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The Solar System is the gravitationally bound system of the Sun and the masses that orbit it, most prominently its eight planets, of which Earth is one.
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The system formed about 4.6 billion years ago when a dense region of a molecular cloud collapsed, creating the Sun and a protoplanetary disc from which the orbiting bodies assembled.
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Inside the Sun's core hydrogen is fused into helium for billions of years, releasing energy which is over even longer periods of time emitted through the Sun's outer layer, the photosphere.
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This creates the heliosphere and a decreasing temperature gradient across the Solar System.
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The mass of the Solar System is by 99.86% almost completely made up of the Sun's mass.
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The next most massive objects of the system are the eight planets, which by definition dominate the orbits they occupy.
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Closest to the Sun in order of increasing distance are the four terrestrial planets – Mercury, Venus, Earth and Mars.
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These are the planets of the inner Solar System.
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Earth and Mars are the only planets in the Solar System which orbit within the Sun's habitable zone, in which the sunlight can make surface water under atmospheric pressure liquid.
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Beyond the frost line at about five astronomical units (AU), are two gas giants – Jupiter and Saturn – and two ice giants – Uranus and Neptune.
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These are the planets of the outer Solar System.
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Jupiter and Saturn possess nearly 90% of the non-stellar mass of the Solar System.
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Additionally to the planets there are in the Solar System other planetary-mass objects, but which do not dominate their orbits, such as dwarf planets and planetary-mass moons.
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Dwarf planets there are generally nine Solar System objects identified as such: Ceres, Orcus, Pluto, Haumea, Quaoar, Makemake, Gonggong, Eris, and Sedna.
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Natural satellites, which are commonly called 'moons', can be found throughout the Solar System and in sizes from planetary-mass moons to much less massive moonlets at their smallest.
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The largest two moons (Ganymede of Jupiter and Titan of Saturn) are larger than the smallest planet (Mercury), while the seven most massive, which includes Earth's Moon, are more massive and larger than any of the dwarf planets.
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Less massive than these planetary-mass objects are the vast number of small Solar System bodies, such as asteroids, comets, centaurs, meteoroids, and interplanetary dust clouds.
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All dwarf planets and many of the smaller bodies are within the asteroid belt (between Mars's and Jupiter's orbit) and the Kuiper belt (just outside Neptune's orbit).
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The Solar System is within the heliosphere constantly flooded by the charged plasma particles of the solar wind, which forms with the interplanetary dust, gas and cosmic rays between the bodies of the Solar System an interplanetary medium.
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At around 70–90 AU from the Sun, the solar wind is halted by the interstellar medium, resulting in the heliopause and the border of the interplanetary medium to interstellar space.
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Further out somewhere beyond 2,000 AU from the Sun extends the outermost region of the Solar System, the theorized Oort cloud, the source for long-period comets, stretching to the edge of the Solar System, the edge of its Hill sphere, at 178,000–227,000 AU (2.81–3.59 ly), where its gravitational potential becomes equal...
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The Solar System currently moves through a cloud of interstellar medium called the Local Cloud.
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The closest star to the Solar System, Proxima Centauri, is 269,000 AU (4.25 ly) away.
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Both are within the Local Bubble, a relatively small 1,000 light-years (ly) wide region of the Milky Way.
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Definition The Solar System includes the Sun and all objects that are bound to it by gravity and orbit it.
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The International Astronomical Union describes the Solar System as all objects that are bound by the gravity of the Sun, the Sun itself, its eight planets, and the other celestial bodies which orbit it.
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26
NASA describes the Solar System as a planetary system, including the Sun and all objects that orbit it.
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When not used as a proper noun and written without capitalization, "solar system" may refer to either the Solar System itself or any system reminiscent of the Solar System.
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Formation and evolution Past The Solar System formed at least 4.568 billion years ago from the gravitational collapse of a region within a large molecular cloud.
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29
This initial cloud was likely several light-years across and probably birthed several stars.
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As is typical of molecular clouds, this one consisted mostly of hydrogen, with some helium, and small amounts of heavier elements fused by previous generations of stars.
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As the pre-solar nebula collapsed, conservation of angular momentum caused it to rotate faster.
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The center, where most of the mass collected, became increasingly hotter than the surroundings.
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As the contracting nebula spun faster, it began to flatten into a protoplanetary disc with a diameter of roughly 200 AU and a hot, dense protostar at the center.
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34
The planets formed by accretion from this disc, in which dust and gas gravitationally attracted each other, coalescing to form ever larger bodies.
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35
Hundreds of protoplanets may have existed in the early Solar System, but they either merged or were destroyed or ejected, leaving the planets, dwarf planets, and leftover minor bodies.
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In the inner Solar System, heat from the accretion process exceeded the boiling point of hydrocarbon molecules for the first million years, leading to low carbon content for the inner planets.
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The boundary for this process has been dubbed the soot line.
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As the Solar System disk cooled, this line moved inward and now lies within Earth's orbit around the Sun.
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Material other than metals and silicates, due to their higher boiling points, could not persist in solid form.
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Here planets formed that are mainly rocky, which are Mercury, Venus, Earth, and Mars.
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Because these refractory materials only comprised a small fraction of the solar nebula, the terrestrial planets could not grow very large.
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The giant planets (Jupiter, Saturn, Uranus, and Neptune) formed further out, beyond the frost line, the point between the orbits of Mars and Jupiter where material is cool enough for volatile icy compounds to remain solid.
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The ices that formed these planets were more plentiful than the metals and silicates that formed the terrestrial inner planets, allowing them to grow massive enough to capture large atmospheres of hydrogen and helium, the lightest and most abundant elements.
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Leftover debris that never became planets congregated in regions such as the asteroid belt, Kuiper belt, and Oort cloud.
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Within 50 million years, the pressure and density of hydrogen in the center of the protostar became great enough for it to begin thermonuclear fusion.
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As helium accumulates at its core, the Sun is growing brighter; early in its main-sequence life its brightness was 70% that of what it is today.
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The temperature, reaction rate, pressure, and density increased until hydrostatic equilibrium was achieved: the thermal pressure counterbalancing the force of gravity.
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At this point, the Sun became a main-sequence star.
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Solar wind from the Sun created the heliosphere and swept away the remaining gas and dust from the protoplanetary disc into interstellar space.
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Following the dissipation of the protoplanetary disk, the Nice model proposes that gravitational encounters between planetesimals and the gas giants caused each to migrate into different orbits.
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This led to dynamical instability of the entire system, which scattered the planetesimals and ultimately placed the gas giants in their current positions.
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During this period, the grand tack hypothesis suggests that a final inward migration of Jupiter dispersed much of the asteroid belt, leading to the Late Heavy Bombardment of the inner planets.
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Present and future The Solar System remains in a relatively stable, slowly evolving state by following isolated, gravitationally bound orbits around the Sun.
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Although the Solar System has been fairly stable for billions of years, it is technically chaotic, and may eventually be disrupted.
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There is a small chance that another star will pass through the Solar System in the next few billion years.
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Although this could destabilize the system and eventually lead millions of years later to expulsion of planets, collisions of planets, or planets hitting the Sun, it would most likely leave the Solar System much as it is today.
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The Sun's main-sequence phase, from beginning to end, will last about 10 billion years for the Sun compared to around two billion years for all other subsequent phases of the Sun's pre-remnant life combined.
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The Solar System will remain roughly as it is known today until the hydrogen in the core of the Sun has been entirely converted to helium, which will occur roughly 5 billion years from now.
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This will mark the end of the Sun's main-sequence life.
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At that time, the core of the Sun will contract with hydrogen fusion occurring along a shell surrounding the inert helium, and the energy output will be greater than at present.
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The outer layers of the Sun will expand to roughly 260 times its current diameter, and the Sun will become a red giant.
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Because of its increased surface area, the surface of the Sun will be cooler (2,600 K (4,220 °F) at its coolest) than it is on the main sequence.
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The expanding Sun is expected to vaporize Mercury as well as Venus, and render Earth and Mars uninhabitable (possibly destroying Earth as well).
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Eventually, the core will be hot enough for helium fusion; the Sun will burn helium for a fraction of the time it burned hydrogen in the core.
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The Sun is not massive enough to commence the fusion of heavier elements, and nuclear reactions in the core will dwindle.
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Its outer layers will be ejected into space, leaving behind a dense white dwarf, half the original mass of the Sun but only the size of Earth.
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The ejected outer layers may form a planetary nebula, returning some of the material that formed the Sun – but now enriched with heavier elements like carbon – to the interstellar medium.
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General characteristics Astronomers sometimes divide the Solar System structure into separate regions.
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The inner Solar System includes Mercury, Venus, Earth, Mars, and the bodies in the asteroid belt.
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The outer Solar System includes Jupiter, Saturn, Uranus, Neptune, and the bodies in the Kuiper belt.
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Since the discovery of the Kuiper belt, the outermost parts of the Solar System are considered a distinct region consisting of the objects beyond Neptune.
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Composition The principal component of the Solar System is the Sun, a G-type main-sequence star that contains 99.86% of the system's known mass and dominates it gravitationally.
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The Sun's four largest orbiting bodies, the giant planets, account for 99% of the remaining mass, with Jupiter and Saturn together comprising more than 90%.
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The remaining objects of the Solar System (including the four terrestrial planets, the dwarf planets, moons, asteroids, and comets) together comprise less than 0.002% of the Solar System's total mass.
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The Sun is composed of roughly 98% hydrogen and helium, as are Jupiter and Saturn.
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A composition gradient exists in the Solar System, created by heat and light pressure from the early Sun; those objects closer to the Sun, which are more affected by heat and light pressure, are composed of elements with high melting points.
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Objects farther from the Sun are composed largely of materials with lower melting points.
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The boundary in the Solar System beyond which those volatile substances could coalesce is known as the frost line, and it lies at roughly five times the Earth's distance from the Sun.
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Orbits The planets and other large objects in orbit around the Sun lie near the invariable plane of the Solar System, as does Earth's orbit, known as the ecliptic, and most closely the orbit of Jupiter, with an inclination to it of 0.3219°.
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Smaller icy objects such as comets frequently orbit at significantly greater angles to this plane.
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Most of the planets in the Solar System have secondary systems of their own, being orbited by natural satellites called moons.
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All of the largest natural satellites are in synchronous rotation, with one face permanently turned toward their parent.
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The four giant planets have planetary rings, thin discs of tiny particles that orbit them in unison.
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As a result of the formation of the Solar System, planets and most other objects orbit the Sun in the same direction that the Sun is rotating.
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That is, counter-clockwise, as viewed from above Earth's north pole.
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There are exceptions, such as Halley's Comet.
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Most of the larger moons orbit their planets in prograde direction, matching the direction of planetary rotation; Neptune's moon Triton is the largest to orbit in the opposite, retrograde manner.
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Most larger objects rotate around their own axes in the prograde direction relative to their orbit, though the rotation of Venus is retrograde.
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To a good first approximation, Kepler's laws of planetary motion describe the orbits of objects around the Sun.
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These laws stipulate that each object travels along an ellipse with the Sun at one focus, which causes the body's distance from the Sun to vary over the course of its year.
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A body's closest approach to the Sun is called its perihelion, whereas its most distant point from the Sun is called its aphelion.
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With the exception of Mercury, the orbits of the planets are nearly circular, but many comets, asteroids, and Kuiper belt objects follow highly elliptical orbits.
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Kepler's laws only account for the influence of the Sun's gravity upon an orbiting body, not the gravitational pulls of different bodies upon each other.
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On a human time scale, these perturbations can be accounted for using numerical models, but the planetary system can change chaotically over billions of years.
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The angular momentum of the Solar System is a measure of the total amount of orbital and rotational momentum possessed by all its moving components.
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Although the Sun dominates the system by mass, it accounts for only about 2% of the angular momentum.
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The planets, dominated by Jupiter, account for most of the rest of the angular momentum due to the combination of their mass, orbit, and distance from the Sun, with a possibly significant contribution from comets.
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Distances and scales The radius of the Sun is 0.0047 AU (700,000 km; 400,000 mi).
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Thus, the Sun occupies 0.00001% (1 part in 107) of the volume of a sphere with a radius the size of Earth's orbit, whereas Earth's volume is roughly 1 millionth (10−6) that of the Sun.
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