Birth and Death of Stars
... energy to the outer shell of hydrogen which allows fusion to continue. This ongoing fusion radiates energy outward and the outer shell expands and cools creating a red supergiant. ...
... energy to the outer shell of hydrogen which allows fusion to continue. This ongoing fusion radiates energy outward and the outer shell expands and cools creating a red supergiant. ...
Please read the following excerpt from an editorial about the Atkins
... Please read each passage carefully and rate how difficult it was to read on the 6 point scale. You will be given 13 minutes to read them. Later you will be asked several questions about each passage. Supernova Supernovae are stupendous explosions that destroy an entire star. The "nova" ("new") part ...
... Please read each passage carefully and rate how difficult it was to read on the 6 point scale. You will be given 13 minutes to read them. Later you will be asked several questions about each passage. Supernova Supernovae are stupendous explosions that destroy an entire star. The "nova" ("new") part ...
Chapter 13 The Life of a Star The Life of a Star Mass Is the Key The
... supernova explosion sweeping up interstellar material as it goes is called a supernova remnant – During a 1-100 year time frame, a supernova will expand from 0.03 ly to several light-years in diameter – Supernova remnants have a more ragged look compared to planetary and other nebulae ...
... supernova explosion sweeping up interstellar material as it goes is called a supernova remnant – During a 1-100 year time frame, a supernova will expand from 0.03 ly to several light-years in diameter – Supernova remnants have a more ragged look compared to planetary and other nebulae ...
Chapter 13
... • Objects with masses between planets and are called brown dwarfs, “failed stars” extremely dim and difficult to observe • Upper mass limit of stars (about 30 M) due to extreme temperatures and luminosity preventing additional material from falling on them - intense radiation may even strip off out ...
... • Objects with masses between planets and are called brown dwarfs, “failed stars” extremely dim and difficult to observe • Upper mass limit of stars (about 30 M) due to extreme temperatures and luminosity preventing additional material from falling on them - intense radiation may even strip off out ...
14-1 Reading Questions: Neutron Stars
... __________, can be left as a remnant after a type ______ supernova explosion. A neutron star’s density is so high that physicists calculate that this material is stable only as a ___________________________. Theory predicts that such an object would spin _____________ times per second, have a surfac ...
... __________, can be left as a remnant after a type ______ supernova explosion. A neutron star’s density is so high that physicists calculate that this material is stable only as a ___________________________. Theory predicts that such an object would spin _____________ times per second, have a surfac ...
Astrophysical explosions: from solar flares to cosmic gamma
... collapse supernovae and cosmic gamma-ray bursts, each representing a different type and amount of energy release. This paper summarizes the properties of these explosions and describes new research on thermonuclear explosions and explosions in extended circumstellar media. Parallels are drawn betwee ...
... collapse supernovae and cosmic gamma-ray bursts, each representing a different type and amount of energy release. This paper summarizes the properties of these explosions and describes new research on thermonuclear explosions and explosions in extended circumstellar media. Parallels are drawn betwee ...
UCLA 2004
... When 1 Ori C goes supernova, all the disks in the Orion Nebula will be pelted with radioactive ejecta Even more true for the disks observed in Carina Nebula, with sixty O stars [Smith et al. (2003)], many other H II regions Ejecta dust grains penetrate disk, evaporate on entry, but leave SLRs lodg ...
... When 1 Ori C goes supernova, all the disks in the Orion Nebula will be pelted with radioactive ejecta Even more true for the disks observed in Carina Nebula, with sixty O stars [Smith et al. (2003)], many other H II regions Ejecta dust grains penetrate disk, evaporate on entry, but leave SLRs lodg ...
unit notes filled out
... The most massive stars can get hot enough to fuse carbon and other elements. After they go through the giant stage they eventually fuse elements through iron. Iron cannot release energy through fusion reactions, as a result the core becomes unstable and produces a supernova explosion. The final ...
... The most massive stars can get hot enough to fuse carbon and other elements. After they go through the giant stage they eventually fuse elements through iron. Iron cannot release energy through fusion reactions, as a result the core becomes unstable and produces a supernova explosion. The final ...
Acceleration of Coronal Mass Ejection In Long Rising Solar
... The core collapses at the dynamic time scale, i.e. seconds For a core of 1.2 Ms contracting from a density of 109 cm-3 (degenerate electron state, Earth size) to 1015 cm-3 (neutron star, city size), it releases the gravitational energy in the order of 1053 ergs, comparable to the energy released by ...
... The core collapses at the dynamic time scale, i.e. seconds For a core of 1.2 Ms contracting from a density of 109 cm-3 (degenerate electron state, Earth size) to 1015 cm-3 (neutron star, city size), it releases the gravitational energy in the order of 1053 ergs, comparable to the energy released by ...
The Sizes of Stars
... When all the hydrogen in a stellar core is changed to helium, there is no more energy to hold it up. Gravity takes over and the core contracts. This produces energy. In the area right surrounding the core, there is plenty of hydrogen. The pressure in this area increases (since contraction increases ...
... When all the hydrogen in a stellar core is changed to helium, there is no more energy to hold it up. Gravity takes over and the core contracts. This produces energy. In the area right surrounding the core, there is plenty of hydrogen. The pressure in this area increases (since contraction increases ...
Introduction to Astronomy
... • Leaves behind no remnant – Just an expanding cloud of heavy elements (C, O, Si, Ni, Co, Fe, etc) ...
... • Leaves behind no remnant – Just an expanding cloud of heavy elements (C, O, Si, Ni, Co, Fe, etc) ...
Chapter 12 Star Stuff How do stars form?
... The relationship between apparent brightness and luminosity depends on distance: ...
... The relationship between apparent brightness and luminosity depends on distance: ...
white dwarf supernova
... 2) Which supernova shows no hydrogen lines in its spectrum? Type I – White dwarf supernova Type II – Massive star supernova They both show hydrogen lines ...
... 2) Which supernova shows no hydrogen lines in its spectrum? Type I – White dwarf supernova Type II – Massive star supernova They both show hydrogen lines ...
Section 14
... time, however, helium is fused to create lithium, beryllium and other elements. Since the core of the star is hotter, the outer shell of the star expands. This expansion is actually great enough that although the star is emitting more energy, it's through a greater surface area and the star's surfac ...
... time, however, helium is fused to create lithium, beryllium and other elements. Since the core of the star is hotter, the outer shell of the star expands. This expansion is actually great enough that although the star is emitting more energy, it's through a greater surface area and the star's surfac ...
PHY111 Stellar Evolution
... luminosity as they evolve, but do change in colour (so they must change in size) ...
... luminosity as they evolve, but do change in colour (so they must change in size) ...
Gold could have come from colliding stars - Horizon Magazine
... ‘The formation of heavy elements is a major topic in stellar astrophysics,’ said Dr Bauswein. ‘We want to understand where and how elements like gold and uranium were produced.’ Our own fairly small star, the sun, can generate helium by fusing pairs of atoms of the lightest element, hydrogen, at tem ...
... ‘The formation of heavy elements is a major topic in stellar astrophysics,’ said Dr Bauswein. ‘We want to understand where and how elements like gold and uranium were produced.’ Our own fairly small star, the sun, can generate helium by fusing pairs of atoms of the lightest element, hydrogen, at tem ...
Life Stages of High
... • Observations of star clusters show that a star becomes larger, redder, and more luminous after its time on the main sequence is over. ...
... • Observations of star clusters show that a star becomes larger, redder, and more luminous after its time on the main sequence is over. ...
Lecture 15, PPT version
... At their maximum brightness, supernovae are as bright as an entire galaxy. ...
... At their maximum brightness, supernovae are as bright as an entire galaxy. ...
ppt - Astronomy & Physics
... Last time we considered the stellar properties in detail: including structure, what we know about it, and how nuclear fusion powers stars ...
... Last time we considered the stellar properties in detail: including structure, what we know about it, and how nuclear fusion powers stars ...
Announcements
... Is a BH a hole in the universe How can we know anything about them How can we find them Can one live forever inside them What is on the other side Why does time run slower How can more heat make gravity stronger Where does stuff go that falls into them ...
... Is a BH a hole in the universe How can we know anything about them How can we find them Can one live forever inside them What is on the other side Why does time run slower How can more heat make gravity stronger Where does stuff go that falls into them ...
Energy Transport in the Sun
... emission of neutrinos Core collapse stops, neutron star is formed Rest of the star collapses in on the core, but bounces off the new neutron star (also pushed outwards by the neutrinos) ...
... emission of neutrinos Core collapse stops, neutron star is formed Rest of the star collapses in on the core, but bounces off the new neutron star (also pushed outwards by the neutrinos) ...
The Ultraluminous X-ray Source in Holmberg IX and its Environment
... mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX X-1, located at a distance of 3.6 Mpc in a dwarf galaxy companion of M81. Miller ...
... mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX X-1, located at a distance of 3.6 Mpc in a dwarf galaxy companion of M81. Miller ...
Slide 1
... • M > 4 M (Sun) – O and B stars • Burn H He via the more efficient CNO cycle • After H-core exhaustion the He-core contracts and heats up, but the H-burning continues around the He-core and the star puffs up • The star expands and cools, but the luminosity remains constant since the huge outer lay ...
... • M > 4 M (Sun) – O and B stars • Burn H He via the more efficient CNO cycle • After H-core exhaustion the He-core contracts and heats up, but the H-burning continues around the He-core and the star puffs up • The star expands and cools, but the luminosity remains constant since the huge outer lay ...
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.