migration,[35][36] but the net trend was for the inner planets to migrate inward as the disk dissipated, leaving the planets in their current orbits. These compounds are quite rare in the Universe, comprising only 0.6% of the mass of the nebula, so the terrestrial planets could not grow very large. At their distance from the Sun, accretion was too slow to allow planets to form before the solar nebula dispersed, and thus the initial disc lacked enough mass density to consolidate into a planet. The "burning" in the sun isn't fire in the sense of combustion, where things are rapidly oxidized. At first the Moon orbited much closer to Earth. Let's dig in. [83][84][85] This origin is indicated by the large sizes of the moons and their proximity to the planet. Although the Solar System as a whole could be affected by these events, the Sun and planets are not expected to be disturbed. This model, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace. During this time, these worlds could support a water-based hydrologic cycle, but as they are too small to hold a dense atmosphere like Earth, they would experience extreme daynight temperature differences. However, there are (again) important exceptions to the general pattern. [52][55] Some of those massive embryos too were ejected by Jupiter, while others may have migrated to the inner Solar System and played a role in the final accretion of the terrestrial planets. Lets look in more detail at how material condensed at different places in the maturing disk (Figure 14.12). The ices that formed the Jovian planets were more abundant than the metals and silicates that formed the terrestrial planets, allowing the giant planets to grow massive enough to capture hydrogen and helium, the lightest and most abundant elements. That they continue to happen is evidenced by the collision of Comet ShoemakerLevy 9 with Jupiter in 1994, the 2009 Jupiter impact event, the Tunguska event, the Chelyabinsk meteor and the impact that created Meteor Crater in Arizona. By the end of this section, you will be able to: As we have seen, the comets, asteroids, and meteorites are surviving remnants from the processes that formed the solar system. For this reason, the first four planets Mercury, Venus, Earth, and Mars are terrestrial planets. NASAs Space Launch System (SLS) rocket with the Orion spacecraft atop has arrived at Launch Pad 39B at Kennedy Space Center. They have compared surface features on planets and moons across the solar system, the orbits of asteroids and comets, and the chemical composition and ages for recovered meteorites. Two NASA spacecraft launched in 1977 have crossed the termination shock: Voyager 1 in 2004 and Voyager 2 in 2007. A moon will raise a tidal bulge in the object it orbits (the primary) due to the differential gravitational force across diameter of the primary. Our mission is to improve educational access and learning for everyone. Also, the Moons gravity causes the oceans tides, reduces the Earths wobble (which helps stabilize climate), and slows the spin of the Earth. The order and arrangement of the planets and other bodies in our solar system is due to the way the solar system formed. Solar System Formation Activity (Cut and Paste) Card sorts can be fun and engaging activities to identify and explain the steps of solar system formation. Resonance in Jupiter and Saturn's orbits moves Neptune out into the Kuiper belt. [3], The time frame of the Solar System's formation has been determined using radiometric dating. Although the Sun and planets may survive, the Solar System, in any meaningful sense, will cease to exist. Direct link to Davin V Jones's post Tidal forces are the prim, Posted 3 years ago. This is still 1020 times more than the current mass in the main belt, which is now about 0.0005MEarth. Other examples are the Galilean moons of Jupiter (as well as many of Jupiter's smaller moons)[104] and most of the larger moons of Saturn. After that, gravity allowed the collapse to continue. What are planets? It is almost large enough to have become a star. [89][90] The formation of the Solar System began about 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. These icy pieces probably formed near the present orbits of Uranus and Neptune but were ejected from their initial orbits by the gravitational influence of the giant planets. [29] This marked the Sun's entry into the prime phase of its life, known as the main sequence. Direct link to WallAvi's post Is any acreation in our o, Posted 9 years ago. In summary, planets are bodies orbiting a star. Balance the following equations. [65][2][43], According to the Nice model, after the formation of the Solar System, the orbits of all the giant planets continued to change slowly, influenced by their interaction with the large number of remaining planetesimals. The initial formation period ended when much of the available raw material was used up and the solar wind (the flow of atomic particles) from the young Sun blew away the remaining supply of lighter gases. Planetesimals Form. Webb will be the premier observatory of the next decade, serving thousands of astronomers worldwide. Beyond the fringes of the Kuiper Belt is the Oort Cloud. There are many regularities to the motions in the solar system. We call them constraints because they place restrictions on our theories; unless a theory can explain the observed facts, it will not survive in the competitive marketplace of ideas that characterizes the endeavor of science. In the Suns system, Earth is one of four rocky planets, but a unique one, with rigid and molten layers. It orbits wayout in a belt of asteroids beyond Neptune (thoughPluto periodically comes closer to the Sun thanNeptune), and does not have enough gravity to clear the neighborhood around its path. [25] Studies of T Tauri stars show that they are often accompanied by discs of pre-planetary matter with masses of 0.0010.1M. Away from the center, solid particles can condense as the nebula cools, giving rise to planetesimals, the building blocks of the planets and moons. collapse, condensation, accretion How many of the planets orbit the Sun in the same direction as Earth does? [31], The various planets are thought to have formed from the solar nebula, the disc-shaped cloud of gas and dust left over from the Sun's formation. [34], When the terrestrial planets were forming, they remained immersed in a disk of gas and dust. Illustration of a fledgling solar system. Pluto and Charon are an example of this type of configuration. [132] After a further series of glancing blows, during which the likelihood of the Solar System's ejection rises to 30%,[133] the galaxies' supermassive black holes will merge. Even tiny asteroids can have moons. Mathematics. Lets take a look at these constraints one by one. The inner parts of the system are generally missing those materials that could not condense (form a solid) at the high temperatures found near the Sun. How does a solar system form? [86][87] Most such moons orbit in the direction opposite the rotation of their primary. This comes from an Anglo-Saxon childrens story, Goldilocks and the Three Bears. In the story, a young girl named Goldilocks wanders into the home of three bears, who are away. They did this by determining the age of stony materials from the asteroid belt. Between the inner and outer planets lies an area filled with millions of asteroids small rocky, icy, and metallic bodies left over from the formation of the Solar System. This is similar to the process by which raindrops on Earth condense from moist air as it rises over a mountain. [26] These discs extend to several hundredAUthe Hubble Space Telescope has observed protoplanetary discs of up to 1000AU in diameter in star-forming regions such as the Orion Nebula[27]and are rather cool, reaching a surface temperature of only about 1,000K (730C; 1,340F) at their hottest. center of nebula fusion begins, star is born. Posted 9 years ago. The 6 stages of formation are: 1. [2][75] The oldest known evidence for life on Earth dates to 3.8billion years agoalmost immediately after the end of the Late Heavy Bombardment. [11] Planetesimals beyond the frost line accumulated up to 4MEarth within about 3million years. As the Sun burns through its hydrogen fuel supply, it gets hotter and burns the remaining fuel even faster. Calculus. [48] One hypothesis for this "eccentricity dumping" is that the terrestrials formed in a disc of gas still not expelled by the Sun. As the large bodies moved through the crowd of smaller objects, the smaller objects, attracted by the larger planets' gravity, formed a region of higher density, a "gravitational wake", in the larger objects' path. When it collapsed, it fell in on itself, creating a disk of material surrounding it. [10] The cloud was about 20parsecs (65 light years) across,[9] while the fragments were roughly 1parsec (three and a quarter light-years) across. In 2007, researchers at the University of CaliforniaDavis determined that our Solar System was fully formed at 4.568 billion years ago. History of Solar System formation and evolution hypotheses, "Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets", "Birth of the planets: The Earth and its fellow planets may be survivors from a time when planets ricocheted around the Sun like ball bearings on a pinball table", "Triggered Star Formation inside the Shell of a WolfRayet Bubble as the Origin of the Solar System", "Lecture 13: The Nebular Theory of the origin of the Solar System", "The supernova trigger for formation of the solar system", "Iron 60 Evidence for Early Injection and Efficient Mixing of Stellar Debris in the Protosolar Nebula", "Slow-Moving Rocks Better Odds That Life Crashed to Earth from Space", "Magnetic Star-Disk Coupling in Classical T Tauri Systems", "Stardust Results in a Nutshell: The Solar Nebula was Like a Blender", "The Primordial Excitation and Clearing of the Asteroid Belt", "Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion", "Pumping of a Planetesimal Disc by a Rapidly Migrating Planet", Monthly Notices of the Royal Astronomical Society, "The primordial excitation and clearing of the asteroid beltRevisited", "A Population of Comets in the Main Asteroid Belt", "Source regions and timescales for the delivery of water to the Earth", "Uranus, Neptune, and the Mountains of the Moon", "Origin of the orbital architecture of the giant planets of the Solar System", "Jupiter may have robbed Mars of mass, new report indicates", "UCLA scientists strengthen case for life more than 3.8 billion years ago", "The Risk to Civilization From Extraterrestrial Objects and Implications of the Shoemaker-Levy 9 Comet Crash", "Neptune's capture of its moon Triton in a binary-planet gravitational encounter", "Interplanetary Weathering: Surface Erosion in Outer Space", Eos, Transactions, American Geophysical Union, "The origin and evolution of stony meteorites", "The Giant Planet Satellite and Moon Page", "Origin of the moonThe collision hypothesis", "A Jovian analogue orbiting a white dwarf star", "A Crystal Ball Into Our Solar System's Future - Giant Gas Planet Orbiting a Dead Star Gives Glimpse Into the Predicted Aftermath of our Sun's Demise", "Astronomers Found a Planet That Survived Its Star's Death - The Jupiter-size planet orbits a type of star called a white dwarf, and hints at what our solar system could be like when the sun burns out", "Numerical evidence that the motion of Pluto is chaotic", "The solar system could go haywire before the sun dies", "Tidal Heating of Io and orbital evolution of the Jovian satellites", "Improved estimate of tidal dissipation within Mars from MOLA observations of the shadow of Phobos", "Measurement and implications of Saturn's gravity field and ring mass", "Introduction to Cataclysmic Variables (CVs)", "Titan under a red giant sun: A new kind of "habitable" moon", "Planetary nebulae and the future of the Solar System", "The Potential of White Dwarf Cosmochronology", "Period of the Sun's Orbit around the Galaxy (Cosmic Year)", "When Our Galaxy Smashes Into Andromeda, What Happens to the Sun? The Solar System that we live in consists of a medium-size star (the Sun) with eight planets orbiting it. The first materials to form solid grains were the metals and various rock-forming silicates. [78], Moons of solid Solar System bodies have been created by both collisions and capture. Earth and Venus are almost the same size, while Mars is about half their size. [113] If it were only for this, Venus and Earth would probably escape incineration,[118] but a 2008 study suggests that Earth will likely be swallowed up as a result of tidal interactions with the Sun's weakly-bound outer envelope. Scientists have developed three different models to explain how planets in and out of the solar system may have formed. [124], This is a relatively peaceful event, nothing akin to a supernova, which the Sun is too small to undergo as part of its evolution. However, in the inner parts of the disk, the temperature never dropped low enough for such materials as ice or carbonaceous organic compounds to condense, so they were lacking on the innermost planets. Proplyds in the Orion Nebula. (b) NaHCO3+H2SO4Na2SO4+H2O+CO2\mathrm{NaHCO}_3+\mathrm{H}_2 \mathrm{SO}_4 \longrightarrow \mathrm{Na}_2 \mathrm{SO}_4+\mathrm{H}_2 \mathrm{O}+\mathrm{CO}_2NaHCO3+H2SO4Na2SO4+H2O+CO2 Planets of our solar system formed from the material drawn from the protostar. Step 3 of the formation of the solar system. Planets form from particles in a disk of gas and dust, colliding and sticking together as they orbit the star. and you must attribute OpenStax. In this way, our Sun came into being. The next full moon is the Crow, Crust, Sap, Sugar, and Worm Moon. While our planet is in some ways a mere speck in the vast cosmos, we have a lot of company out there. Eventually, the Sun will likely expand sufficiently to overwhelm the inner planets (Mercury, Venus, and possibly Earth) but not the outer planets, including Jupiter and Saturn. They simply have similar rotational periods. 1999-2023, Rice University. In the rising heat, the atoms collided more frequently and more violently. The inner Solar System's period of giant impacts probably played a role in the Earth acquiring its current water content (~61021kg) from the early asteroid belt. It is still moving away at a rate of almost two inches (four centimeters) per year. Direct link to Bayley Ridgeway's post if the same process that , Posted 8 years ago. The grains that condensed in the solar nebula rather quickly joined into larger and larger chunks, until most of the solid material was in the form of planetesimals, chunks a few kilometers to a few tens of kilometers in diameter. Is there any attempt at explaining why Earth and Mars rotate at the same speed? The Sun and planets began to form in a rotating cloud of nebular gas and dust. Solar Nebula. Faster moving material, on the other hand, collapsed into a flat disk revolving around the central object (Figure 14.11). Eventually, after about 800 million years, the gravitational disruption caused by galactic tides, passing stars and giant molecular clouds began to deplete the cloud, sending comets into the inner Solar System. The force of these interactions will likely push the Solar System into the new galaxy's outer halo, leaving it relatively unscathed by the radiation from these collisions. A study by Southwest Research Institute, San Antonio, Texas, published June 6, 2011 (called the Grand tack hypothesis), proposes that Jupiter had migrated inward to 1.5AU. Does it relate to gravity? HD 142666 simulation results. Co-formation from a circumplanetary disc (only in the cases of the giant planets); Formation from impact debris (given a large enough impact at a shallow angle); and, This page was last edited on 27 March 2023, at 06:10. Is any acreation in our own solar system still considered ongoing in the asteroid belt between Mars and Jupiter? The Sun's heliosphere doesn't extend quite as far. Detailed recent studies of the orbits of the planets and asteroids, however, suggest that there were more violent events soon afterward, perhaps involving substantial changes in the orbits of Jupiter and Saturn. Direct link to Jose Gurrola's post Could there be a differen, Posted 4 years ago. [88] Before 2006, students learned that our Solar System had nine planets, not eight. No planet formed in this area. Going into space is exciting enough, but we are also going back in time about 4.6 billion years! As the nebula shrinks, its rotation causes it to flatten into a disk. Terms in this set (5) Step 1 of the formation of the solar system. A careful examination of the composition of solid solar-system objects shows a striking progression from the metal-rich inner planets, through those made predominantly of rocky materials, out to objects with ice-dominated compositions in the outer solar system. are licensed under a, Observing the Sky: The Birth of Astronomy, Observations outside Earths Atmosphere, Other Worlds: An Introduction to the Solar System, Life, Chemical Evolution, and Climate Change, Cosmic Influences on the Evolution of Earth, Comets and Asteroids: Debris of the Solar System, The Origin and Fate of Comets and Related Objects, Cosmic Samples and the Origin of the Solar System, Sources of Sunshine: Thermal and Gravitational Energy, Mass, Energy, and the Theory of Relativity, Using Spectra to Measure Stellar Radius, Composition, and Motion, Variable Stars: One Key to Cosmic Distances, The Birth of Stars and the Discovery of Planets outside the Solar System, The HR Diagram and the Study of Stellar Evolution, Evidence That Planets Form around Other Stars, Planets beyond the Solar System: Search and Discovery, Exoplanets Everywhere: What We Are Learning, Evolution from the Main Sequence to Red Giants, Evolution of Massive Stars: An Explosive Finish, Pulsars and the Discovery of Neutron Stars, Active Galaxies, Quasars, and Supermassive Black Holes, Supermassive Black Holes: What Quasars Really Are, Quasars as Probes of Evolution in the Universe, The Evolution and Distribution of Galaxies, Galaxy Mergers and Active Galactic Nuclei, The Formation and Evolution of Galaxies and Structure in the Universe, The Search for Extraterrestrial Intelligence, How to Study for an Introductory Astronomy Class, Physical and Orbital Data for the Planets, The Nearest Stars, Brown Dwarfs, and White Dwarfs. The formation of the solar system is a challenging puzzle for modern astronomy and a terrific tale of extreme forces operating over immense timescales. [123], Gradually, the hydrogen burning in the shell around the solar core will increase the mass of the core until it reaches about 45% of the present solar mass. [51], The outer edge of the terrestrial region, between 2 and 4AU from the Sun, is called the asteroid belt. Giant impacts at this stage may have stripped Mercury of part of its mantle and crust, reversed the rotation of Venus, and broke off part of Earth to create the Moon (all events we discussed in other chapters). The planets are of two different types. Click here to download this video (1280x720, 14 MB, video/mp4). The boundary where the solar wind is abruptly slowed by pressure from interstellar gases is called the termination shock. In all of these cases of transfer of angular momentum and energy, the angular momentum of the two-body system is conserved. Scientists estimate that the Solar System is 4.6billion years old. Its speed is about 220km/s. [59][60] In contrast, comets from the Kuiper belt or farther regions delivered not more than about 6% of Earth's water. As far as age is concerned, we discussed that radioactive dating demonstrates that some rocks on the surface of Earth have been present for at least 3.8 billion years, and that certain lunar samples are 4.4 billion years old. Its inner edge would have been just beyond the orbits of Uranus and Neptune, which were in turn far closer to the Sun when they formed (most likely in the range of 1520AU), and in 50% of simulations ended up in opposite locations, with Uranus farther from the Sun than Neptune. Water delivered to Earth. This caused Jupiter to move slightly inward. These clumps smashed into one another, forming larger and larger objects. The comets visible to us today are merely the tip of the cosmic iceberg (if youll pardon the pun). Each of the planets in our Solar System is unique. [48] Orbital resonances with Jupiter and Saturn are particularly strong in the asteroid belt, and gravitational interactions with more massive embryos scattered many planetesimals into those resonances. The helium-fusing stage will last only 100million years. [11] Over about 100,000 years,[9] the competing forces of gravity, gas pressure, magnetic fields, and rotation caused the contracting nebula to flatten into a spinning protoplanetary disc with a diameter of about 200AU[11] and form a hot, dense protostar (a star in which hydrogen fusion has not yet begun) at the centre. The outer moons of the giant planets tend to be small and have eccentric orbits with arbitrary inclinations. An astronomical unit, or AU, is the average distance between the Earth and the Sun, or about 150 million kilometres. Some planetesimals still survive today as comets and asteroids. Step 4 of the formation of the solar system. nuclear fusion. Initially, this white dwarf may be 100times as luminous as the Sun is now. [45][46], The planets were originally thought to have formed in or near their current orbits. One astronomical unit (or AU) is the distance from the Sun to Earth, or about 93 million miles (150 million kilometers).

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