How can a neutron star be born?
814106
A neutron star is the "squashed" core of a star that is left behind after the star underwent a Type II supernova. So a neutron star can be born when a star "dies".
1118173
Birth and death of stars is an interesting subject, IMO.\n\nHere are some starting points:\n\nhttp://en.wikipedia.org/wiki/Star\nhttp://en.wikipedia.org/wiki/Hertzsprung-Russell_diagram\nhttp://en.wikipedia.org/wiki/Supernova\nhttp://aspire.cosmic-ray.org/labs/star_life/starlife_main.html\nhttp://www.windows.ucar.edu/sun/Solar_interior/Nuclear_Reactions/Fusion/Fusion_in_stars/star_life.html
447612
one of the properties of a neutron star (as far as i can tell) is that the electrons and the protons are so tightly packed that they form in to neutrons. But they are not bound together like they are in the nucleus of an atom.  \n\nThere is actualy a great statmech problem where you are suposed to calulate the radius of a neutron star using only the pauli exclution principle (basicly that fermions have the tendency to repell each other)\n\nat the moment there are two known things that are even denser... a black hole for one, and the neuclus of an atom. \n\nIf there was a free existing small part of a black hole, it would just explode in a matter of moments (~10^-14 sec i think).  as for a neutron star they would also fly appart because for the pauli exclution principle.  But if we have a huge mass of protons and neutron we would have a very very very very heavy atom.  It would attract electrons just like a normal atom.  But it would decay in just moments(problably very violently).   \n\nIt can be made, but it would exist in such small quantity and for so short of a time that it would seemingly have no properites
194430
A Star's Size:\n\nA star begins its "life" in a contracting nebula of gas and dust. As the density of the material increases under the influence of gravity, compression heats the material. If the material gets hot enough, hydrogen atoms begin fusing together to form helium atoms, and a star is born. A star will spend most of its life, called the main sequence phase, fusing hydrogen into helium.\n\n  \nIt's logical that a large nebula (one with a large amount of mass) will form a large star, and a small nebula will form a small star. However, in addition to a star's initial mass, a star's size also depends on the balance between the inward pull of gravity and the outward push of the energy produced by fusion. The entire sequence of a star's evolution can be described in terms of the changing balance between these two opposing forces.
345536
It starts off with a good amount of hydrogen, which is fused into helium as it turns off the main sequence.  The more massive the star, the heavier the element it can fuse up to.  For more massive stars than the sun, helium can be fused higher up to carbon, oxygen, nitrogen, silicon, (i am forgetting one), and anything relatively close to iron.  Most of the elements made near iron will be radioactive and decay into iron.  At iron, you have to put more energy into fusing the atoms than you get out of the reaction.  At this point, for massive stars you will get a supernova as the star stops fusing in the core.  In the shockwave that occurs, enough energy can be put into the iron to fuse even heavier elements.  A good number of smaller than iron elements are also made in the process of making the above stated elements.
784870
seems you have no clue what you are talking about...\nwhat do you mean by how big of a neutron star ??
701207
it goes super nova and then a neutron star the rest of its life.  its life is also shorter because the increased gravity requires more nuclear fusion (and faster fuel consumption) to negate.
732762
Their materials collect together (via gravity) and make new stars.  Granted, they tend to be made of heavier materials and burn cooler (often red).\n\nStars collapse when they run out of material.  A star begins by fusing hydrogen into helium.  Eventually, the hydrogen runs out and the star begins to collapse until it is able to fuse helium into carbon.  This continues through various elements until it is largely iron.  A star is simply not able to fuse iron into anything else (their not massive enough), so it eventually has a final collapse, sometimes into a supernova.\n\nThis final collapse can leave three possible "leftovers":\n1.  A white dwarf - if the star is less than 3 x the mass of our sun, then the core will be left as a burning ember.  Eventually it will burn out to become something known as a brown dwarf, a dead star.\n\n2.  A neutron star - if the star is between 3 and 10 (I think) x the mass of our sun, the explosion compresses the core down enough that protons and electrons are crammed together to form a neutron star.  It's a bunch of neutrons so dense a teaspoonful would weigh, well, tons on the earth.\n\n3.  A black hole - if the star is especially massive, the collapse never ends.  The core itself cannot overcome the massive gravity that is created by a now extremely dense remnant, forming a black hole.
593845
Great Question\nBlack hole fast facts:\n\n1.Once a large star dies, its internal gravitational strength causes all of the stars matter to collapse in on itself,(electrons are compressed into and combined with the atoms nucleus), this forms a neutron star.\nA neutron star, if dense enough will continue to collapse inward compressing the neutron matter further until it exists as matter/energy in its purest form. (All matter and energy is coalesced into one single state of energy)\n\n2.They are the single largest gravitational entity theorized to exist. This large gravitational attraction pulls in matter (atoms) and adds it to the singularity (energy mass) at its center.\n\n3.They represent the possible end of our universe.(big crunch)\n\n4.They are one of the few places that prohibit the propagation of light.\n\n5.The laws of nature at a black hole are completely different from anywhere else in the universe.\n\nThese are the main highlights.
284766
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.
574586
Not sure I buy that.  A neutron star is about 1.3-2.1 solar masses about 10 miles across. While that is much heavier than the earth, 10 miles across is pretty darn big compared to a test tube.  Doesn't work out to me.\n\nA teaspoon of it weighs about 10 million tons, assume 100 teaspoons or even 1,000 teaspoons and you don't have near the weight of the earth. It's mass is about 6 x 10^24 kg.\n\nA neutron star isnt exactly just bare neutrons, but I would need more evidence to beleive it.
910455
A pulsar is a neutron star that has a strong magnetic field that is swept around as the neutron star rotates.  The swept magnetic field creates a beamed "pulse".  A neutron star could fail to be seen as a pulsar because:\n1) it's not rotating fast\n2) it doesn't have a strong magnetic field\n3) the magnetic pole on the neutron star is not displaced from the rotational pole\n4) the swept magnetic field does not have the right density of plasma to interact with\n5) the "beam" of the pulsar is not pointed at the Earth.
654297
A star forms in a nebula which is a very large cloud of hydrogen gas.  hydrogen is the basic building block of the universe.  A prostar is formed when a portion of the hydrogen in the nebula is formed into a hydrogen ball by the pull of gravity.  When the molecules become close enough the friction of their bumping together causes heat.  If it were not for this heat production the prostar would be pulled into a clump by the force of gravity.  Once enough heat is formed in the core of the prostar (about 2 million degrees) hydrogen nuclei join together to form a helium molecule.  The reaction is 6 H >1 He + 2H  That means 6 hydrogens are needed for the process to proceed, but two hydrogen are reclaimed on the other side so the net rxn is 4h > 1 He.  This reaction is possible because of entropy or the conservation of energy.  It takes less energy to maintain one atom of Helium than 4 atoms of hydrogen.  In the sun this energy savings is 0.6% which radiates to the surface and is expelled as sunlight.  Within the Sun about 745,000 tons of Hydrogen is converted to Helium every second.  The balance of the pull of gravity (collapse) and the heat from nuclear fusion (expansion) keeps the star's size and shape constant.  Once this process begins the prostar becomes a star.  There are other nuclear fusion reactions untill the formation of iron.  This step does not give off energy but requires energy input.  At this step stars begin to cool and become a red giant.  This is the first step in the death of a star, resulting in the formation of a nova or a supernova depending upon the size of the star.  a smaller star will form a white dwarf and the larger star will form a neutron star or if large enough it may collapse into a black hole.  Gravity is the attraction of particle to particle between two objects.  This is how a black hole works.  It has an extreemly strong gravitational pull because the core is composed of a very large amount of compacted particles and each of those particles contribute to the gravitational attraction.
636967
Stars are huge, very, very hot balls of gas that shine brightly. Stars like all other matter is made up of millions of atoms. The simplest and lightest element is hydrogen gas. Enormous clouds of hydrogen gas and dust particles form in space. Gravity draws the dust and gas close together forming a huge clump, or mass.\n\nAs more and more matter is added to the mass, its gravity increases. This pushes the atoms of hydrogen gas closer and closer together. The mass begins to contract, or get smaller. It also gets denser and hotter. The center is hottest of all because the atoms are being squeezed together. The heat creates tremendous energy. Energy is the power necessary to make things happen.\n\nFinally, the crowding of the atoms, the heat, and the violent energy forces the hydrogen atoms to combine. This makes a new and heavier element called helium. The change of hydrogen gas to helium gas is called thermonuclear fusion. When this happens a star is born.\n\nTherefore , stars appear to be circular in shape because of the gravitational pull the mass exerts from all sides. It attracts hydrogen and dust particles with equal force from all sides and hence from a distance when we look at a star , it appears like a shining ball to us. When the Helium gas reaction takes place , it still appears cirular to us since the gravitational pull inside the star holds it together with equal force in all directions. \n\nThroughout a star's life, thermonuclear fusion goes on in its core, creating enormous energy. That energy becomes light and heat. It makes the star shine.\n\nThe new star will shine in the heavens for billions of years. It will stay that way until all its hydrogen gas has changed to helium.\n\nWhen a star has finally turned all its hydrogen into helium it is nearing the end of its life. Scientists believe that the amount of mass left in the dead star determines what will become of it.\n\nWhen a star has finally turned all its hydrogen into helium it is nearing the end of its life. Scientists believe that the amount of mass left in the dead star determines what will become of it.\n\nWhen an even bigger star — a giant star — uses up all its energy, it collapses even more than a white dwarf. Its mass and gravity are much greater. No space is left between the atoms. Electrons and protons inside the atoms are pushed together. They become neutrons and the giant star shrinks to a very small size. It is called a "neutron star" and is usually only a few kilometers in diameter. But its mass is so great that a tiny bit of neutron star — less than a teaspoonful — would weigh about half a trillion kilograms. That's as much as a long freight train loaded with bricks!\n\nSometimes, when a giant star collapses, particles called neutrinos are forced out of the atoms. As the neutrinos burst forth from the dying star, the star shines more brightly than any other object in the galaxy. It looks like an enormous sparkler. This is a "supernova."\n\nWhen the amount of mass left in a dying star is three or more times the mass of the sun, something very mysterious happens. A star this massive shrinks much faster than the white dwarf and the neutron star. Its force of gravity is very great. Nothing can escape it — not even light, which moves faster than anything else in the universe. This star becomes a "black hole."\n\nMany astrophysicists believe that there are black holes at the center of most galaxies, including our Milky Way. Although that may be so, our solar system is too far removed from the black hole for us to be influenced by its pull of gravity.\n\nAnother popular belief about black holes is that it can be a very vital tool in time travel\n\nCheck these links :) very interesting :) \n\nhttp://www.astronomycafe.net/qadir/q285.html\nhttp://science.howstuffworks.com/time-travel3.htm
166575
The mathematical grammer for your question would read,\n\n3.23x-666(ab/=y)-9x12.8.\nBut if it is advice you are after,\n\n1.If I had a white dwarf, I would presumably be in the North Pole downtown toy warehouse district? \n2.Neutrons are synonimus with black holes. Never turn your back on one.
575470
There are two possible causes of supernovae:\n\n- A massive star may no longer produce fusion energy from fusing the nuclei of atoms in its core. Gravity wins and the star collapses inward under its own weight.\n\n-A old, white dwarf star that has a close companion from which material falls on it. If its mass becomes larger than about 1.5 solar masses it will undergo a thermonuclear explosion. \n\nIn both cases, the resulting supernova explosion expels an enormous amount of steller material forming a nebula.
1153711
A star takes birth from nebula. Then in the ending years of its life it's volume gets increased and becomes red supergiant. Then it becomes supernova for a few months or years but about 10 billion times as bright as our sun. Then \n1) It can get recycled into nebula OR\n2) It can become a neutron star OR\n3) It can become a black hole.\n\nBlack holes are thought to form from stars or other massive objects if and when they collapse from their own gravity to form an object whose density is infinite: in other words, a singularity. During most of a star's lifetime, nuclear fusion in the core generates electromagnetic radiation, including photons, the particles of light. This radiation exerts an outward pressure that exactly balances the inward pull of gravity caused by the star's mass. \n\nAs the nuclear fuel is exhausted, the outward forces of radiation diminish, allowing the gravitation to compress the star inward. The contraction of the core causes its temperature to rise and allows remaining nuclear material to be used as fuel. The star is saved from further collapse -- but only for a while.\n\nEventually, all possible nuclear fuel is used up and the core collapses. How far it collapses, into what kind of object, and at what rate, is determined by the star's final mass and the remaining outward pressure that the burnt-up nuclear residue (largely iron) can muster. If the star is sufficiently massive or compressible, it may collapse to a black hole. If it is less massive or made of stiffer material, its fate is different: it may become a white dwarf or a neutron star\n\nThe gravitationsl pull of black hole is so powerful that it can even suck in light.\n\nThere is a theory that what gets suck by black holes is thrown out by a "whitehole" that matter travels through a "wormhole". But if this is true then may be one day we may travel with or more than the speed of light to reach very very far away points in the universe.\n\nFor more information search http://www.google.com for black hole.