Powerpoint for today
... C: a black hole + expanding shell D: no remnant, just the expanding shell ...
... C: a black hole + expanding shell D: no remnant, just the expanding shell ...
Background Presentation
... 2. Knots came from star, were blown out by the supernova, and travel at a constant velocity in a constant direction 3. If we can calculate that velocity, we can calculate how long to get from the star to the “current” location ...
... 2. Knots came from star, were blown out by the supernova, and travel at a constant velocity in a constant direction 3. If we can calculate that velocity, we can calculate how long to get from the star to the “current” location ...
“Astronomy Picture of the Day” Leads to a Research Breakthrough
... the thermonuclear explosion of a carbon-oxygen white dwarf that has reached the Chandrasekhar mass limit (1.4 times the mass of the sun, i.e., MCh = 1.4 Msol), these supernovae provide the best cosmological distance measurements in modern astronomy because of the supposedly identical nature of their ...
... the thermonuclear explosion of a carbon-oxygen white dwarf that has reached the Chandrasekhar mass limit (1.4 times the mass of the sun, i.e., MCh = 1.4 Msol), these supernovae provide the best cosmological distance measurements in modern astronomy because of the supposedly identical nature of their ...
the 82nd arthur h. compton lecture series
... of low-mass, there are a lot of binary systems composed of two stars with slightly different masses, yet still “low-mass”. ...
... of low-mass, there are a lot of binary systems composed of two stars with slightly different masses, yet still “low-mass”. ...
Powerpoint Presentation (large file)
... • An accreting white dwarf in a close binary system can also become a supernova when carbon fusion ignites explosively throughout such a degenerate star ...
... • An accreting white dwarf in a close binary system can also become a supernova when carbon fusion ignites explosively throughout such a degenerate star ...
Astronomy 115 Homework Set #1 – Due: Thursday, Feb
... In what ways did supernova 1987A confirm our models of supernova explosions? In what ways did it challenge it? ...
... In what ways did supernova 1987A confirm our models of supernova explosions? In what ways did it challenge it? ...
1. Neutron stars 2. Black holes
... The star implodes! (falls in on itself!) Core temperature rises again, all heavy elements in core undergo Photodisintegration, undoing the fusion process of the previous 10 million years. End up with electrons, protons, neutrons, and photons in core. Core compresses, stops and rebounds with a vengea ...
... The star implodes! (falls in on itself!) Core temperature rises again, all heavy elements in core undergo Photodisintegration, undoing the fusion process of the previous 10 million years. End up with electrons, protons, neutrons, and photons in core. Core compresses, stops and rebounds with a vengea ...
g9u4c12part3
... burn their hydrogen fuel very slowly 100 billion years. Die as hot dim white dwarfs and quietly burn out. ...
... burn their hydrogen fuel very slowly 100 billion years. Die as hot dim white dwarfs and quietly burn out. ...
Chapter 13
... The End of a Star’s Life When all the nuclear fuel in a star is used up, gravity will win over pressure and the star will die. ...
... The End of a Star’s Life When all the nuclear fuel in a star is used up, gravity will win over pressure and the star will die. ...
Supernova scrutiny: Astronomers look inside the heart of a dying
... The observations captured by NuSTAR have led the astronomers to believe that the explosion was shaped by pressure inside the iron core of the dying star “sloshing” about; an asymmetrical process (below) that could explain why supernova remnants look so crooked compared to the spherical stars they on ...
... The observations captured by NuSTAR have led the astronomers to believe that the explosion was shaped by pressure inside the iron core of the dying star “sloshing” about; an asymmetrical process (below) that could explain why supernova remnants look so crooked compared to the spherical stars they on ...
ASTRONOMY 120
... strong lines from these elements. Type-II supernovae fuse more mass than Type-I supernovae, and thus get brighter and linger longer. 9. Chaisson Review and Discussion 21.11 What evidence is there that many supernovae have occurred in our Galaxy? (3 points) When the supernova explosion occurs, it rap ...
... strong lines from these elements. Type-II supernovae fuse more mass than Type-I supernovae, and thus get brighter and linger longer. 9. Chaisson Review and Discussion 21.11 What evidence is there that many supernovae have occurred in our Galaxy? (3 points) When the supernova explosion occurs, it rap ...
tire
... 6. The oscillations of space caused the rapid movement of matter, such as a supernova or orbiting black holes. 7. An object whose gravity is so strong that the escape speed exceeds the speed of light. 8. A type of yellow supergiant pulsating star. 9. A starlike object that is not massive enough to i ...
... 6. The oscillations of space caused the rapid movement of matter, such as a supernova or orbiting black holes. 7. An object whose gravity is so strong that the escape speed exceeds the speed of light. 8. A type of yellow supergiant pulsating star. 9. A starlike object that is not massive enough to i ...
Starending jeopardy
... Once hydrogen is depleted it can no longer fuse hydrogen into helium. With no energy source to cause outware pressure the gravity is able to collapse the core and change the star’s structure. ...
... Once hydrogen is depleted it can no longer fuse hydrogen into helium. With no energy source to cause outware pressure the gravity is able to collapse the core and change the star’s structure. ...
Supernova worksheet with solutions ()
... In low-mass stars, the core never gets hot or dense enough to fuse carbon and oxygen into heavier elements. Once the helium is used up, the core is able to stave off gravitational collapse with a new source of pressure: electron degeneracy pressure. This is a quantum mechanical effect similar to the ...
... In low-mass stars, the core never gets hot or dense enough to fuse carbon and oxygen into heavier elements. Once the helium is used up, the core is able to stave off gravitational collapse with a new source of pressure: electron degeneracy pressure. This is a quantum mechanical effect similar to the ...
Lecture 18: Supernovae
... and carry off energy Makes the core collapse faster, as the insufficient pressure is decreased further ...
... and carry off energy Makes the core collapse faster, as the insufficient pressure is decreased further ...
Stellar Explosions
... Within the cores of the most massive stars, neutron capture can create heavier elements, all the way up to bismuth-209 Heaviest elements are made during the first few seconds of a supernova explosion ...
... Within the cores of the most massive stars, neutron capture can create heavier elements, all the way up to bismuth-209 Heaviest elements are made during the first few seconds of a supernova explosion ...
Lecture 16 - Yet More Evolution of Stars
... • Solar mass star produce elements up to Carbon and Oxygen – these are ejected into planetary nebula and then recycled into new stars and planets • Supernova produce all of the heavier elements – Elements up to Iron can be produced by fusion – Elements heavier than iron are produced by the neutrons ...
... • Solar mass star produce elements up to Carbon and Oxygen – these are ejected into planetary nebula and then recycled into new stars and planets • Supernova produce all of the heavier elements – Elements up to Iron can be produced by fusion – Elements heavier than iron are produced by the neutrons ...
Deep Space Mystery Note Form 3
... formation process is growing. American astronomers Rudolph Minkowski and Fritz Zwicky developed the modern supernova classification scheme beginning in 1941. In the 1960s astronomers found that the maximum intensities of supernova explosions could be used as standard candles, hence indicators of ast ...
... formation process is growing. American astronomers Rudolph Minkowski and Fritz Zwicky developed the modern supernova classification scheme beginning in 1941. In the 1960s astronomers found that the maximum intensities of supernova explosions could be used as standard candles, hence indicators of ast ...
File
... A. Core-collapse of massive star B. Rebounding shock wave blows outer layers of star into space C. As bright as an entire galaxy! D. Signature: 1. Abundance of H2 2. Plateau in light curve ...
... A. Core-collapse of massive star B. Rebounding shock wave blows outer layers of star into space C. As bright as an entire galaxy! D. Signature: 1. Abundance of H2 2. Plateau in light curve ...
No Slide Title
... • Type Ia come from binary star systems that have one member that is a white dwarf (WD). • The WD is less than 1.4 solar masses ...
... • Type Ia come from binary star systems that have one member that is a white dwarf (WD). • The WD is less than 1.4 solar masses ...
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.