Lectures 12 & 13 powerpoint (stellar death)
... into smaller nuclei, and the A: As the matter falls inward, it creates a degenerate electrons that shockwave that travels outward. supported the core are This shockwave is aided by two additional removed core contracts sources of energy; 2. T so high that the average 1. The disrupted nuclei in the ...
... into smaller nuclei, and the A: As the matter falls inward, it creates a degenerate electrons that shockwave that travels outward. supported the core are This shockwave is aided by two additional removed core contracts sources of energy; 2. T so high that the average 1. The disrupted nuclei in the ...
Stellar Explosions
... Supernova explosions are very energetic events. By studying supernovae and their remnants in multiwavelengths, astronomers gain a clearer picture of the death of massive stars and their effect on the gas and dust of the interstellar medium surrounding them. The supernova blasts from massive stars ca ...
... Supernova explosions are very energetic events. By studying supernovae and their remnants in multiwavelengths, astronomers gain a clearer picture of the death of massive stars and their effect on the gas and dust of the interstellar medium surrounding them. The supernova blasts from massive stars ca ...
16.1 A Little History
... this observation suggests that Type Ia SNe can have long-lived, low-mass progenitors. In contrast, Types II, Ib and Ic are associated with regions of star formation in spiral galaxies, and therefore are likely to have shortlived, high-mass progenitors. These observations have led to the current vie ...
... this observation suggests that Type Ia SNe can have long-lived, low-mass progenitors. In contrast, Types II, Ib and Ic are associated with regions of star formation in spiral galaxies, and therefore are likely to have shortlived, high-mass progenitors. These observations have led to the current vie ...
42 SCIENTIFIC AMERICAN OCTOBER 2006 TEN
... Fred Hoyle of the University of Cambridge and Willy Fowler of Caltech conceived of the explosions as giant nuclear bombs. When a sunlike star exhausts its hydrogen fuel and then its helium, it turns to its carbon and oxygen. Not only can the fusion of these elements release a titanic pulse of energy ...
... Fred Hoyle of the University of Cambridge and Willy Fowler of Caltech conceived of the explosions as giant nuclear bombs. When a sunlike star exhausts its hydrogen fuel and then its helium, it turns to its carbon and oxygen. Not only can the fusion of these elements release a titanic pulse of energy ...
Stellar evolution
... • The implosion produces enough energy to create a supernova. • The supernova can last weeks or months, and release as much energy as the sun does in its entire lifespan. • The supernova is a main source of heavy elements in the universe. • The remaining core will collapse into either a neutron star ...
... • The implosion produces enough energy to create a supernova. • The supernova can last weeks or months, and release as much energy as the sun does in its entire lifespan. • The supernova is a main source of heavy elements in the universe. • The remaining core will collapse into either a neutron star ...
Chapter20
... 1. For main sequence stars, radius increases as mass increases. For white dwarf stars, radius decreases as mass increases. 2. The Chandrasekhar limit, the maximum mass a white dwarf can have, is 1.4 solar masses. 3. The more massive white dwarf is dimmer because it is smaller and has less surface to ...
... 1. For main sequence stars, radius increases as mass increases. For white dwarf stars, radius decreases as mass increases. 2. The Chandrasekhar limit, the maximum mass a white dwarf can have, is 1.4 solar masses. 3. The more massive white dwarf is dimmer because it is smaller and has less surface to ...
After Dark M S
... both are supernovas, the natures of these two exploding stars are very different. The supernova in M51 may mark the death of a massive star. The supernova in M101 may mark the death of a white dwarf star in a binary star system. The discovery and origins of these two exploding stars, more than 20 mi ...
... both are supernovas, the natures of these two exploding stars are very different. The supernova in M51 may mark the death of a massive star. The supernova in M101 may mark the death of a white dwarf star in a binary star system. The discovery and origins of these two exploding stars, more than 20 mi ...
Life Cycle of a Star
... The core that is leftover after a supernova may form a ______________ star. If the leftover core was above a certain mass, it will continue to collapse in on itself and form a _______ _________. Its gravity is so powerful that nothing within its range can escape, not even _______! ...
... The core that is leftover after a supernova may form a ______________ star. If the leftover core was above a certain mass, it will continue to collapse in on itself and form a _______ _________. Its gravity is so powerful that nothing within its range can escape, not even _______! ...
Lifecycle of a Star
... A white dwarf may only be the size of Earth, but it has a mass equal to ½ of the Sun. ...
... A white dwarf may only be the size of Earth, but it has a mass equal to ½ of the Sun. ...
Slide 1
... 3. Nova and Supernova Type Ia: A binary with a white dwarf and a red giant creates an explosion. Mass from the red giant is pulled onto the surface of the white dwarf until it reaches 1.43 solar masses—critical mass. ...
... 3. Nova and Supernova Type Ia: A binary with a white dwarf and a red giant creates an explosion. Mass from the red giant is pulled onto the surface of the white dwarf until it reaches 1.43 solar masses—critical mass. ...
Stellar Evolution
... … another one, observed Energy equivalent to the entire mass by us with the MDM 1.3 m of the sun (E = mc2), converted into gamma-rays in just a few seconds! telescope on Kitt Peak! ...
... … another one, observed Energy equivalent to the entire mass by us with the MDM 1.3 m of the sun (E = mc2), converted into gamma-rays in just a few seconds! telescope on Kitt Peak! ...
White Dwarfs
... b. They are too dim for our present-day telescopes to detect. c. Astronomers are not motivated to search for such objects. d. They are all too distant (in theory) to be detected. e. Our galaxy is too young for any to have formed. ...
... b. They are too dim for our present-day telescopes to detect. c. Astronomers are not motivated to search for such objects. d. They are all too distant (in theory) to be detected. e. Our galaxy is too young for any to have formed. ...
Evolution of Close Binary Systems
... • In the early 1900s `novae’ were sometimes observed in other galaxies and were used to help set the distances to galaxies. • But, when it became clear that even the nearest galaxies were much further away than anyone had thought this suggested that the extragalactic `nova’ were much brighter than G ...
... • In the early 1900s `novae’ were sometimes observed in other galaxies and were used to help set the distances to galaxies. • But, when it became clear that even the nearest galaxies were much further away than anyone had thought this suggested that the extragalactic `nova’ were much brighter than G ...
What is a star`s life cycle?
... ____________________ 1. A star changes its heat into energy. ____________________ 2. In 1987, a protostar was observed in the Large Magellanic Cloud. ____________________ 3. During nuclear reactions in large stars, helium is changed into carbon. ____________________ 4. A star stays in the main seque ...
... ____________________ 1. A star changes its heat into energy. ____________________ 2. In 1987, a protostar was observed in the Large Magellanic Cloud. ____________________ 3. During nuclear reactions in large stars, helium is changed into carbon. ____________________ 4. A star stays in the main seque ...
The Lives of Stars
... The increased oudlow of energy will push out the outer layers, which will cool and become red. The sun will become a “Red Giant”. ...
... The increased oudlow of energy will push out the outer layers, which will cool and become red. The sun will become a “Red Giant”. ...
Investigating Supernova Remnants - Chandra X
... MWG occurred ~146 years ago. Because supernovas are rare within any galaxy, obtaining a good sample of supernovas to study requires regular monitoring of many galaxies. In the Large Magellanic Cloud galaxy, one hundred and sixty thousand (160,000) light years away, a supernova event took place in 19 ...
... MWG occurred ~146 years ago. Because supernovas are rare within any galaxy, obtaining a good sample of supernovas to study requires regular monitoring of many galaxies. In the Large Magellanic Cloud galaxy, one hundred and sixty thousand (160,000) light years away, a supernova event took place in 19 ...
The Story of Pulsational Pair-Instability SNe
... Do pair instability ejections have to be the mechanism by which the envelope is removed? It seems like any stellar wind followed by any explosion would lead to high speed collisions of gas. What is special about the pair instability ejections that make them more likely than other scenarios? Last wee ...
... Do pair instability ejections have to be the mechanism by which the envelope is removed? It seems like any stellar wind followed by any explosion would lead to high speed collisions of gas. What is special about the pair instability ejections that make them more likely than other scenarios? Last wee ...
answers - Salem State University
... larger. In instellar medium (ISM) where there is not sufficient gravity to force the materials of the ISM to contract, the pressure will be lower than in a star or on most planets. 10. There is larger nuclear fusion (more energy and emission) in a high mass due to gravity increasing the pressure and ...
... larger. In instellar medium (ISM) where there is not sufficient gravity to force the materials of the ISM to contract, the pressure will be lower than in a star or on most planets. 10. There is larger nuclear fusion (more energy and emission) in a high mass due to gravity increasing the pressure and ...
Unit 8 Astronomy
... All stars spend the majority of their lives fusing __________ the main hydrogen into ________________: helium sequence. When all of the __________ hydrogen in the central regions is converted to helium, the star will begin to “burn” carbon helium into _______________. sun Stars heavier than about 5 ...
... All stars spend the majority of their lives fusing __________ the main hydrogen into ________________: helium sequence. When all of the __________ hydrogen in the central regions is converted to helium, the star will begin to “burn” carbon helium into _______________. sun Stars heavier than about 5 ...
The Lifecycle of Stars
... When A Star Dies Supernova Some massive stars may explode in a large, bright display called a Supernova Supernova occur when a massive star collapses and throws its outer layers into space. This explosion is so powerful that it can be brighter than an entire galaxy for several days!! ...
... When A Star Dies Supernova Some massive stars may explode in a large, bright display called a Supernova Supernova occur when a massive star collapses and throws its outer layers into space. This explosion is so powerful that it can be brighter than an entire galaxy for several days!! ...
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.