PowerPoint Presentation - Neutron stars, pulsars and black
... • Some of the x-ray binaries have allowed a measurement of the neutron star mass: In 10 of 11 cases, M=1.44Mo This is good! Neutron stars are all supposed to be more massive than the Chandrasekar limit and there is even reason to expect them to be close to this limit as that is what initiated the co ...
... • Some of the x-ray binaries have allowed a measurement of the neutron star mass: In 10 of 11 cases, M=1.44Mo This is good! Neutron stars are all supposed to be more massive than the Chandrasekar limit and there is even reason to expect them to be close to this limit as that is what initiated the co ...
Black Hole
... Black Hole - a theoretical massive object, formed at the beginning of the universe or by the gravitational collapse of a star exploding as a supernova, whose gravitational field is so intense that no electromagnetic radiation can ...
... Black Hole - a theoretical massive object, formed at the beginning of the universe or by the gravitational collapse of a star exploding as a supernova, whose gravitational field is so intense that no electromagnetic radiation can ...
powerpoint file
... Do Black Holes Exist? We are confident that very massive black holes exist at the centers of most galaxies. Black holes of a few solar masses are believed to form when massive stars undergo core collapse if the collapsed core exceeds the maximum of ~ 3 M permitted for neutron stars. The best evide ...
... Do Black Holes Exist? We are confident that very massive black holes exist at the centers of most galaxies. Black holes of a few solar masses are believed to form when massive stars undergo core collapse if the collapsed core exceeds the maximum of ~ 3 M permitted for neutron stars. The best evide ...
Slide 1
... and since ul=c u=c/l so E=hc/l. A photon has its energy change as it moves away from a massive body. That is, it loses some energy as the gravitational field does work on it. This means that l must change. Since E goes down l gets bigger. • We have a RED shift! ...
... and since ul=c u=c/l so E=hc/l. A photon has its energy change as it moves away from a massive body. That is, it loses some energy as the gravitational field does work on it. This means that l must change. Since E goes down l gets bigger. • We have a RED shift! ...
DTU_9e_ch14 - USD Home Pages
... and disappear so quickly that they do not violate any laws of nature. The tidal force just outside of the event horizon of a black hole is strong enough to tear apart two virtual particles that appear there before they destroy each other. The gravitational energy that goes into separating them makes ...
... and disappear so quickly that they do not violate any laws of nature. The tidal force just outside of the event horizon of a black hole is strong enough to tear apart two virtual particles that appear there before they destroy each other. The gravitational energy that goes into separating them makes ...
Dark Matter
... Decide whether each of the following statements makes sense (is clearly true) or does not make sense (is clearly false). Explain your reasoning thoroughly. #5. “The white dwarf at the center of the Helix Nebula has a mass three times the mass of our Sun.” #6. “The pulsation period of a pulsar appear ...
... Decide whether each of the following statements makes sense (is clearly true) or does not make sense (is clearly false). Explain your reasoning thoroughly. #5. “The white dwarf at the center of the Helix Nebula has a mass three times the mass of our Sun.” #6. “The pulsation period of a pulsar appear ...
Goodbye Big Bang, hello black hole? A new theory of the
... Goodbye Big Bang, hello black hole? A new theory of the universe's creation 19 September 2013, by Elizabeth Howell, Universe Today not give enough time—as far as we can tell—to reach a temperature equilibrium. Most cosmologists say the universe must have been expanding faster than the speed of light ...
... Goodbye Big Bang, hello black hole? A new theory of the universe's creation 19 September 2013, by Elizabeth Howell, Universe Today not give enough time—as far as we can tell—to reach a temperature equilibrium. Most cosmologists say the universe must have been expanding faster than the speed of light ...
Answers to Physics 176 One-Minute Questionnaires Lecture date: January 27, 2011
... You can find a good discussion of this in the article “Specific heats and the equipartition law in introductory textbooks” by C. Gearhart, American Journal of Physics, Volume 64, pages 995-1000 (1996). Quantum mechanics predicts that the spacing between energy levels associated with rotation about a ...
... You can find a good discussion of this in the article “Specific heats and the equipartition law in introductory textbooks” by C. Gearhart, American Journal of Physics, Volume 64, pages 995-1000 (1996). Quantum mechanics predicts that the spacing between energy levels associated with rotation about a ...
Local Group Dwarfs
... – Planck length, time = QED – Compton length, time = QED – Schwarzschild length, time = gravity The way these are related defines who is in charge – gravity or QED Funny feature: a Planck mass into the formula for Compton, Schwarzschild lengths = Planck length Also, all times are equal. Meaning? Pla ...
... – Planck length, time = QED – Compton length, time = QED – Schwarzschild length, time = gravity The way these are related defines who is in charge – gravity or QED Funny feature: a Planck mass into the formula for Compton, Schwarzschild lengths = Planck length Also, all times are equal. Meaning? Pla ...
GR100QuantumGravity2015 - Institute for Advanced Study
... system if we stay outside. • Quantum mechanics suggests that there should be an exact description where entropy does not increase. (As viewed from outside). And where Hawking radiation is not mixed. • 2nd law already suggests that information is not lost (if information were lost, why should the 2nd ...
... system if we stay outside. • Quantum mechanics suggests that there should be an exact description where entropy does not increase. (As viewed from outside). And where Hawking radiation is not mixed. • 2nd law already suggests that information is not lost (if information were lost, why should the 2nd ...
Astronomy 15 - Problem Set Number 7
... which is numerically equal to Rs = (2.95 km) × mass in solar masses Thus the sun’s Schwarzschild radius would be about 3 km, while a 10-solar mass object has about a 30 km Schwarzschild radius. If you compress an object of mass M to a radius smaller than this, it will be a black hole; nothing can es ...
... which is numerically equal to Rs = (2.95 km) × mass in solar masses Thus the sun’s Schwarzschild radius would be about 3 km, while a 10-solar mass object has about a 30 km Schwarzschild radius. If you compress an object of mass M to a radius smaller than this, it will be a black hole; nothing can es ...
Jets from Black Holes in Quasars
... How big is a BLACK HOLE? - Depends on its mass Human-mass black hole: much smaller than the nucleus of an atom Black hole with sun’s mass: 6 km (about the size of downtown) 1 billion times sun’s mass: about the size of the solar system ...
... How big is a BLACK HOLE? - Depends on its mass Human-mass black hole: much smaller than the nucleus of an atom Black hole with sun’s mass: 6 km (about the size of downtown) 1 billion times sun’s mass: about the size of the solar system ...
Brown-Henneaux`s Canonical Approach to Topologically Massive
... The simulation data is nicely fitted by the above function up to Therefore we conclude the gauge/gravity correspondence is correct even if we take account of the finite contributions. It is interesting to study the region of quite low temperature numerically to understand the final state of the blac ...
... The simulation data is nicely fitted by the above function up to Therefore we conclude the gauge/gravity correspondence is correct even if we take account of the finite contributions. It is interesting to study the region of quite low temperature numerically to understand the final state of the blac ...
Death of massive stars
... nearby object to escape its gravitational pull. • It can be identified by either how much space it takes up or by the mass. ...
... nearby object to escape its gravitational pull. • It can be identified by either how much space it takes up or by the mass. ...
BLACK HOLES - Science Center of Iowa
... of space-time. We now know that these wormholes are too unstable to exist, but even if they did, wormholes could not support human “time travel” as science fiction writers would imagine it. The enormous gravity associated with black holes and wormholes would rip apart any matter that came near it. S ...
... of space-time. We now know that these wormholes are too unstable to exist, but even if they did, wormholes could not support human “time travel” as science fiction writers would imagine it. The enormous gravity associated with black holes and wormholes would rip apart any matter that came near it. S ...
here - Event Horizon Telescope
... hole makes in the fabric of spacetime. As a photon loses energy, its wavelength becomes longer, until it’s stretched to infinity and right out of existence. The second and prevailing reason for the silhouette effect is what happens to radiation emitted by material on the event horizon’s far side. Th ...
... hole makes in the fabric of spacetime. As a photon loses energy, its wavelength becomes longer, until it’s stretched to infinity and right out of existence. The second and prevailing reason for the silhouette effect is what happens to radiation emitted by material on the event horizon’s far side. Th ...
Astronomy 120
... What is the source of the electromagnetic radiation in the pulses of pulsars? 7. Zeilik Study Exercise 16.6 Make a list of the observational evidence that supports the idea of the Crab Nebula as a supernova remnant. 8. Zeilik Study Exercise 16.8 If a black hole is really black, how can it be an x-ra ...
... What is the source of the electromagnetic radiation in the pulses of pulsars? 7. Zeilik Study Exercise 16.6 Make a list of the observational evidence that supports the idea of the Crab Nebula as a supernova remnant. 8. Zeilik Study Exercise 16.8 If a black hole is really black, how can it be an x-ra ...
White dwarfs - University of Toronto
... degeneracy pressure, the material collapses further. There is not other thing known in physics at the present time to prevent it from forming a black hole. Black holes are characterized by a distance from the center called an event horizon, at which the gravitational pull is just strong enough that ...
... degeneracy pressure, the material collapses further. There is not other thing known in physics at the present time to prevent it from forming a black hole. Black holes are characterized by a distance from the center called an event horizon, at which the gravitational pull is just strong enough that ...
Review: How does a star`s mass determine its life story?
... – Its light would be increasingly redshifted as it approached the black hole. – The object would never quite reach the event horizon, but it would soon disappear from view as its light became so redshifted that no instrument could detect it. ...
... – Its light would be increasingly redshifted as it approached the black hole. – The object would never quite reach the event horizon, but it would soon disappear from view as its light became so redshifted that no instrument could detect it. ...
Slide 1 - Arif Solmaz
... After a Type I supernova, little or nothing remains of the original star. After a Type II supernova, part of the core may survive. It is very dense—as dense as an atomic nucleus—and is called a neutron ...
... After a Type I supernova, little or nothing remains of the original star. After a Type II supernova, part of the core may survive. It is very dense—as dense as an atomic nucleus—and is called a neutron ...
Bez tytułu slajdu
... Z=1057. With such a big compression, neutrons start to "crowd-up", following the Pauli's rule, which does not allow them to be in the same quantum state. It is energetically useful to replace some neutrons with protons, or even by isolated quarks. It seems (A.R. Bodmer 1971 , E. Witten 1984) that th ...
... Z=1057. With such a big compression, neutrons start to "crowd-up", following the Pauli's rule, which does not allow them to be in the same quantum state. It is energetically useful to replace some neutrons with protons, or even by isolated quarks. It seems (A.R. Bodmer 1971 , E. Witten 1984) that th ...
Hawking radiation
Hawking radiation is black body radiation that is predicted to be released by black holes, due to quantum effects near the event horizon. It is named after the physicist Stephen Hawking, who provided a theoretical argument for its existence in 1974, and sometimes also after Jacob Bekenstein, who predicted that black holes should have a finite, non-zero temperature and entropy.Hawking's work followed his visit to Moscow in 1973 where the Soviet scientists Yakov Zeldovich and Alexei Starobinsky showed him that, according to the quantum mechanical uncertainty principle, rotating black holes should create and emit particles. Hawking radiation reduces the mass and energy of black holes and is therefore also known as black hole evaporation. Because of this, black holes that lose more mass than they gain through other means are expected to shrink and ultimately vanish. Micro black holes are predicted to be larger net emitters of radiation than larger black holes and should shrink and dissipate faster.In September 2010, a signal that is closely related to black hole Hawking radiation (see analog gravity) was claimed to have been observed in a laboratory experiment involving optical light pulses. However, the results remain unverified and debatable. Other projects have been launched to look for this radiation within the framework of analog gravity. In June 2008, NASA launched the Fermi space telescope, which is searching for the terminal gamma-ray flashes expected from evaporating primordial black holes. In the event that speculative large extra dimension theories are correct, CERN's Large Hadron Collider may be able to create micro black holes and observe their evaporation.