19Nov_2014
... light cannot escape a black hole, how can we see one?” • If a black hole is in orbit around a companion star, the black hole can pull material away from it. ...
... light cannot escape a black hole, how can we see one?” • If a black hole is in orbit around a companion star, the black hole can pull material away from it. ...
Today`s Powerpoint
... a) cannot explain how the Sun is stable. b) detect only one-third the number of neutrinos expected by theory. c) cannot detect neutrinos easily. d) are unable to explain how neutrinos oscillate between other types. e) cannot create controlled fusion reactions on Earth. ...
... a) cannot explain how the Sun is stable. b) detect only one-third the number of neutrinos expected by theory. c) cannot detect neutrinos easily. d) are unable to explain how neutrinos oscillate between other types. e) cannot create controlled fusion reactions on Earth. ...
Stars
... Apparent magnitude: brightness as seen from Earth Absolute magnitude: brightness if it were a standard distance from Earth ...
... Apparent magnitude: brightness as seen from Earth Absolute magnitude: brightness if it were a standard distance from Earth ...
A Red Giant - Cloudfront.net
... Stars with masses similar to our Sun fuse at a rate that allows them to “live” as mainsequence stars for about 10 billion years. Then they run out of Hydrogen in their core Hydrostatic Equilibrium is lost… They Shrink a bit And begin to fuse Hydrogen into Helium in a shell outside the core. ...
... Stars with masses similar to our Sun fuse at a rate that allows them to “live” as mainsequence stars for about 10 billion years. Then they run out of Hydrogen in their core Hydrostatic Equilibrium is lost… They Shrink a bit And begin to fuse Hydrogen into Helium in a shell outside the core. ...
Ch.10 Stellar old age
... A white dwarf cannot be more massive than 1.4MSun (Chandrasekhar limit) Nobel Prize 1983 ...
... A white dwarf cannot be more massive than 1.4MSun (Chandrasekhar limit) Nobel Prize 1983 ...
Lesson 4: Stellar Explosions and Neutron Stars
... • The triple-alpha reaction and the major carbon and oxygen burning reactions are helium capture reactions. The capture of helium nuclei continues until silicon is created, at which point the supply of helium nuclei in the star’s core is depleted: • 20Ne + 4He → 24Mg + γ • 24Mg + 4He → 28Si + γ • Fo ...
... • The triple-alpha reaction and the major carbon and oxygen burning reactions are helium capture reactions. The capture of helium nuclei continues until silicon is created, at which point the supply of helium nuclei in the star’s core is depleted: • 20Ne + 4He → 24Mg + γ • 24Mg + 4He → 28Si + γ • Fo ...
Notes: Nuclear Chemistry
... disintegration. This is natural radioactive decay. a. Artificial bombardment of the nucleus with an energetic particle that changes the composition of the nucleus. This is artificial transmutation. a. Discovered by scientists Becquerel and his students, Marie & Pierre Curie in 1896. a. They won the ...
... disintegration. This is natural radioactive decay. a. Artificial bombardment of the nucleus with an energetic particle that changes the composition of the nucleus. This is artificial transmutation. a. Discovered by scientists Becquerel and his students, Marie & Pierre Curie in 1896. a. They won the ...
Supernova worksheet with solutions ()
... certain mass, it begins to collapse in on itself. As it collapses, it heats up. The collapse continues until the center of the cloud is hot enough to fuse hydrogen into helium. Energy Source: Gravitational energy ...
... certain mass, it begins to collapse in on itself. As it collapses, it heats up. The collapse continues until the center of the cloud is hot enough to fuse hydrogen into helium. Energy Source: Gravitational energy ...
Stellar evolution, II
... tightly bound nucleus. Nuclear reactions to form heavier atoms would use up more energy than they would produce. The outer layers squeeze down onto the iron core and the star explodes as a Type II supernova. ...
... tightly bound nucleus. Nuclear reactions to form heavier atoms would use up more energy than they would produce. The outer layers squeeze down onto the iron core and the star explodes as a Type II supernova. ...
Life and fate of a star
... is expected around 2027 these reactions slowly drain the available hydrogen reservoir. In ● At the end of the red giant phase of the Sun, nuclear fusion reactions another five billion years, the should produce carbon and oxygen atoms from the helium of the core. core of our Sun will run out of Heavi ...
... is expected around 2027 these reactions slowly drain the available hydrogen reservoir. In ● At the end of the red giant phase of the Sun, nuclear fusion reactions another five billion years, the should produce carbon and oxygen atoms from the helium of the core. core of our Sun will run out of Heavi ...
nuclear reactions
... A chain reaction is a sequence of reactions where a reactive product or by-product causes additional reactions to take place, leading to a self-amplifying chain of events. • When an atom (such as Uranium235) undergoes nuclear fission, a few neutrons are ejected from the reaction. These free neutrons ...
... A chain reaction is a sequence of reactions where a reactive product or by-product causes additional reactions to take place, leading to a self-amplifying chain of events. • When an atom (such as Uranium235) undergoes nuclear fission, a few neutrons are ejected from the reaction. These free neutrons ...
File
... and protons. Nuclear binding energy can be calculated from the difference of mass of a nucleus, and the sum of the masses of the number of free neutrons and protons that make up the nucleus. This mass difference is called the mass defect or mass deficiency, next, Einstein's formula: E = mc2 can be u ...
... and protons. Nuclear binding energy can be calculated from the difference of mass of a nucleus, and the sum of the masses of the number of free neutrons and protons that make up the nucleus. This mass difference is called the mass defect or mass deficiency, next, Einstein's formula: E = mc2 can be u ...
April11
... • Red Giant stars can fill their Roche lobes • In a binary star system, the Roche lobes of the two stars can touch, and mass can pass between them. ...
... • Red Giant stars can fill their Roche lobes • In a binary star system, the Roche lobes of the two stars can touch, and mass can pass between them. ...
Consequences of Neutrino Emission from a Phase
... In our study we did not consider the detail formation process from normal matter to quark matter. We simply assume that a neutron star suddenly undergoes a phase-transition. We use a 3D Newtonian hydrodynamic code to study the consequences of phase-transitioninduced collapse. This code solves a set ...
... In our study we did not consider the detail formation process from normal matter to quark matter. We simply assume that a neutron star suddenly undergoes a phase-transition. We use a 3D Newtonian hydrodynamic code to study the consequences of phase-transitioninduced collapse. This code solves a set ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... We know this since one solar mass stars should last on the main sequence (see §III.C.) for 10 billion years and the Sun is currently 5 billion years old. As such, we have 5 billion more years before the Sun becomes a red giant, at which such time, it will “swallow” the most of the inner planets of t ...
... We know this since one solar mass stars should last on the main sequence (see §III.C.) for 10 billion years and the Sun is currently 5 billion years old. As such, we have 5 billion more years before the Sun becomes a red giant, at which such time, it will “swallow” the most of the inner planets of t ...
Time From the Perspective of a Particle Physicist
... Supernova and Neutron Stars For heavy white dwarves with a companion star • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) ...
... Supernova and Neutron Stars For heavy white dwarves with a companion star • acquire mass, if becomes > 1.4 M(Sun) SUPERNOVA (Ia). p + e n + neutrino • Usually leaves neutron star For high mass stars • fusion continues beyond C,O to Iron • if Mass(core) > 1.4 M(Sun) core collapses in SUPERNOVA (II) ...
1. Compute the deflection angle of a star whose light... limb of the Sun. Also compute the deflection angle of...
... 1. Compute the deflection angle of a star whose light just grazes the limb of the Sun. Also compute the deflection angle of a star whose light just grazes the limb of a 1.4M neutron star, if the neutron star was at the same distance from the Earth as the Sun. State assumptions. 2. Use the Plummer p ...
... 1. Compute the deflection angle of a star whose light just grazes the limb of the Sun. Also compute the deflection angle of a star whose light just grazes the limb of a 1.4M neutron star, if the neutron star was at the same distance from the Earth as the Sun. State assumptions. 2. Use the Plummer p ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.