Linking Asteroids and Meteorites through Reflectance
... Can Carbon undergo fusion? • Yes, but can’t reach the needed temperature (600 million Kelvin) in a low-mass star • Carbon on Earth is produced in the cores of stars ...
... Can Carbon undergo fusion? • Yes, but can’t reach the needed temperature (600 million Kelvin) in a low-mass star • Carbon on Earth is produced in the cores of stars ...
Astronomy 12 - hrsbstaff.ednet.ns.ca
... (d) How much hydrogen does it need to fuse into helium every second to support itself? H. Supernova Essay. Write a short essay on supernovae that answers that following questions: (a) What are the differences between Type Ia and II supernovae in terms of their: lightcurves, spectra, location in gala ...
... (d) How much hydrogen does it need to fuse into helium every second to support itself? H. Supernova Essay. Write a short essay on supernovae that answers that following questions: (a) What are the differences between Type Ia and II supernovae in terms of their: lightcurves, spectra, location in gala ...
On the Progenitors of Type Ia Supernovae
... Double degenerate systems detected observationally. Mergers with some significant consequences appear inevitable. In ellipticals, consistent with observed x-ray flux (~30x smaller than predicted for SDS). ...
... Double degenerate systems detected observationally. Mergers with some significant consequences appear inevitable. In ellipticals, consistent with observed x-ray flux (~30x smaller than predicted for SDS). ...
Lecture 2
... There are two different types of supernovae, both equally common: Type I -- results from excess mass being dumped onto a white dwarf from a binary companion Type II -- the “normal” death of a high-mass star. ...
... There are two different types of supernovae, both equally common: Type I -- results from excess mass being dumped onto a white dwarf from a binary companion Type II -- the “normal” death of a high-mass star. ...
Star Formation
... Stars form: a. In Giant Molecular clouds b. When a shock like a supernova explosion compresses a giant molecular cloud c. With more massive stars forming first ...
... Stars form: a. In Giant Molecular clouds b. When a shock like a supernova explosion compresses a giant molecular cloud c. With more massive stars forming first ...
ref H-R Spectral types
... It is also the brightest star seen from Earth. One of the two stars that make up what we call “Sirius”,Sirius A is a type A star. ...
... It is also the brightest star seen from Earth. One of the two stars that make up what we call “Sirius”,Sirius A is a type A star. ...
The Stars - Department of Physics and Astronomy
... The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star’s nuclear fuel is depleted, the star must ...
... The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star’s nuclear fuel is depleted, the star must ...
Lecture 33: The Lives of Stars Astronomy 141
... The primary source of energy for stars over most of their lives is nuclear fusion. Example: Fuse 4 Hydrogen nuclei into 1 Helium nucleus 4 protons weigh slightly more than 1 Helium (2p+2n): 1 kg of Hydrogen would fuse into 0.993 kg of Helium. Leftover 0.007 kg (7 grams) is converted into energy: ...
... The primary source of energy for stars over most of their lives is nuclear fusion. Example: Fuse 4 Hydrogen nuclei into 1 Helium nucleus 4 protons weigh slightly more than 1 Helium (2p+2n): 1 kg of Hydrogen would fuse into 0.993 kg of Helium. Leftover 0.007 kg (7 grams) is converted into energy: ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... made of) were made in the big bang. Many of the helium atoms in the Universe were also made in the big bang. The other atoms were made inside of stars or during explosions of stars. When the Sun becomes a red giant, carbon and maybe oxygen will be made in its core. But the core will be the left-over ...
... made of) were made in the big bang. Many of the helium atoms in the Universe were also made in the big bang. The other atoms were made inside of stars or during explosions of stars. When the Sun becomes a red giant, carbon and maybe oxygen will be made in its core. But the core will be the left-over ...
White Dwarf
... of energy, and Fe fusion taking energy from the gas, pressure support in the star’s core is lost… ...
... of energy, and Fe fusion taking energy from the gas, pressure support in the star’s core is lost… ...
Section 1 Notes on Stars
... reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of energy rather than causing energy to be released ...
... reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of energy rather than causing energy to be released ...
Document
... reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of energy rather than causing energy to be released ...
... reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of energy rather than causing energy to be released ...
Document
... reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of energy rather than causing energy to be released ...
... reactions • The sequence of thermonuclear reactions stops here, because the formation of elements heavier than iron requires an input of energy rather than causing energy to be released ...
The Death of a Low Mass Star
... contained heat only No further contraction takes place Electron degeneracy pressure supports the star ...
... contained heat only No further contraction takes place Electron degeneracy pressure supports the star ...
The Birth, Life, and Death of Stars
... Black Holes ... “an object from which not even light can escape” Gravity is a geometric property of spacetime Photons, although massless, feel the effect of gravity Event horizon of a black hole Unrelated to the physical dimensions of the BH A “boundary” from which not even light can escape Schwarz ...
... Black Holes ... “an object from which not even light can escape” Gravity is a geometric property of spacetime Photons, although massless, feel the effect of gravity Event horizon of a black hole Unrelated to the physical dimensions of the BH A “boundary” from which not even light can escape Schwarz ...
Life and Death of a Star The Universe Season 1 Episode 10
... into such density that the gravity field is enormous. Light can’t leave because the gravity is so strong. There is limit to where you will get pulled into a black hole. ...
... into such density that the gravity field is enormous. Light can’t leave because the gravity is so strong. There is limit to where you will get pulled into a black hole. ...
Main-sequence stage Stellar lifetimes
... – Star’s inner regions collapse on to compressed core. – They are then ejected together with the neutrinos out through the star to produce a supernova event. – > 90% of star’s mass may be ejected into interstellar space. – Energy released ~ 1043 J ! – Most likely remnant is a neutron star -- mass ~ ...
... – Star’s inner regions collapse on to compressed core. – They are then ejected together with the neutrinos out through the star to produce a supernova event. – > 90% of star’s mass may be ejected into interstellar space. – Energy released ~ 1043 J ! – Most likely remnant is a neutron star -- mass ~ ...
Document
... blue lines show contraction from about 20 km then evolution at constant R = 10 km as the luminosity declines. Thompson, Burrows, and Meyer, (2001), ApJ, 562, 887 ...
... blue lines show contraction from about 20 km then evolution at constant R = 10 km as the luminosity declines. Thompson, Burrows, and Meyer, (2001), ApJ, 562, 887 ...
The Distance Ladder I - Sierra College Astronomy Home Page
... A binary system in which the compact companion is a white dwarf star near 1.44M. Mass flows from the expanding giant star, forming an accretion disk. Frequent novae occur. The white dwarf star approaches 99% the Chandrasekhar Limit. Uncontrolled C and O burning sweep through the white dwarf, releas ...
... A binary system in which the compact companion is a white dwarf star near 1.44M. Mass flows from the expanding giant star, forming an accretion disk. Frequent novae occur. The white dwarf star approaches 99% the Chandrasekhar Limit. Uncontrolled C and O burning sweep through the white dwarf, releas ...
The Death of a Star
... If it was born into a binary star system, the white dwarf can take mass from it’s neighbor until its core exceeds the Chandrasekhar limit. Animation ...
... If it was born into a binary star system, the white dwarf can take mass from it’s neighbor until its core exceeds the Chandrasekhar limit. Animation ...
Stars and Galaxies
... A black hole does not suck matter in like a vacuum cleaner. But a black hole’s gravity is very strong because all of its mass is concentrated in a single point. Because astronomers cannot see a black hole, they only can infer its existence. For example, if they detect a star circling around somethin ...
... A black hole does not suck matter in like a vacuum cleaner. But a black hole’s gravity is very strong because all of its mass is concentrated in a single point. Because astronomers cannot see a black hole, they only can infer its existence. For example, if they detect a star circling around somethin ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... So the conclusion seemed inescapable: supermassive black holes had to have started life already monstrous at cosmic dawn. But how? Monster stars Just as ordinary black holes are the stellar remnants left by supernova explosions of stars more than 20 solar masses, supermassive black holes could have ...
... So the conclusion seemed inescapable: supermassive black holes had to have started life already monstrous at cosmic dawn. But how? Monster stars Just as ordinary black holes are the stellar remnants left by supernova explosions of stars more than 20 solar masses, supermassive black holes could have ...
2017 Maryland Regional
... 40. True or false: Type Ia supernovae are primarily distinguished from Types Ib and Ic by their lack of an oxygen absorption line. a. True b. False 41. What role does electron degeneracy pressure play in determining the Chandrasekhar Limit? 42. Following neutronization, what must first occur before ...
... 40. True or false: Type Ia supernovae are primarily distinguished from Types Ib and Ic by their lack of an oxygen absorption line. a. True b. False 41. What role does electron degeneracy pressure play in determining the Chandrasekhar Limit? 42. Following neutronization, what must first occur before ...
The Death of High Mass Stars
... are moving with speeds according to the temperature of the cloud. If the cloud is cold enough, the particles will begin to come together due to the attractive force of gravity. The first several stages of star formation take about 2 million years as the densest pockets collapse first leading to frag ...
... are moving with speeds according to the temperature of the cloud. If the cloud is cold enough, the particles will begin to come together due to the attractive force of gravity. The first several stages of star formation take about 2 million years as the densest pockets collapse first leading to frag ...
Classifying Stars - Concord Academy Boyne
... Click on the picture above to watch a video from the history channel on the life cycle of a star! Quit ...
... Click on the picture above to watch a video from the history channel on the life cycle of a star! Quit ...
Supernova
A supernova is a stellar explosion that briefly outshines an entire galaxy, radiating as much energy as the Sun or any ordinary star is expected to emit over its entire life span, before fading from view over several weeks or months. The extremely luminous burst of radiation expels much or all of a star's material at a velocity of up to 7007300000000000000♠30,000 km/s (10% of the speed of light), driving a shock wave into the surrounding interstellar medium. This shock wave sweeps up an expanding shell of gas and dust called a supernova remnant. Supernovae are potentially strong galactic sources of gravitational waves. A great proportion of primary cosmic rays comes from supernovae.Supernovae are more energetic than novae. Nova means ""new"" in Latin, referring to what appears to be a very bright new star shining in the celestial sphere; the prefix ""super-"" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky in 1931. It is pronounced /ˌsuːpərnoʊvə/ with the plural supernovae /ˌsuːpərnoʊviː/ or supernovas (abbreviated SN, plural SNe after ""supernovae"").Supernovae can be triggered in one of two ways: by the sudden re-ignition of nuclear fusion in a degenerate star; or by the gravitational collapse of the core of a massive star. In the first case, a degenerate white dwarf may accumulate sufficient material from a companion, either through accretion or via a merger, to raise its core temperature, ignite carbon fusion, and trigger runaway nuclear fusion, completely disrupting the star. In the second case, the core of a massive star may undergo sudden gravitational collapse, releasing gravitational potential energy that can create a supernova explosion.The most recent directly observed supernova in the Milky Way was Kepler's Star of 1604 (SN 1604); remnants of two more recent supernovae have been found retrospectively. Observations in other galaxies indicate that supernovae should occur on average about three times every century in the Milky Way, and that any galactic supernova would almost certainly be observable in modern astronomical equipment. Supernovae play a significant role in enriching the interstellar medium with higher mass elements. Furthermore, the expanding shock waves from supernova explosions can trigger the formation of new stars.