How much radioactive nickel does ASASSN
... show that mass-loss rates reach several 10 −3 M⊙ yr −1 during core helium burning phases of 300 – 500 M⊙ rotating and non-rotating models (eWNE phase). The supernova shock smashes into the surrounding medium, and instead of the usual shock breakout the luminous supernovalike event is observed. This ...
... show that mass-loss rates reach several 10 −3 M⊙ yr −1 during core helium burning phases of 300 – 500 M⊙ rotating and non-rotating models (eWNE phase). The supernova shock smashes into the surrounding medium, and instead of the usual shock breakout the luminous supernovalike event is observed. This ...
Life Stages of High
... • Late life stages of high-mass stars are similar to those of low-mass stars: —Hydrogen core fusion (main sequence) ...
... • Late life stages of high-mass stars are similar to those of low-mass stars: —Hydrogen core fusion (main sequence) ...
Chapter 15, Galaxies
... and the white dwarf collapses, increasing temperature and density until it reaches carbon fusion temperature. • The carbon inside the white dwarfs are simultaneously ignited. It explodes to form a White dwarf supernova. (Type I). • Nothing is left behind from a white dwarf supernova explosion (In co ...
... and the white dwarf collapses, increasing temperature and density until it reaches carbon fusion temperature. • The carbon inside the white dwarfs are simultaneously ignited. It explodes to form a White dwarf supernova. (Type I). • Nothing is left behind from a white dwarf supernova explosion (In co ...
Lecture 15
... After a few million years After a few billion years It depends on its mass When the hydrogen fuel in its core is used up C and D ...
... After a few million years After a few billion years It depends on its mass When the hydrogen fuel in its core is used up C and D ...
CEA - Nuclear astrophysics
... – visible light tells us about the different nuclear reactions produced within the stars throughout their life; – radio waves, X-rays and gamma rays show us the sometimes very violent phenomena that occur at the end of a star’s life: supernovae, pulsars, neutron stars and black holes. By interpretin ...
... – visible light tells us about the different nuclear reactions produced within the stars throughout their life; – radio waves, X-rays and gamma rays show us the sometimes very violent phenomena that occur at the end of a star’s life: supernovae, pulsars, neutron stars and black holes. By interpretin ...
The Classification of Stellar Spectra
... it was in the single-shell burning phase, and due to the peculiar nature of degenerate matter, the more massive core is physically smaller. The gravity experienced by overlying layers is hence stronger, requiring higher luminosities to maintain the balance between pressure and gravity. Thus the star ...
... it was in the single-shell burning phase, and due to the peculiar nature of degenerate matter, the more massive core is physically smaller. The gravity experienced by overlying layers is hence stronger, requiring higher luminosities to maintain the balance between pressure and gravity. Thus the star ...
Stellar Evolution in the HR Diagram
... Electron degeneracy cannot support cores more massive than 1.4 M. If a degenerate C/O core (i.e., a white dwarf) is pushed above this limit, it was collapse and begin fusing, but it will not have time to adjust its structure (all the energy will just go into lifting the degeneracy). The star will b ...
... Electron degeneracy cannot support cores more massive than 1.4 M. If a degenerate C/O core (i.e., a white dwarf) is pushed above this limit, it was collapse and begin fusing, but it will not have time to adjust its structure (all the energy will just go into lifting the degeneracy). The star will b ...
Biography of a Star - Max-Planck
... Russell drew a simple system of coordinates with x- and y-axes, familiar to schoolchildren from geometry lessons. On this diagram, he entered the stars according to their spectral type or temperature (x-axis) and absolute brightness or luminosity (y-axis). Contrary to what might have been expected, ...
... Russell drew a simple system of coordinates with x- and y-axes, familiar to schoolchildren from geometry lessons. On this diagram, he entered the stars according to their spectral type or temperature (x-axis) and absolute brightness or luminosity (y-axis). Contrary to what might have been expected, ...
Luminosity - UCF Physics
... What the “computers” did was sift through literally 100’s of thousands of stellar spectra. Established a classification scheme based on Hydrogen lines…. The types were alphabetical….letters were assigned in declining strength of the H-lines ...
... What the “computers” did was sift through literally 100’s of thousands of stellar spectra. Established a classification scheme based on Hydrogen lines…. The types were alphabetical….letters were assigned in declining strength of the H-lines ...
slides
... Because stars are powered by nuclear reactions which consume star material, they have a finite life span. ...
... Because stars are powered by nuclear reactions which consume star material, they have a finite life span. ...
Life cycle of low mass stars
... Life cycle of High Mass stars: 5. Supernova All element greater than iron require energy, instead of releasing it. When a Red Supergiant reaches this stage the core condenses to attempt to create the energy need. The star collapses rapidly, creating a supernova Supernova = the explosion of a massiv ...
... Life cycle of High Mass stars: 5. Supernova All element greater than iron require energy, instead of releasing it. When a Red Supergiant reaches this stage the core condenses to attempt to create the energy need. The star collapses rapidly, creating a supernova Supernova = the explosion of a massiv ...
A105 Stars and Galaxies
... What about Massive Stars? • Massive stars continue to generate energy by nuclear reactions until they have converted all the hydrogen and helium in their cores into iron. • Once the core is iron, no more energy can be generated • The core collapses and the star explodes ...
... What about Massive Stars? • Massive stars continue to generate energy by nuclear reactions until they have converted all the hydrogen and helium in their cores into iron. • Once the core is iron, no more energy can be generated • The core collapses and the star explodes ...
Stellar Lifetime - Madison Public Schools
... • Nuclear reactions occur within the core of a star at tremendous temperatures and pressures. Explain what occurs in the core on an atomic level. What happens to an atom made up of many protons, neutrons, and electrons? What causes the particles to fuse together? How is energy released and where doe ...
... • Nuclear reactions occur within the core of a star at tremendous temperatures and pressures. Explain what occurs in the core on an atomic level. What happens to an atom made up of many protons, neutrons, and electrons? What causes the particles to fuse together? How is energy released and where doe ...
Power-point slides for Lecture 5
... MHC and is more conducive to explosion. Less electron capture, less neutrino escape, larger initial Ye could raise YL. ...
... MHC and is more conducive to explosion. Less electron capture, less neutrino escape, larger initial Ye could raise YL. ...
Chapter 6
... Thus this is roughly the trapped energy that will later be radiated in neutrinos. The trapped lepton fraction YL is a crucial parameter in the explosion physics: a higher trapped YL leads to a larger homologous core, a stronger shock wave, and easier passage of the shock wave through the outer core, ...
... Thus this is roughly the trapped energy that will later be radiated in neutrinos. The trapped lepton fraction YL is a crucial parameter in the explosion physics: a higher trapped YL leads to a larger homologous core, a stronger shock wave, and easier passage of the shock wave through the outer core, ...
Unit 1
... • a. Because this is the only phase that is common to all stars • b. because most stars die at the end of main sequence phase • c. because most stars in the sky are created at about the same time • d. because this is the longest lasting phase in each star life ...
... • a. Because this is the only phase that is common to all stars • b. because most stars die at the end of main sequence phase • c. because most stars in the sky are created at about the same time • d. because this is the longest lasting phase in each star life ...
Stars - Mike Brotherton
... Low luminosity; high temperature => White dwarfs are found in the lower center/left of the H-R diagram. ...
... Low luminosity; high temperature => White dwarfs are found in the lower center/left of the H-R diagram. ...
2017 Div. C (High School) Astronomy Help Session
... They are red giants – very late stages of stellar evolution for low mass stars, on the asymptotic giant branch, – will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years. Massive enough that they have undergone helium fusion in their cores but are les ...
... They are red giants – very late stages of stellar evolution for low mass stars, on the asymptotic giant branch, – will expel their outer envelopes as planetary nebulae and become white dwarfs within a few million years. Massive enough that they have undergone helium fusion in their cores but are les ...
NGC 3370 Spiral Galaxy
... • Stars form in clusters, with all types of stars forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the ...
... • Stars form in clusters, with all types of stars forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the ...
the summary
... turned into iron, there is no energy source to prevent the core from collapsing under the weight of the star. During the gravitational collapse that follows, a lot of energy is released and the object becomes very bright for a couple of days to weeks. This is the phenomenon we already mentioned: a s ...
... turned into iron, there is no energy source to prevent the core from collapsing under the weight of the star. During the gravitational collapse that follows, a lot of energy is released and the object becomes very bright for a couple of days to weeks. This is the phenomenon we already mentioned: a s ...
death_low_mass
... • Stars form in clusters, with all types of stars forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the ...
... • Stars form in clusters, with all types of stars forming. O,B,A,F,G,K,M • Spiral arms barely move, but gas clouds and stars orbit around the galaxy moving in and out of spiral arms • From the HR diagram, by far the most luminous stars are the O-type stars. Their luminosity can be 100,000 times the ...
Review: How does a star`s mass determine its life story?
... that nothing can move faster than light When electron speeds in white dwarf approach speed of light, electron degeneracy pressure can no longer support it ...
... that nothing can move faster than light When electron speeds in white dwarf approach speed of light, electron degeneracy pressure can no longer support it ...
Powerpoint
... the explosion. b) its distance was already known. c) it was observed early, as its light was still increasing. d) its evolution was captured with detailed images from the Hubble Space Telescope. e) All of the above are true. ...
... the explosion. b) its distance was already known. c) it was observed early, as its light was still increasing. d) its evolution was captured with detailed images from the Hubble Space Telescope. e) All of the above are true. ...
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.