what is a star with a contracted burned out center called?
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The burned out centre of a low mass star is a white dwarf. It's a hot ball of carbon and oxygen, though too cool for thermonuclear reactions to occur. They're about the size of Earth and are too dim to be seen with the naked eye.
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Stars are massive, glowing balls of hot gases, mostly hydrogen and helium. Some stars are extremely hot, while others are cooler. You can tell by the color of light that the stars give off. If you look at the coals in a charcoal grill, you know that the red glowing coals are cooler than the white hot ones. The same is true for stars. A blue or white star is hotter than a yellow star, which is hotter than a red star. Temperature of stars range in the high hundreds to thousands degrees F. So to touch the stars that are in the sky is almost impossible, as your body would burn due to high temperatures surrounding them.
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The general term is double star. If the two stars are actually physically close so that they orbit each other, it is also called a binary star. Stars that appear close together but are actually at very different distances are called optical doubles.
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look at the star on the left
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When a star runs out of nuclear fuel, and therefore continues to lose energy from the surface (it is emitting light energy), while not replacing the lost energy through nuclear fusion (no more nuclear fuel), gravity will win out over internal pressure and the star will contract slowly or collapse quickly depending upon the details of the internal structure and composition. Gravity wins out over the internal pressure of the star, because that pressure was produced by a normal, hot gas, and that gas is losing energy as the star radiates energy from the surface. \n\nThe star may thus end up as a black hole.
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upper left hand corner....icon looks ike a star
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This is caused by thermic convection of the air. In the deserts you normally have high differences in temperature between day and night, so hot air is rising rapidly while cold air is moving downwards after sunset. This different densities in the air makes the light bend and the stars seems as if they are dancing, just as if you were looking through an irregular glass. \nIt's a bad night for astronomers.
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The prominent Y-shaped asterism called the "Water Jar" (or "Urn") of Aquarius, the Water Bearer, is in the middle of the picture and is made of a "Y" of stars with Zeta Aquarii) at the center. Sadalmelik, Aquarius's Alpha star, is immediately to the right of the Water Jar, just to the right of center, and is tied for the brightest star in the image. The other bright star, just below center near the right-hand edge of the picture, is Sadalsuud, Beta Aquarii. Sadachbia, Gamma Aquarii, is the lower right star of the Water Jar while Eta Aqr is the left-hand star. Hydor (Lambda Aqr) is the brightest star down and to the left of the asterism. Part of the "Circlet" of Pisces lies at left.
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Stars need hydrogen, period. The fancy name for what happens in the star is thermonuclear fusion, which just means that two hydrogen atoms are fused to make helium, and in the process release a lot of light and energy, allowing the star to shine. So, you know how when you pump up a bike tire, the pump gets hot? That's because you're compressing a fluid (in the case of stars it's hydrogen) and when you compress a fluid the fluid heats up (in this case it's the air heating up the pump). This heating up has to reach 25 million degrees before a star will shine, and the "pump" is gravity in this case. so a star has to have a lot of hydrogen from which to form if it's going to become hot enough to go into thermonuclear fusion.
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Very simply: Every element when heated gives off a radiation frequency that is specific to itself. When the entire spectrum of light from a star is analyzed, those frequencies representing specific elements are absorbed and show up as dark lines in specific areas. Each star has a unique pattern. After correcting for any red or blue shift ( discuss that another time), the same elements will appear in the same spectral region.
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A very bright "star" that's usually reported is the planet Venus. It rises and sets close to the sun and has therefore in ancient times been given the names Eveningstar and Morningstar. \n\nIf you see a star that sets or rises just hours before or after the sun and is exceptionally bright, you're with highest probability looking at our neighbour planet Venus.
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Monoceros\n\nHere's a link for you to check the answer,\nhttp://www.astrofilitrentini.it/mat/costell/mon_e.html
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Star's are for the most part the same as our star/sun. The difference being we named our star The Sun.
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The star begins as a cool cloud of gas. Under its own gravity, the cloud begins to collapse. As it collapses, it releases its gravitational energy as radiation. So a young star is cool but bright. We usually don't see these proto-stars, however, because they are generally shrouded in dust and only give off light. \n\nThe proto-star continues to collapse, and as it does, it gets hotter and hotter. "Stars" less than a percent of the Sun's mass eventually halt their collapse due to gas pressure. These stars are "brown dwarfs" or "giant planets," like Jupiter. They never ignite their hydrogen, and gradually dim away. \n\nStars larger than about 0.05 to 0.07 solar masses contract, getting hotter and hotter, until their cores are hot enough to begin burning hydrogen. When a star "turns on" its hydrogen-burning phase, we say that it has reached the main sequence, and is a true star, not a protostar, brown dwarf, or planet. The main sequence is a line of stars plotted on the HR-diagram, which represent stars which are burning hydrogen, fusing it into helium. The fusion process in the core releases heat and light, supporting the star against further gravitational collapse, and making it shine. Stars spend most of their life in one spot on the main sequence. Very massive stars live at the top of the main sequence, shining very blue and very bright, while low-mass stars are dim and red. The sun is between these two extremes. \n\nEventually, the hydrogen in the core whose fusion supports the star begins to run out. The core becomes mostly helium (the product of hydrogen fusion), and hydrogen burning moves out away from the core, forming a burning shell around the core. When this happens, the core begins to collapse again, but the outer regions of the star are pushed outwards. The star becomes brighter and cooler. This is the Red Giant stage. When the sun reaches the Red Giant stage, 5 billion years from now, it will likely grow to engulf Mercury, Venus, and the Earth. \n\nIf the star has little mass, it may end its life here, throwing off its outer layers, creating a planetary nebula out of its atmosphere, and a hot, dense "white dwarf" out of its core. The white dwarf shines only by residual left-over heat, and will eventually fade into a mere cinder. Cores of stars at least half as massive as the sun, however, will eventually collapse and heat enough to start burning helium in their cores. Once helium-burining starts, the star decends the giant branch again, reverses its swelling a bit, and lives happily fusing helium in its core, and hydrogen in a shell around the core. \n\nThen the giant dance begins again. The core helium runs out, and the star once again becomes a red giant. Stars like the sun get off the bus here, and become planetary nebulae and white dwarfs. Heavier stars begin burning carbon. This happens over and over again with heavier and heavier elements. The star ascends and descends the giant branch many times. Lighter stars that don't get hot enough in their cores to burn the next element become planetary nebulae and white dwarfs. Stars that are heavy enough eventually heat their cores enough to begin the next stage of burning and descend the giant branch for a while. For each element, the process is quicker and quicker. A star might burn Hydrogen on the main sequence for billions of years, but once this process gets to, say, silicon, the star might burn silicon for only a few days. \n\nA very massive star, more than 5-10 times solar mass, will ascend and descend the giant branch many times, until the star is ready to burn iron. But iron fusion doesn't release energy; it sucks it up. So what happens is that the star is ascending the giant branch, its iron core is collapsing and heating, until iron is ready to fuse. As soon as it does, though, it absorbs all of the heat around it, chilling the core. All fusion abrubtly stops, and the star implodes. The rebou
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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.
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luminal celestial body of super heated gasses, Stars don't have names per say, they do have classifications like G-2 class of star, which is a yellow main type of star, if you were referring to the name of our sun it is called Sol, and a yellow main type of G-2 class of star to boot.
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Mintaka or delta Orionis is a massive O star.  These stars are roughly 20 times the mass of the Sun.  In a short few million years after the star is born it will die in as supernova.  The remnant of the supernova will be either a neutron star or a black hole.  In some cases a supernova can completey annihilate a star and then leave nothing behind.\n\nMintaka is likely just 1 million years old so it will be some time before it dies.