what is the formation of a solar system from a nebula?
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It appears that the question period has expired.  If you have received an answer that meets your needs, please choose one of those as a 'best answer.'  If you haven't received a good answer for your question, you may want to consider the following,\n\n1) Re-post your question.  Newer questions get more activity on Yahoo! Answers than old ones.\n2) If you do re-post your question, consider why it wasn't answered the first time.  Could it be more specific?  Could it be worded better? Were there grammatical or spelling errors? Was it in the best category?\n\nIf it doesn't seem likely that re-posting your question will help you, then here's a listing of my favorite 'answer sites'.  Maybe one of them will help you.\n\nAnswers.com http://www.answers.com/\nBartleby http://www.bartleby.com/\nYahoo Reference http://education.yahoo.com/reference/\nHowStuffWorks http://www.howstuffworks.com/\nWikipedia http://en.wikipedia.org/wiki/Main_Page\n\nSince I really haven't answered your question, it is not necessary to give me any points.  Regards.
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A meteoroid is a relatively small (sand- to boulder-sized) fragment of debris in the Solar System. When entering a planet's atmosphere, the meteoroid heats up and partially or completely vaporizes. The gas along the path of the meteoroid becomes ionized and glows. The trail of glowing vapor is called a meteor, or shooting star. If any portion of the meteor survives to reach the ground, it is then referred to as a meteorite.79% of meteorites are Chondrites - balls of mafic minerals with small grain size indicative of rapid cooling. In most chondrites small spherules, called chondrules, can be found. Chondrites are typically about 4.6 billion years old and are thought to represent material from the asteroid belt. It is unknown how they formed. Carbonaceous Chondrites, thought to be unaltered solar nebula material, constitute about 5% of meteorites and contain small amounts of organic materials, including amino acids. Also, presolar grains are identified in carbonaceous chondrites. The isotope ratios of carbonaceous chondrites are similar to those of the Sun.Achondrites are similar to terrestrial mafic igneous rocks and sometimes are brecciated. Achondrites constitute about 8% of the incoming material and are thought to represent crustal material of larger asteroids. About 6% of meteorites are iron meteorites with intergrowths of iron-nickel alloys, such as kamacite. Unlike chondrites, the crystals are large and appear to represent slow crystallization. Iron meteorites are thought to be the core material of one or more planets that subsequently broke up. Stony iron meteorites constitute the remaining 2%. They are a mixture of iron-nickel and silicate minerals. They are thought to have originated in the boundary zone above the core regions where iron meteorites originated. A small number of meteorites belong to additional groups or subgroups with unique chemical characteristics relative to other members of the larger groups, such as Lunar meteorites or Martian meteorites.
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It was formed from the ring of dust and debris orbiting the sun when the sun gained enough mass to start the fusion process.  It was formed in the same way and at the same time as all the other planets.
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The comets we can see are believed to have formed at various stages in the formation of the solar nebula (proto solar system), and depending on how well preserved they are, can yield clues on the nebula's molecular composition in those stages.  (Paraphrased from ref.)
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The theory in question is called Nebular Theory, and while (like much of modern science) it is only a theory, it is a theory based on solid evidence and calculus, rather than educated guesswork. While nebular theory is difficult to compress into a single paragraph for easy explanation, suffice it to say that solar nebulae comprised of a sun surrounded by a cloud of particles can be observed in space; and that these clouds tend to condense into solid masses and protoplanets, due to the natural gravity of the component particles.
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Actually, there aren't as many solar systems as there are stars. Unlike our star, most stars are gravitationally bound to other stars, forming binary stars. So, most solar systems have multiple stars.
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Our solar system is tucked into a corner of the galaxy where the stars are scattered far from each other.\n\nThe stars are denser closer to its centre.
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Up until the time that the earth started forming, the sun had time (I can't speculate, but probably a few billion years) to begin it's nuclear fusion and begin burning. Sol would have been surrounded by thick clouds of dust, ice and gases (see planetary nebulae). The particles of gas and dust began to clump together into larger and larger pieces and began spinning around the sun either falling in their maintainable orbits or falling back into the sun. These clumps continued to come together and the planets were formed in their respective distances around the sun.
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Fifteen minutes since you asked your question and nobody has taken a shot at an answer. That's a pretty good indication that there isn't one, neither a known birth-place nebula for Sirius nor an answer. In researching your question, I did find a photo of the Sirius system and a nebula is clearly visible, but apparently it has no specific name or designation.\n\nhttp://www.solstation.com/stars/sirius2.htm
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Meteors, Asteroids, comets, Nebula's (gaseous clouds where stars are born) photon stars, Neutron stars, pulsars, quasars, black holes, regular starts like out sun, galactic clusters, spiral galaxies, bar galaxies, moons, and planets, and solar systems.\n\nmetaphsyics1221, black holes are not considered to be a fact, they actually have photos of them
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Earth is the third planet from the Sun. It is the largest of the solar system's terrestrial planets, and the only planetary body that modern science confirms as harboring life. Scientific evidence indicates that the planet formed around 4.57 billion (4.57×109) years ago, and shortly thereafter (4.533 billion years ago) acquired its single natural satellite, the Moon.
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Solar winds,nebulars,planets,milky way,\nmeteors,comets,darkness,\nsolar systems,black holes,\npulsars,nova's,super nova's.\nsatalites,Asteroids.\nspiral galaxys,oval galaxys\nhelp u.
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A Planetary Nebula is a misleading name.  At the end of a lower mass star's life (for stars up to about 8 times the mass of the sun), the star puffs up, and loses the outer layers of gas surrounding it.  All this gas goes out into space where it can be seen as what we call a planetary nebula.\n\nOriginally the word "nebula" was applied to any astronomical object that was not a star or a memeber of our solar system (planets, asteroids etc), the word essentially means "cloud."\n\nAs telescopes got better people started to find many different types of nebulae. A Spiral Nebula looks like, well a spiral, today we know that these are spiral galaxies.  Planetary Nebula were named because the looked round, and a number of them had the same greenish color that Uranus had been seen to have by Hershel.
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The sun is only about 4.5 billion years old.  The cloud of gas and dust that it formed out of was probably huge, though.
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It has to do with the formation of the planets from the solar nebula based on the "nebular hypothesis."  That is why they are all on different orbits.
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Since the diameter of the sun is 864,000 miles and the diameter of a typical basketball is about 9½ inches (they vary from 9¼ to 9½ inches), if we divide 864,000 miles by 9½ inches, we discover that in our model 1 inch represents roughly 91,000 miles. To see how everything else fits into our model we need only divide any other dimensions of our solar system by 91,000. For example, Mercury, on the average, is about 36,250,000 miles from the sun. If we divide 36,250,000 by 91,000 we find that in our model it is roughly 398 inches-or about 33 feet away from the basketball. And, if we divide Mercury' s diameter of 3050 miles by 91,000, we find that the Mercury in our model is just .034 inches wide-about 1/30 inch. This is smaller than a typical BB. \n\nIf you know your stride (mine is about 2½ feet) you can put the basketball on the ground and pace this off. Better yet, if you have access to a football field at a local high school or college, place a basketball on one of the goal lines and walk out to the 11 yard line. This is where Mercury is.\n\nScientists believe that the solar system was formed when a cloud of gas and dust in space was disturbed, maybe by the explosion of a nearby star (called a supernova). This explosion made waves in space which squeezed the cloud of gas and dust. Squeezing made the cloud start to collapse, as gravity pulled the gas and dust together, forming a solar nebula. Just like a dancer that spins faster as she pulls in her arms, the cloud began to spin as it collapsed. Eventually, the cloud grew hotter and denser in the center, with a disk of gas and dust surrounding it that was hot in the center but cool at the edges. As the disk got thinner and thinner, particles began to stick together and form clumps. Some clumps got bigger, as particles and small clumps stuck to them, eventually forming planets or moons . Near the center of the cloud, where planets like Earth formed, only rocky material could stand the great heat. Icy matter settled in the outer regions of the disk along with rocky material, where the giant planets like Jupiter formed. As the cloud continued to fall in, the center eventually got so hot that it became a star, the Sun, and blew most of the gas and dust of the new solar system with a strong stellar wind. By studying meteorites, which are thought to be left over from this early phase of the solar system, scientists have found that the solar system is about 4,600 million years old!
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Star formation occurs in molecular clouds, large regions of high density in the interstellar medium (though still less dense than the inside of an earthly vacuum chamber). Star formation begins with gravitational instability inside those clouds, often triggered by shockwaves from supernovae or collision of two galaxies (as in a starburst galaxy). High mass stars powerfully illuminate the clouds from which they formed. One example of such a nebula is the Orion Nebula.\n\nStars spend about 90% of their lifetime fusing hydrogen to produce helium in high-temperature and high-pressure reactions near the core. Such stars are said to be on the main sequence.\n\nSmall stars (called red dwarfs) burn their fuel very slowly and last tens to hundreds of billions of years. At the end of their lives, they simply become dimmer and dimmer, fading into black dwarfs. However, since the lifespan of such stars is greater than the current age of the universe (13.7 billion years), no black dwarfs exist yet.\n\nAs most stars exhaust their supply of hydrogen, their outer layers expand and cool to form a red giant. In about 5 billion years, when the Sun is a red giant, it will be so large that it will consume both Mercury and Venus. Eventually the core is compressed enough to start helium fusion, and the star heats up and contracts. Larger stars will also fuse heavier elements, all the way to iron, which is the end point of the process. Since iron nuclei are more tightly bound than any heavier nuclei, they cannot be fused to release energy. Likewise, since they are more tightly bound than all lighter nuclei, energy cannot be released by fission. In old, very massive stars, a large core of inert iron will accumulate in the center of the star.\n\nAn average-size star will then shed its outer layers as a planetary nebula. The core that remains will be a tiny ball of degenerate matter not massive enough for further fusion to take place, supported only by degeneracy pressure, called a white dwarf. These too will fade into black dwarfs over very long stretches of time.\n\n \nThe Crab Nebula, remnants of a supernova which occurred around 1050 AD.In larger stars, fusion continues until an iron core accumulates that is too large to be supported by electron degeneracy pressure. This core will suddenly collapse as its electrons are driven into its protons, forming neutrons and neutrinos in a burst of inverse beta decay. The shockwave formed by this sudden collapse causes the rest of the star to explode in a supernova. Supernovae are so bright that they may briefly outshine the star's entire home galaxy. When they occur within the Milky Way, supernovae have historically been observed by naked-eye observers as "new stars" where none existed before. Eventually, most of the matter in a star is blown away by the explosion (forming nebulae such as the Crab Nebula) and what remains will be a neutron star (sometimes a pulsar or X-ray burster) or, in the case of the largest stars, a black hole.\n\nThe blown-off outer layers of dying stars include heavy elements which may be recycled during new star formation. These heavy elements allow the formation of rocky planets. The outflow from supernovae and the stellar wind of large stars play an important part in shaping the interstellar medium.