Slide 1
... All of these are Type Ic All have broad line spectra -> ejection velocities ~ 50,000 km/s They account for 20% of the BL SN Ic = 2% of all SN Ic ...
... All of these are Type Ic All have broad line spectra -> ejection velocities ~ 50,000 km/s They account for 20% of the BL SN Ic = 2% of all SN Ic ...
PPT Slides - Center for Computational Sciences
... galaxies determined by the supersonic turbulent motions in the interstellar gas • Turbulence likely driven by combination of supernova explosions and galactic shear • Efficient star formation in young galaxies drives winds that can retard further growth of that galaxy and probably also nearby galaxi ...
... galaxies determined by the supersonic turbulent motions in the interstellar gas • Turbulence likely driven by combination of supernova explosions and galactic shear • Efficient star formation in young galaxies drives winds that can retard further growth of that galaxy and probably also nearby galaxi ...
Lect16-3-28-and-30-1..
... Each time the star’s core collapses further, the surrounding shell burning intensifies, and the star’s outer layers inflate further. Each time the core ignites again, the outer layers may contract a ...
... Each time the star’s core collapses further, the surrounding shell burning intensifies, and the star’s outer layers inflate further. Each time the core ignites again, the outer layers may contract a ...
Assessment Schedule
... Sun (electromagnetic radiation). On the other hand a brown dwarf has insufficient mass to start fusion process of hydrogen nuclei. Brown dwarfs are small in comparison to the sun and (emit only infra-red radiation). No luminosity. Evidence can be obtained from a ...
... Sun (electromagnetic radiation). On the other hand a brown dwarf has insufficient mass to start fusion process of hydrogen nuclei. Brown dwarfs are small in comparison to the sun and (emit only infra-red radiation). No luminosity. Evidence can be obtained from a ...
Level 2 Science (90764) 2011 Assessment Schedule
... Sun (electromagnetic radiation). On the other hand a brown dwarf has insufficient mass to start fusion process of hydrogen nuclei. Brown dwarfs are small in comparison to the sun and (emit only infra-red radiation). No luminosity. Evidence can be obtained from a ...
... Sun (electromagnetic radiation). On the other hand a brown dwarf has insufficient mass to start fusion process of hydrogen nuclei. Brown dwarfs are small in comparison to the sun and (emit only infra-red radiation). No luminosity. Evidence can be obtained from a ...
Instructor Notes
... Without the life and death of stars, there would be no rocky material from which to make terrestrial planets, there would be no oxygen to make water, and there would be no carbon, nitrogen, oxygen, or other materials with which to make life – we wouldn’t be here to take this class. ...
... Without the life and death of stars, there would be no rocky material from which to make terrestrial planets, there would be no oxygen to make water, and there would be no carbon, nitrogen, oxygen, or other materials with which to make life – we wouldn’t be here to take this class. ...
Document
... Many hundreds of neutron stars are known today; they appear mostly as pulsars: pulsating, starlike sources of radio and visible light, discovered in 1967 by Jocelyn Bell. The Oppenheimer-Volkoff theory of neutron stars, and their maximum mass, has been confirmed in all essentials. Theory and exp ...
... Many hundreds of neutron stars are known today; they appear mostly as pulsars: pulsating, starlike sources of radio and visible light, discovered in 1967 by Jocelyn Bell. The Oppenheimer-Volkoff theory of neutron stars, and their maximum mass, has been confirmed in all essentials. Theory and exp ...
Death of Stars • Models of Star behavior can give estimates of how
... • Big stars are already hot at their centers and don’t need to compress their cores much to get to this temperature. • If 0.4M < M < 3M , the degeneracy point is hit first, then the Temperature rises above 100 Million K and Helium fusion starts. • But the pressure doesn’t change with temperature, ...
... • Big stars are already hot at their centers and don’t need to compress their cores much to get to this temperature. • If 0.4M < M < 3M , the degeneracy point is hit first, then the Temperature rises above 100 Million K and Helium fusion starts. • But the pressure doesn’t change with temperature, ...
http://www.lanl.gov/orgs/adtsc/publications/science_highlights_2013/docs/Pg24_25.pdf
... combinations of progenitor properties. To perform a more controlled test of the accuracy of our code, we are beginning a project to match a simulation to SN 1987A. We chose this SN as a test case since it has been very consistently and thoroughly observed since it first exploded, due to its nearby l ...
... combinations of progenitor properties. To perform a more controlled test of the accuracy of our code, we are beginning a project to match a simulation to SN 1987A. We chose this SN as a test case since it has been very consistently and thoroughly observed since it first exploded, due to its nearby l ...
Document
... • 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 ...
Lecture Nine (Powerpoint format) - Flash
... Manufactured lenses for Naval Observatory (where Pluto’s moon Charon was discovered) and the University of Chicago Yerkes Observatory (which just shut down research very recently). In 1862, when testing a new 18 inch telescope at the Dearborn observatory at Northwestern University in Evanston, h ...
... Manufactured lenses for Naval Observatory (where Pluto’s moon Charon was discovered) and the University of Chicago Yerkes Observatory (which just shut down research very recently). In 1862, when testing a new 18 inch telescope at the Dearborn observatory at Northwestern University in Evanston, h ...
File - Mr. Catt`s Class
... Figure 14.25b: Cluster of stars with 7 white dwarfs Kitt Peak National Observatory 0.9-meter telescope, National Optical Astronomy Observatories; Courtesy M. Bolte (University of California, Santa Cruz) and Harvey Richer (University of British Columbia, Vancouver, Canada) and NASA ...
... Figure 14.25b: Cluster of stars with 7 white dwarfs Kitt Peak National Observatory 0.9-meter telescope, National Optical Astronomy Observatories; Courtesy M. Bolte (University of California, Santa Cruz) and Harvey Richer (University of British Columbia, Vancouver, Canada) and NASA ...
Neutron Stars
... Binary pulsars: two pulsars in orbit around each other. Einstein predicted that binary orbits should "decay", i.e. the masses would spiral in towards each other, losing energy through "gravitational radiation". Confirmed by binary pulsar. ...
... Binary pulsars: two pulsars in orbit around each other. Einstein predicted that binary orbits should "decay", i.e. the masses would spiral in towards each other, losing energy through "gravitational radiation". Confirmed by binary pulsar. ...
To understand the deaths of stars and how it depends on
... from main sequence to white dwarf (which for our sun would be 1 billion years after it leaves the main sequence). • White dwarfs are small and very hot. • With time they cool down. • There is no fusion, so they slowly loose energy and get cooler. ...
... from main sequence to white dwarf (which for our sun would be 1 billion years after it leaves the main sequence). • White dwarfs are small and very hot. • With time they cool down. • There is no fusion, so they slowly loose energy and get cooler. ...
Presentation
... Prialnik, Dina (2000). An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press. Stahler, S. W. & Palla, F. (2004). The Formation of Stars. Weinheim: Wiley-VCH. ...
... Prialnik, Dina (2000). An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press. Stahler, S. W. & Palla, F. (2004). The Formation of Stars. Weinheim: Wiley-VCH. ...
PowerPoint - Star Life Cycle
... Which of the following best describes the category in which the Sun would be placed? A. blue supergiant stars B. red giant stars C. yellow main sequence stars D. white dwarf stars ...
... Which of the following best describes the category in which the Sun would be placed? A. blue supergiant stars B. red giant stars C. yellow main sequence stars D. white dwarf stars ...
CHAPTER 14
... 7. Because of degeneracy, the core cannot cool by expanding and thus helium fusion reactions occur faster and faster. Helium flash is the process of runaway helium fusion reactions that occurs during the evolution of a red giant. 8. The end result of the helium flash is that the core heats up, the ...
... 7. Because of degeneracy, the core cannot cool by expanding and thus helium fusion reactions occur faster and faster. Helium flash is the process of runaway helium fusion reactions that occurs during the evolution of a red giant. 8. The end result of the helium flash is that the core heats up, the ...
Estimating the Age of Supernova Remnants - Chandra X
... Purpose: To use the observed size of the Cassiopeia A supernova remnant (SNR) from its X-ray image and an estimated rate of expansion to calculate its approximate age. Background: ...
... Purpose: To use the observed size of the Cassiopeia A supernova remnant (SNR) from its X-ray image and an estimated rate of expansion to calculate its approximate age. Background: ...
Lecture 13 Presupernova Models, Core Collapse and Bounce
... old astronomy text books), that the so called prompt shock mechanism – worked on extensively by Bethe, Brown, Baron, Cooperstein, and colleagues in the 1980 s – does not work. The shock fails and becomes in a short time (< 10 ms) an accretion shock. It will turn to neutrinos and other physics to act ...
... old astronomy text books), that the so called prompt shock mechanism – worked on extensively by Bethe, Brown, Baron, Cooperstein, and colleagues in the 1980 s – does not work. The shock fails and becomes in a short time (< 10 ms) an accretion shock. It will turn to neutrinos and other physics to act ...
Lecture 30
... Main-sequence lifetime is strongly mass-dependent, more massive stars: • sustain higher core temperatures • have higher rates of nuclear fusion • are more luminous and exhaust H fuel more quickly ...
... Main-sequence lifetime is strongly mass-dependent, more massive stars: • sustain higher core temperatures • have higher rates of nuclear fusion • are more luminous and exhaust H fuel more quickly ...
Evolution of our Sun
... What elements are created in a sun-like star? What elements are created in a massive star? Evolution of the Sun – Part 2 Name and briefly describe the stages that our sun will go through as it ages. About how long does our sun live as a main sequence star? About how much longer does Earth have until ...
... What elements are created in a sun-like star? What elements are created in a massive star? Evolution of the Sun – Part 2 Name and briefly describe the stages that our sun will go through as it ages. About how long does our sun live as a main sequence star? About how much longer does Earth have until ...
Document
... that there is a black hole that came from a massive star: – Strong X-ray sources (usually flares). – Optically dark objects (that is, only one star is seen in the spectrum, and it is the mass-losing one). – Masses too large to be a white dwarf or a neutron star. ...
... that there is a black hole that came from a massive star: – Strong X-ray sources (usually flares). – Optically dark objects (that is, only one star is seen in the spectrum, and it is the mass-losing one). – Masses too large to be a white dwarf or a neutron star. ...
Planetary Nebulae – White dwarfs
... • Low mass: < 2 times the Sun • Intermediate mass: 2-8 times the Sun • High mass: > 8 times the Sun ...
... • Low mass: < 2 times the Sun • Intermediate mass: 2-8 times the Sun • High mass: > 8 times the Sun ...
Mark Rubin
... this process. They have potential to yield enormous insight into the behavior of high-mass (> 140 Msolar) Pop III stars. • Moreover, SNe IIn are the most luminous SN type in the restframe UV, rendering them easier to detect at high redshift than any other SN type. • SNe IIn are defined by the presen ...
... this process. They have potential to yield enormous insight into the behavior of high-mass (> 140 Msolar) Pop III stars. • Moreover, SNe IIn are the most luminous SN type in the restframe UV, rendering them easier to detect at high redshift than any other SN type. • SNe IIn are defined by the presen ...
White Dwarfs
... Eventually at ρ greater than about 10 7 g cm −3 electrons in the central part of the white dwarf start to move close to the speed of light. As the mass continues to grow, a larger fraction of the star is supported by relativistic electron degeneracy pressure. Consider the limit: GM ρ ...
... Eventually at ρ greater than about 10 7 g cm −3 electrons in the central part of the white dwarf start to move close to the speed of light. As the mass continues to grow, a larger fraction of the star is supported by relativistic electron degeneracy pressure. Consider the limit: GM ρ ...
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.