Lecture 10 - University of Minnesota
... • This picture is confirmed by observations – Young stars have higher metallicities – Even numbered elements much more common than odd numbered elements ...
... • This picture is confirmed by observations – Young stars have higher metallicities – Even numbered elements much more common than odd numbered elements ...
Astronomy 5682 Problem Set 6: Supernova Cosmology Due
... is well defined even at redshifts large enough that the Doppler formula and Hubble’s law begin to break down. When a supernova explodes, its brightness increases rapidly, reaches a maximum, then declines over the course of a few weeks. There are at least two broad classes of supernovae, ones produce ...
... is well defined even at redshifts large enough that the Doppler formula and Hubble’s law begin to break down. When a supernova explodes, its brightness increases rapidly, reaches a maximum, then declines over the course of a few weeks. There are at least two broad classes of supernovae, ones produce ...
Powerpoint
... “With all reserve we advance the view that a supernova represents the transition of an ordinary star into a neutron star consisting mainly of neutrons. Such a star may possess a very small radius and an extremely high density. As neutrons can be packed much more closely than ordinary nuclei and elec ...
... “With all reserve we advance the view that a supernova represents the transition of an ordinary star into a neutron star consisting mainly of neutrons. Such a star may possess a very small radius and an extremely high density. As neutrons can be packed much more closely than ordinary nuclei and elec ...
ppt - ciera
... Chandra and XMM fields reveals no new 530 s pulsars, so there is a <0.5% chance of finding a magnetar in any field (Nechita, Gaensler, Muno, et al. in prep). • The pulsar is well within the cluster, with a <10% chance of being an unrelated X-ray source. ...
... Chandra and XMM fields reveals no new 530 s pulsars, so there is a <0.5% chance of finding a magnetar in any field (Nechita, Gaensler, Muno, et al. in prep). • The pulsar is well within the cluster, with a <10% chance of being an unrelated X-ray source. ...
Stellar Evolution after the Main Sequence
... Supernova What if the hydrogen layer is deposited more quickly and so that it doesn’t have the time to heat up enough to 'flash' into a nova, but instead just adds mass to the white dwarf? ...
... Supernova What if the hydrogen layer is deposited more quickly and so that it doesn’t have the time to heat up enough to 'flash' into a nova, but instead just adds mass to the white dwarf? ...
Test 1 - Brock physics
... (c) the radius of the region around a neutron star within which X-ray bursts occur. (d) the radius of the region around a black hole within which not even light can escape. 35. Neutron stars with masses greater than about 3 solar masses do not exist because neutron degeneracy pressure is not strong ...
... (c) the radius of the region around a neutron star within which X-ray bursts occur. (d) the radius of the region around a black hole within which not even light can escape. 35. Neutron stars with masses greater than about 3 solar masses do not exist because neutron degeneracy pressure is not strong ...
kaekae14 dae dae15 lifecycleofastar
... The most common red giants are the so-called red giant branch stars (RGB stars) whose shells are still fusing hydrogen into helium, while the core is inactive helium. Red giants are stars with radii tens to hundreds of times larger than that of the Sun which have exhausted the supply of hydrogen ...
... The most common red giants are the so-called red giant branch stars (RGB stars) whose shells are still fusing hydrogen into helium, while the core is inactive helium. Red giants are stars with radii tens to hundreds of times larger than that of the Sun which have exhausted the supply of hydrogen ...
Supernovae and Gamma-Ray Bursts (draft)
... by this interaction with the circumstellar material. Supernovae (e.g., § 8.3) that show evidence for such interactions are sometimes referred to as Type IIa supernovae (SNe IIa), though how this fits into the overall supernova scheme and, in particular, its relation to SNe IIb devies any obvious log ...
... by this interaction with the circumstellar material. Supernovae (e.g., § 8.3) that show evidence for such interactions are sometimes referred to as Type IIa supernovae (SNe IIa), though how this fits into the overall supernova scheme and, in particular, its relation to SNe IIb devies any obvious log ...
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. ...
Ch_16-18_Example_Exam
... a. The luminosity would increase because the star would become a nova. b. The luminosity would increase because the star’s central pressure would rise and the rate of nuclear reactions would increase. c. The luminosity would decrease because the outgoing energy has to pass through more layers in the ...
... a. The luminosity would increase because the star would become a nova. b. The luminosity would increase because the star’s central pressure would rise and the rate of nuclear reactions would increase. c. The luminosity would decrease because the outgoing energy has to pass through more layers in the ...
Neutron Stars
... What is a pulsar? A. A neutron star emitting pulses of light. B. A white dwarf emitting pulses of hydrogen gas. C. A red giant expanding and contracting in very short (millisecond) pulses. D. A powerful gamma ray burst. ...
... What is a pulsar? A. A neutron star emitting pulses of light. B. A white dwarf emitting pulses of hydrogen gas. C. A red giant expanding and contracting in very short (millisecond) pulses. D. A powerful gamma ray burst. ...
Phys 100 – Astronomy (Dr. Ilias Fernini) Review Questions for
... c. occurs when carbon and oxygen combine to form nitrogen, which produces energy. d. produces the energy responsible for bipolar flows. * e. combines four hydrogen nuclei to form one helium nucleus, which produces energy. 31. The region of the sun just below the photosphere a. is undergoing thermonu ...
... c. occurs when carbon and oxygen combine to form nitrogen, which produces energy. d. produces the energy responsible for bipolar flows. * e. combines four hydrogen nuclei to form one helium nucleus, which produces energy. 31. The region of the sun just below the photosphere a. is undergoing thermonu ...
Quiz on Chapter 11
... black holes lose mass by emitting photons from their interiors c) black holes lose mass by creating particles outside themselves X d) black holes lose mass by accreting matter from binary companions and then exploding that matter off their surfaces 11-26. A friend takes a ride on a spaceship to a di ...
... black holes lose mass by emitting photons from their interiors c) black holes lose mass by creating particles outside themselves X d) black holes lose mass by accreting matter from binary companions and then exploding that matter off their surfaces 11-26. A friend takes a ride on a spaceship to a di ...
Neutron Stars
... What is a pulsar? A. A neutron star emitting pulses of light. B. A white dwarf emitting pulses of hydrogen gas. C. A red giant expanding and contracting in very short (millisecond) pulses. D. A powerful gamma ray burst. ...
... What is a pulsar? A. A neutron star emitting pulses of light. B. A white dwarf emitting pulses of hydrogen gas. C. A red giant expanding and contracting in very short (millisecond) pulses. D. A powerful gamma ray burst. ...
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 ...
supernova remnants: a link between massive stars and the
... been accreting matter from a non-degenerate companion star, a donor that survives the explosion (see Branch 2001 for a review of current models for low mass SNe). Massive stars, on the other hand, presumably evolve from the main sequence to red giants and have a series of nuclear burning stages prod ...
... been accreting matter from a non-degenerate companion star, a donor that survives the explosion (see Branch 2001 for a review of current models for low mass SNe). Massive stars, on the other hand, presumably evolve from the main sequence to red giants and have a series of nuclear burning stages prod ...
Stars Part Two
... event horizon due to the Heisenberg uncertainty principle. 2. When stars orbit a black hole, we can see their orbit, but not the black hole. We can infer the mass from the mass of the star and its orbit. 3. The Andromeda galaxy has stars orbiting a dark object that is 30 to 70 million times the mass ...
... event horizon due to the Heisenberg uncertainty principle. 2. When stars orbit a black hole, we can see their orbit, but not the black hole. We can infer the mass from the mass of the star and its orbit. 3. The Andromeda galaxy has stars orbiting a dark object that is 30 to 70 million times the mass ...
test - Scioly.org
... binary system? One of the components is a dwarf-type star, cooler than the Sun, while the other is a white dwarf, the stms are so close that they complete their orbital revolution in slightly over 6 1/2 hours and have a light curve illustrated in figure #2 D) SN 2Ollfe A) HM Cancri E) NGC 1846 B) SS ...
... binary system? One of the components is a dwarf-type star, cooler than the Sun, while the other is a white dwarf, the stms are so close that they complete their orbital revolution in slightly over 6 1/2 hours and have a light curve illustrated in figure #2 D) SN 2Ollfe A) HM Cancri E) NGC 1846 B) SS ...
Type II SuperNova - University of Dayton
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
Stellar Evolution Review
... a) they don’t emit any radiation b) they are surrounded by clouds of gas and dust c) they only emit infrared radiation d) they are all moving away from Earth so fast that their visible light is Doppler shifted into the infrared ...
... a) they don’t emit any radiation b) they are surrounded by clouds of gas and dust c) they only emit infrared radiation d) they are all moving away from Earth so fast that their visible light is Doppler shifted into the infrared ...
Life Cycles of Stars
... Massive Stars (8 times or more larger than the Sun. Core remains massive after the supernova. Fusion is stopped. Nothing supports the core. The core is swallowed by its gravity. It becomes a black hole ...
... Massive Stars (8 times or more larger than the Sun. Core remains massive after the supernova. Fusion is stopped. Nothing supports the core. The core is swallowed by its gravity. It becomes a black hole ...
life cycles of stars
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
... In which order will a single star of one solar mass progress through the various stages of stellar evolution? 1. Planetary nebula, main-sequence star, white dwarf, black hole 2. Proto-star, main-sequence star, planetary nebula, white dwarf 3. Proto-star, red giant, supernova, planetary nebula 4. Pr ...
Lec9_2D
... The gravity at the surface of a red giant star is extremely weak. Any excess motion in the stellar atmosphere can cause the star to lose its mass into space. During this phase, stars can lose a lot of mass. ...
... The gravity at the surface of a red giant star is extremely weak. Any excess motion in the stellar atmosphere can cause the star to lose its mass into space. During this phase, stars can lose a lot of mass. ...
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.