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Solar Nebula

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Image:M42proplyds.jpg Orion Nebula.html" title="Meaning of right right|thumb|A planetary disc forming in the [[Orion Nebula..html" title="Meaning of thumb|A planetary disc forming in the [[Orion Nebula">right|thumb|A planetary disc forming in the [[Orion Nebula.">thumb|A planetary disc forming in the [[Orion Nebula">right|thumb|A planetary disc forming in the [[Orion Nebula. In cosmogony, the '''solar nebula''' is the gaseous cloud from which Earth's solar system is believed to have formed. This '''nebular hypothesis''' was first proposed in 1755 by Immanuel Kant (this has been contested, see Emanuel Swedenborg), who argued that nebulae slowly rotate, gradually collapsing and flattening due to gravity and eventually forming stars and planets. A similar model was proposed in 1796 by Pierre-Simon Laplace.

Overview of the Solar Nebula Theory
The theory maintains that the solar system began as a large (about 100 Astronomical Unit AU diameter and 2-3 times the current mass of the Sun), roughly spherical cloud of very cold interstellar gas, the '''solar nebula''', part of a larger molecular cloud. The nebula was just dense enough to begin contracting under the force of its own gravity, and its collapse may have been initiated by a pressure wave from a nearby event (such as a shock wave from a supernova) pushing into the molecular cloud. The composition of the solar nebula was the same as the composition of the sun today: about 98% (by mass) hydrogen and helium present since the Big Bang, and 2% heavier elements created by earlier generations of stars which died and ejected them back into interstellar space (see nucleosynthesis). Once begun, the gravitational contraction of the solar nebula accelerates slowly but inevitably. As it collapses, three physical processes shape the nebula: it heats up, it spins up, and it flattens. The nebula heats up because atoms move more quickly as they fall deeper into the gravitational well and become density denser, colliding more frequently (gravitational potential energy is converted to kinetic energy of the atoms, or thermal energy). While initially imperceptible, the solar nebula had some small amount of net rotation (angular momentum), and because angular momentum is conserved, the nebula must rotate more quickly as it shrinks in size. The nebula must also flatten into a disk, called a protoplanetary disk, as collisions and mergers of blobs of gas average out their motions in favor of the direction of the net angular momentum. At the center, the solar nebula's gravity accumulates an increasingly dense protostar protosun. During the process of planet formation in the disk, the protosun gradually compacts further, until after about 10-50 million years, it finally reaches the conditions of temperature and pressure needed to initiate hydrogen nuclear fusion, and becoming the Sun. As is typical of a young star (a T Tauri star), the young Sun produces a solar wind much stronger than the present solar wind, which eventually blows the remaining gases out of the disk, and largely ending the accretion process (particularly for the gas giant jovians). The gas in the protoplanetary disk, meanwhile, gradually cools from the gravitational heating of its collapse, and as it cools, dust (metals and silicates) and ice (hydrogen compounds such as water, methane, and ammonia) grains condensation condense out of the gas (solidify). These grains gently bump into neighboring grains (collide) and stick together electrostatically, beginning the accretion process. Gas atoms and molecules are present in great abundance, but cannot be accreted, because they are moving too quickly to be held electrostatically. Hydrogen and helium, 98% of the mass of the disk, remain gaseous throughout the solar nebula, never condensing. Initially-microscopic 'seeds' of solid material gradually increase in size and become '''planetesimals''' (pieces of planets). As they grow larger, in fact, they grow more quickly: larger objects have more surface area for other grains to bump against and stick to, and as planetesimals become significantly massive, their gravity helps bring more grains into contact. Planetesimals have a hard time growing above a few hundred kilometers in size, however. With significant mass, planetesimals now have gravitational interactions with each other, modifying their orbits from circular to more eccentric ones, particularly so for the lower mass planetesimals. With crossing orbits, planetesimals now sometimes collide violently, often shattering into smaller pieces again. (Asteroids are understood to be left-over planetesimals, now gradually grinding each other down into smaller and smaller bits. Meteorites are therefore samples of planetesimals and give us a great deal of information about the formation of our solar system. Primitive-type meteorites are chunks of shattered low-mass planetesimals, where no gravitational differentiation took place, while processed-type meteorites are chunks from shattered massive planetesimals.) Only the largest of planetesimals survive these high-energy collisions with lower mass planetesimals, and can continue to grow. The temperature in the protoplanetary disk was not uniform, however, and this is key to understanding the differentiation between terrestrial and jovian planet formation. Inside the '''frost line''', the temperature is too high (above 150 kelvin K) for hydrogen compounds to condense: they remain gaseous. The only grains available for accretion, then, are the heavier metal and silicate dust grains. Thus the planetesimals in this region are composed entirely of rock and metal, such as the asteroids, and make up the terrestrial planets. In this formation process, terrestrial planets only get moons by capturing them (Mars' two tiny asteroid moons) or giant impact theory giant impacts (Earth's Moon). Outside the frost line, hydrogen compounds such as water, methane and ammonia are able to solidify into 'ice' grains, and accrete. Rock and metal grains are also available, but are vastly outnumbered (and outweighed) by the hydrogen compounds, which are much more abundant everywhere. Thus the planetesimals in this region are icy bodies with small amounts of rock and metal mixed in. The Kuiper Belt and Oort Cloud objects, comets, Neptune's huge moon Triton, and probably Pluto and its moon Charon (moon) Charon, are all examples of these 'dirty snowball' planetesimals. Because there is so much more solid material available, and collisions are less frequent and lower velocity (being in much larger orbits), the largest of these planetesimals grow so massive their gravity begins to collect and retain helium and then hydrogen gases. Once that starts, they grow rapidly, as hydrogen and helium are 98% of the disk, and collecting these gases increases their mass and consequently the size of their gravitational net. Soon these jovian planetesimals are nothing like the icy bodies they came from, but are dominated by the hydrogen and helium gas they have captured, huge gaseous clouds with dense terrestrial-like cores. These jovian gas balls then, in close analogy to the solar system itself, gradually collapse gravitationally, heating up, rotating more quickly, and flattening. The natural satellite moons of the gas giant jovian planets are formed in an analogous process to the planets themselves, coalescing from condensed grains in the disks which formed as the gas giant protoplanet collapsed. This explains why jovian planets all have many moons and rings. The growth of the jovians ends when the young Sun's strong solar wind blows the remaining hydrogen and helium gas out of the disk and into interstellar space. Finally, long after the solar wind cleared the gas out of the disk, the jovian planets (particularly Jupiter and Neptune) gradually swept the disk clean of leftover planetesimals, either by slinging them in the distant outer reaches of the Oort Cloud (as far as 50,000 astronomical unit AU), or continually nudging their orbits into collisions with other planets (or into more stable orbits like the asteroid belt). This period of '''heavy bombardment''' lasts several hundred million years, and is evident in the cratering still visible on geologically dead bodies of the solar system. Planetesimals impacting Earth are thought to have brought the Earth its water and other hydrogen compounds. Although not widely accepted, some believe life itself may have been deposited on Earth in this way (known as the panspermia hypothesis). Jupiter's regular gravitational interactions (see orbital resonance) are also responsible for preventing the material which once inhabited the asteroid belt from accreting into another probably sizable terrestrial planet. Most of that material has long since been thrown into eccentric orbits and collided with something else; the total mass of the asteroid belt is now less than a tenth of Earth's Moon! The nebular theory effectively explains all the major features of our solar system: # regular motions of the planets and moons (all revolve in the same plane, in same direction the sun rotates, and nearly all rotate in the same direction too) # all major differences between terrestrial and jovian planets (mass, distance from sun, composition, moon and ring systems) # small bodies (asteroids and comets, both short- and long-period) # exceptions to the trends (Earth's massive moon and axial tilt, Venus's backwards rotation/axial tilt, Uranus' axial tilt) The current challenges for the nebular theory include explaining: # missing mass in Kuiper Belt # capture process for Triton_(moon) Triton # discovered ''hot Jupiter'' extrasolar planet exoplanets # discovered exoplanets in binary and trinary stellar systems

The meaning of ''accretion''
Use of the term accretion disk for the protoplanetary disk leads to confusion over the planetary accretion process. The protoplanetary disk is sometimes referred to as an accretion disk, because while the young T Tauri star T Tauri-like protosun is still contracting, gaseous material may still be falling onto, accreting on, its surface from the disk's inner edge. However, that meaning should not to be confused with the process of accretion forming the planets. In this context, accretion refers to the process of cooled, solidified grains of dust and ice orbiting the protosun in the protoplanetary disk, colliding and sticking together and gradually growing, up to and including the high energy collisions between sizable planetesimals. If that weren't confusing enough, the jovians, probably had accretion disks of their own, in the first meaning of the word. The clouds of captured hydrogen and helium gas contract, spin up, flatten, and deposit gas onto the surface of each jovian protoplanet, while solid grains within that disk accrete into planetesimals and eventually forming the jovian moons.

History of Solar System Formation Hypotheses
During the late-19th century the Kant-Laplace nebular hypothesis was criticized by James Clerk Maxwell, who showed that if matter of the known planets had once been distributed around the Sun in the form of a disk, forces of differential rotation would have prevented the condensation of individual planets. Another objection was that the Sun possesses less angular momentum than the Kant-Laplace model indicated. For several decades, most astronomers preferred the ''near-collision hypothesis'', in which the planets were considered to have been formed due to the approach of some other star to the Sun. This near-miss would have drawn large amounts of matter out of the Sun and the other star by their mutual tidal forces, which could have then condensed into planets. Objections to the near-collision hypothesis were also raised and, during the 1940s, the nebular model was improved such that it became broadly accepted. In the modified version, the mass of the original protoplanet was assumed to be larger, and the angular momentum discrepancy was attributed to magnetic forces. That is, the young Sun transferred some angular momentum to the protoplanetary disk and planetesimals through Alven waves, as is understood to occur in T Tauri stars. The refined nebular model was developed based entirely on observations of our own solar system, because it was the only one known until the mid 1990's. It was not confidently assumed to be widely applicable to other planetary systems, although scientists were anxious to test the nebular model by finding or protoplanetary disks or even planets around other stars, so-called extrasolar planets. Stellar nebula or protoplanetary disks have now been observed in the Orion nebula, and other star-forming regions, by astronomers using the Hubble Space Telescope. Some of these are as large as 1000 AU in diameter. And as of January 2006, the discovery of over 180 extrasolar planet exoplanets has turned up many surprises, and the nebular model must be revised to account for these discovered planetary systems, or new models considered. There is no consensus on how to explain the observed 'hot Jupiters,' but one leading idea is that of '''planetary migration'''. This idea is that planets must be able to migrate from their initial orbit to one nearer their star, by any of several possible physical processes, such as orbital friction while the protoplanetary disk is still full of hydrogen and helium gas. In recent years, an alternative model for the formation of the solar system, the Capture Theory, has been developed which has explained features of the solar system not explained by the Solar Nebula Theory. This hypothesis has been published in the following references: *M M Woolfson 1969, Rep. Prog. Phys. 32 135-185 *M M Woolfson 1999, Mon. Not. R. Astr. Soc.304, 195-198.

See also
*History of Earth *Asteroid Belt, Kuiper Belt, and Oort Cloud *Bok globule, Herbig-Haro object *T Tauri star Category:Sun Category:Solar System Category:Planetary systems Category:Planets Category:Nebulae Category:Unclassified nebulae Category:History of astronomy de:Sonnennebel es:Nebulosa protosolar fr:NÃ©buleuse solaire it:Nebulosa solare pt:Nebulosa solar sk:SlneÄ?nÃ¡ hmlovina see Solar nebula

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