What is the supernova scene?
541769
chevy nova really did.
579859
I assume you mean "star" and not "sun", as in OUR sun, in the first question.  In that case, a supernova is essentially the spectacular explosion that occurs when a star of a significant sized mass ends its life.  IN that case, all the elements with a periodic table number higher than oxygen are created.  In addition, the remaining core of the dead star becomes so dense, that it creates an object that even light can't escape.  This object is now a black hole.\n\nOur sun is not big enough to supernova, therefore it will just die out and become a black dwarf when it is dead.\n\nDefinition from the Big Wiki...\n\nhttp://en.wikipedia.org/wiki/Supernova
524772
This happened in three ways.\n1) at the time of the Big Bang the matter was very dense. Because of this about a quarter of the available protons got changed into neutrons. These fused with protons to make principally Helium, heavy hydrogen and a tiny bit of Lithium.\n2) this mixture ended up in the first generation of stars.\nDuring their lifetime hydrogen was again fused mainly into helium, but also heavier stuff, like oxygen, sulfur and a few more elements upto iron\n3) the bigger stars of the first and later generation explode at the end of their life, when there is no longer enough fusion going on in their cores for lack of elements to fuse. The supernova explosions produce a lot of neutrinos. Neutrinos are capable to transmutate elements into others. In this proces all the elements are produced even the ones heavier than iron.\n\nHow do we know this?\n\nThese three processes can be modeled and calculated on computers. These models give predictions on the amount of helium and other elements produced in the Big Bang and in supernovae. These predictions can be checked against the actual abondance of the elements in stars, in the solar system and in the earth's crust.
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.
671170
Are you including the stars that are being created, as well as those that do not actually exist anymore but have died out/ supernova'd/ etc. that we are just still seeing since the light has to travel so far?  \n\nI would be interested in how you determined this number ^_^
496226
STARS AND NEBULAE.\n\nMost of the things you can see in the night sky are stars: a few thousand are visible to the unaided eye. A star is a hot ball of mostly hydrogen gas; the Sun is an example of a typical, ordinary star. Gravity keeps the gas from evaporating into space, and pressure due to the star's high temperature and density keeps the ball from shrinking. In the core of the star, the temperature and densities are high enough to sustain nuclear fusion reactions, and the energy produced by these reactions works its way to the surface and radiates into space as heat and light. When the fuel for the fusion reactions is depleted, the structure of the star changes. The process of building up heavier elements from lighter ones by nuclear reactions, and adjusting the internal structure to balance gravity and pressure, is called stellar evolution. \nLooking at a star through a telescope can tell us many of its important properties. The color of a star tells us its temperature, and the temperature depends on some combination of the star's mass and evolutionary phase. Usually, observations also allow us to find the luminosity of the star, or the rate at which it radiates energy as heat and light. \nAll stars visible to the unaided eye are in our galaxy, the Milky Way. The Milky Way is system of roughly 100 billion stars, along with a great deal of interstellar material. The galaxy is shaped like a flattened disk embedded in a round, faint halo. Gravity keeps the stars from drifting away, and the motions of the stars keep the system from falling in on itself. The Milky Way has no distinct edge - the distribution of stars tapers off gradually with increasing distance from the center. The SDSS detects stars more than a million times fainter than can be seen with the unaided eye, far enough to see the outer structure of the Milky Way. \nStar Colors and Luminosities: The H-R Diagram\nAstronomers often make plots of the luminosities of stars compared to their colors. The first such charts were made in the early twentieth century, when astronomers took spectra of thousands of stars, then placed the spectra into a sequence based on the appearance of several different features. The classes of stars were given different letters as names; in order of decreasing temperature, they are OBAFGKMLT. The hottest stars are class O, while the coolest are class T. Two astronomers, Ejnar Hertzsprung and Henry Norris Russell, independently started to wonder what would happen if they compared stars' luminosities to their spectral classifications (or, alternatively, to their temperatures). They knew that some stars were hotter and more luminous than the sun, and that others were cooler and less luminous. Hertzsprung and Russell found that 90% of the stars fell into a narrow band they termed the "main sequence." Today, we call this type of plot a Hertzsprung-Russell (or H-R) diagram. \nAstronomers further divide each letter into ten categories from 0 to 9, with 0 being the hottest star in that spectral class and 9 being the coolest. So, a B1 star is hotter than a B2 star, and a B9 star is hotter than an A0 star. Our own sun is at the "hot" end of the G range with a surface temperature of 5,770° K; therefore, it's called a G2 star. \nSpectral classes give us a convenient way to refer to most types of stars - from O0, the hottest at over 25,000° K, down to T9, the coolest failed stars at 1,000° K. Each spectral type of star is associated with a specific color: all G-type stars like the sun are yellow, all M-type stars appear red, and all B-type stars are bluish. Thus, this system of letters and numbers tells us where a star is on the horizontal (color or temperature) axis of the H-R diagram. \nTwo alternative systems tell us approximately where on the vertical (luminosity) axis a star can be found. One system uses absolute magnitude, a measure of luminosity derived from the apparent magnitude, or brightness of the star
994321
I'm afraid it won't explode now.\nIt won't go and explode as a nova or super-nova unless something real bad happens and it gets a denser core.\nOur star won't explode until at least 5 billion years time, unless anything makes it do it.\nThe term nova means very large explosion. But our star won't explode it will widen with a little explosive force and all of it's gaseous surface and mid layers will blow off.\nOur star is an M class (G Medium class) a super-nova will only happen with L class stars (O Large class) + (M Small class) the M and S class have novas only when they collide it is likely to be explosive as the stars are young and hot.\nThe main course of nuclear fusion is:\nD+T=4He+1n or 3-2H+2-1H=4He-3.5MeV+1n-14.1/14.2MeV\nThe sun will not explode in at least 1 billion to 5 billion years!
321257
We do this all the time today.  We have many times looked into the heart of a planetary nebula (leftover from the death of a low mass star) or a supernova remnant (leftover from the death of a high mass star) to see the small compact objects left over after the star has died.\n\nIn the case of a low mass stars we see many white dwarf stars, and for the high mass case we see neutron stars.  A good example is the pulsar we have seen in the Crab nebula, or the white dwarf at the heart of the Ring nebula.
404738
In 1094 AD, a  supernova, clearly visible in daylight, was witnessed and recorded in China and India, and the result of it can now be seen in space as the luminous Crab Nebula, measuring 10 light years wide and being lit by the Crab Pulsar in the center. At 9.7 kilometres wide, it rotates 33 times per second and has an extremely strong magnetic field. This magnetic field constantly hurls particles out of the inner part of the nebula and into the larger cloudlike part.
185980
Our sun will not supernova.  It will, over a very long time, expand into a relatively small red giant, which will have a diameter greater than the Earth's orbit.\n\nLong before that the Earth will have become far too hot to live on, but the process will be very, very slow -- it'll take over a billion years -- not a giant explosion.\n\nSorry to disappoint you.  I know, you sound like you were looking forward to it.  Funny how many people answering this question think otherwise.  I guess that's the irony of the internet for you.\n\nSee the link below for all the details:
236965
What my colleagues are getting at is that stars (the most notable bodies within any galaxy) are simply extremely dense spheres of gas (usually mainly hydrogen and helium) that are so condensed by their collective gravitiy, they actually fuse together, forming heavier elements and releasing massive amounts of energy in the process.
847308
It's a bit complicated.  The Earth's magnetic field is powerful enough to minimize charged particles from the solar wind, and the atmosphere attunates almost all other particles.  However, when a star goes nova, two jets are created at the poles.  These jets are extremely powerful with respect to the rest of the explosion.\n\nTherefore, if the Earth were not in the line of sight of the jets, the atmosphere and magnetic field would be extremely effective, and a supernova would have to be with a few 10s of light years to be dangerous.  However, if the Earth were in a line of sight of the jets, then during a few seconds the Earth could be bathed in deadly radiation, even if the source were a thousand light years away.
680419
A star is a massive body of plasma in outer space that is currently producing or has produced energy through nuclear fusion. The most familiar and closest star to the Earth is the Sun. Unlike a planet, from which most light is reflected, a star emits light because of its intense heat. Scientifically, stars are defined as self-gravitating spheres of plasma in hydrostatic equilibrium, which generate their own energy through the process of nuclear fusion. Stellar astronomy is the study of stars.
518670
go to mininova.org and search it... u should beable to find it there man.
492304
Nebulas: One of the most beautiful phenomenon in the universe. They are made up of gas left behind by stars forming or exploding. \n \nTypes/Classes of nebula: planetary, supernova remnants, diffuse nebula\n\nPlanetary nebulas: Resemble planets, and are actually left over shell material from forming stars during their giant Red Stage.  \n\nSupernova: Remnants are exactly what they say: supernova nebulas are remnants of a star that exploded.  Left over remnants become surrounded by gas, causing a nebula.   One of the most famous supernova nebulas is the crab nebula in the star constellation Taurus.\n\nDiffuse nebulas: Extremely large, and can be light years in width.  They have no definite shape, and are either light or dark.
164275
I've not heard of this, but the biggest explosion since Big Bang? Sounds very exaggurated in my opinion. There was however an article about a large star exploding and turning into a black hole that was observed.\n\nThe last link I think talks about your event. The middle one is just interesting if you wonder about them in general.
84045
A black hole is the collapsed stellar remnant of a supernova (a nova is an entirely different phenomena caused by matter falling onto a white dwarf). Depending on how massive the star is either a white dwarf (lightest) a neutron star (heavier) or a black hole (heaviest) form when a star dies.\n\nType II Supernovas are the catastrophic, yet natural, deaths of massive stars. The star has to be 8 times more massive than the sun to cause a supernova. \n\nOnce a star has used up all of its hydrogen in the fusion processes in the core, there is no more pressure to keep the stars core from collapsing under its own weight. Eventually it gets so hot that the helium begins to fuse which again causes pressure that temporarily halts the collapse. In a star like the sun helium fusion is the end. Once the helium is spent the stars core begins collapsing again while its outer layer puffs out into space leaving a white dwarf. \n\nIn a more massive star carbon fusion, which produces neon and manganese, takes over when the helium is spent because its gravity can cause temperature and pressures great enough. When the carbon is gone the core begins collapsing again. This goes on for several stages of contraction with resulting fusion of increasingly heavier elements. \n\nFinally silicon fuse into iron and the core is the size of earth. The temperature is over 3 billion degrees. No more energy can be produced from fusion as iron is too tightly bound in its nuclei. Instead the iron core collapses with a quarter the speed of light. It shrinks in size from the size of earth to a sphere 100 kilometers across in less then one tenth of a second. This produces gravitational energy 100 times greater than the energy the sun has put out during its entire life. This energy is what blows the outer layers of the star apart. In the expanding envelope neutrons are created that slam into other nuclei to form extremely heavy isotopes. As they decay they form elements heavier than iron. \n\nIn the core, denisty is now so great that protons and electrons can no longer exist. Instead they begin to form neutrons. When that process is complete a neutron star, about 10 to 20 km in diameter, is born. \n\nIf the mass of the star is so great that not even the neutrons can keep it from coallapsing further eventually you end up with an objects so dense its escape velocity becomes greater than the speed of light and a black hole is born.