How is it that heavier elements mangaged to escape the sun's core during formation, resulting in planets?

Question

You would think that lighter elements would have been thrown out, and the sun would be made of the higher density elements then the throw out one's. Was the fusion repulsive to these elements for some universal principle cause?

Answer 1

The heavier elements did not escape the sun's core at all. Actually,~99% of the heavy elements that comprised the pre-solar system nebula are now residing in the mass of the Sun. (This is what is meant by the "metalicity" of a given star.) The 1% or so of the heavy elements that had sufficient angular momentum to escape collapse into the Sun's gravity well are now orbiting our Sun in the form of planets. Angular momentum is the only known force that can cancel the gravitational pull of planet sized objects and keep them from falling into the Sun. Thus we have planets, and moons, for that manner.

Answer 2

The Sun did not "throw out" any mass as it formed. Once its density increased to the point at which hydrogen could begin to fuse into helium, the radiation pressure from the Sun was able to "blow away" the lighter gasses in the solar system which had not already been swept up by the protoplanets.

The planets themselves formed from the accretion disk which surrounded the Sun. The materials which make up the planets were never part of the Sun. The Sun and the planets all contain the same elements, though the Sun, with most of the mass of the solar system, contains the most of each element.

The gaseous nebula from which the Sun and planets formed was made up of a relatively homogeneous cloud of atoms and molecules, much of which was the remains of a supernova's ejected mass. Everything heavier than helium in the Sun and planets came from a supernova at some point.

Answer 3

The sun has plenty of heavy elements in it. It is mostly hydrogen but there is enough other stuff to make the earth a few times over.



In the early system lighter elements are easier to accelerate as the system collapsed. As a result most of the hydrogen (the lightest element) rushed to the center. The heavier stuff lagged behind a bit. Once fusion started the sun pushed away various elements and kept a lot of it from reaching the sun. These were swept up by the forming planets.

Answer 4

According to modern cosmological theory, very little mateial actually got thrown out of the sun during the formation of the solar system. What actually hapdened is that the proplyd, from which the solar system formed , flattened out into a disk due to rotation and most of the material was drawn to the centre due to gravity. At that stage the material in the protosun and the material in the disk had the same composition.



When the sun ignited, it "boiled off" most of the lighter material from the inner parts of the solar system, and what was left condensed into the inner planets. The "boiled off" material condensed into the giant planets from Jupiter onwards to Pluto.



Also think about the relative sizes of the Earth, the Sun and the original planetary disk. The mass of the Earth is only a tiny portion of the original disk. It represents the tiny fraction of cosmic material that consists of material other than hydrogen and helium.



This is an abridged account of the modern theory of solar system formation. Please refer to the wiki for a more comprehensive explanation.



Cheers!

Answer 5

Elements heavier than iron are formed during supernovas, which "throw" everything. Those lighter are formed in supernovas as well as in star's cores, which get ejected during star deaths of various forms.



The elements on earth aren't from our sun, mate.

Answer 6

Those heavier elements were not excluded from the sun.



"...

Fraunhofer Spectral Analyses are Important to Understanding Elements, Atoms, Sun and Universe

Scientists recognize approximately 92 naturally-occurring earthly elements and 72 solar elements.



The sun is 93 million miles (150 million kilometers) away from earth. The sun's core is about 64 % helium and 34 % hydrogen, and the core temperature is 15 million degrees Centigrade (27 million degrees Farenheit). The sun's core is totally gaseous due to the heat which prohibits solid or liquid forms of the elements, but the core is as dense as hard steel with large, concentrated masses of atoms.



Atoms of elements energized by the heat of nuclear fusion reactions can emit light and heat. Beginning in 1814, solar light was analyzed more critically and further by Joseph von Fraunhofer, an optical physicist in Germany, who noted distinct black lines (A through G as major lines, and a total of 576 lines). Fraunhofer proved that the black lines were the absorption spectra — those portions of the spectrum that were missing because they were absorbed. How does this actually happen?



Thermonuclear Solar Reactions, Fusion, Core Density, Electromagnetic Radiation

The sun is an intensely hot mass of hydrogen and helium and associated elements. The core of the sun is hottest, and the sun becomes cooler outward from the core. Intense heat is generated by solar thermonuclear fusion reactions: two hydrogen atoms combine to produce helium.



Read on

Detecting Planets Orbiting Stars

Water on Extrasolar Planets

Spectroscopy and Types of Spectra

Fusion generates both heat and light in the sun's core, and all 72 solar elements each emit unique spectral signatures. Solar radiation contains powerful X-rays and visible light which covers the full visible spectrum from 4,000 to 7,000 Angstroms. Light passes from the sun's interior and reaches the corona which is cooler and, there, portions of light are partially absorbed by the various elements.



The characteristic bright emission spectra of earthly elements correspond to the actual, similar elements in the sun. Fraunhofer determined that the dark lines are absorbed, missing regions of the spectrum. Both emission and absorption spectral lines are constant and specific for each element. Further, each element possesses multiple signature spectra. Foucault in 1849 showed that a double yellow flame spectrum was the dark D line of Fraunhofer. Angstrom identified hydrogen's spectrum in 1853, and Bunsen and Kirchhoff followed with systemic flame identification and cataloguing of thousands of spectral lines and the distinct elements they signified. Kirchhoff decoded the meaning of spectral lines, sunlight and Fraunhofer's spectral drawings, and he proved copper, zinc, calcium, iron, magnesium and sodium were present in the sun. In 1869, Lockyer discovered helium in the sun.



Spectroscopes, attached to telescopes, reveal that stars are very elementary, indeed!



Sources



Micropaedia of Encyclopedia Brittanica.1976. 15th ed., Chicago, Illinois.



Moore, Patrick. 1968. Amateur Astronomy. W.W. Norton & Co., Inc., New York, N.Y. 328 pp



NASA, U.S. 2006. Technology Through Time Issue #39: Solar Spectroscopy.



The New Book of Knowledge. 1995. Grolier, Inc., Danbury, Conn.





Copyright Donald Reinhardt. Contact the author to obtain permission for republication





Read more at Suite101: Fraunhofer Lines, the Sun, Elements and Universe: Continuous, Emission and Absorption Spectra Yield Elemental Data http://www.suite101.com/content/fraunhofer-lines-the-sun-elements-and-universe-a137804#ixzz16uEUv5VQ ..."



http://www.suite101.com/content/fraunhofer-lines-the-sun-elements-and-universe-a137804

Answer 7

formed when the stars collapsed at the end of their lives

Answer 8

bass ackwards....