Lecture 24 Early Universe
... An important property of quarks is called confinement, which states that individual quarks are not seen because they are always confined inside subatomic particles called hadrons (e.g., protons and neutrons); an exception is the top quark, which decays so quickly that it does not hadronize, and can ...
... An important property of quarks is called confinement, which states that individual quarks are not seen because they are always confined inside subatomic particles called hadrons (e.g., protons and neutrons); an exception is the top quark, which decays so quickly that it does not hadronize, and can ...
Document
... Step 6: Once the red giant is unable to support itself the outer layers will come off forming a planetary nebula and the super heated core of the star will remain which is a white dwarf 6. Explain why stars appear to move in the night sky. (MC) Because Earth moves 7. Understand how scientists can fi ...
... Step 6: Once the red giant is unable to support itself the outer layers will come off forming a planetary nebula and the super heated core of the star will remain which is a white dwarf 6. Explain why stars appear to move in the night sky. (MC) Because Earth moves 7. Understand how scientists can fi ...
Lecture 1
... 1. Equation of state (EOS) determines the pressure of the matter, P. 2. The neutron star matter is so dense that P is almost independent of the temperature T and is determined by the mass density and the composition of the matter; one usually writes P P( ). 3. The mass density is defined as ...
... 1. Equation of state (EOS) determines the pressure of the matter, P. 2. The neutron star matter is so dense that P is almost independent of the temperature T and is determined by the mass density and the composition of the matter; one usually writes P P( ). 3. The mass density is defined as ...
Star Life
... a. Clouds of gas and dust b. Planets with temperatures reaching over 6000 degrees Kelvin c. Red giants d. Large masses of radioactive elements 2) Our solar system’s star, the Sun, is in which stage of its life cycle? a. A white dwarf b. A super giant c. A main sequence star d. The only star in the M ...
... a. Clouds of gas and dust b. Planets with temperatures reaching over 6000 degrees Kelvin c. Red giants d. Large masses of radioactive elements 2) Our solar system’s star, the Sun, is in which stage of its life cycle? a. A white dwarf b. A super giant c. A main sequence star d. The only star in the M ...
Stars 3
... The blue glow in the inner part of the nebula -- light emitted by energetic electrons as they spiral through the Crab’s magnetic field -- is powered by the Crab Pulsar. The picture on the right shows a Hubble Space Telescope image of the inner parts of the Crab. The pulsar itself is visible as the l ...
... The blue glow in the inner part of the nebula -- light emitted by energetic electrons as they spiral through the Crab’s magnetic field -- is powered by the Crab Pulsar. The picture on the right shows a Hubble Space Telescope image of the inner parts of the Crab. The pulsar itself is visible as the l ...
Stars - Montville.net
... 10. When a supergiant runs out of fuel it can suddenly explode. This explosion is called a super nova. ...
... 10. When a supergiant runs out of fuel it can suddenly explode. This explosion is called a super nova. ...
Birth, Lives, and Death of Stars
... Stars similar to our Sun can synthesize He, C, O. Massive stars (M* > 5 solar masses) can synthesize He, C, O, Ne. Mg, Si, S, Ar, Ca, Ti, Cr, Fe. Elements heavier than iron are made in supernova explosions from the combination of the abundant neutrons with heavy nuclei. Synthesized elements are disp ...
... Stars similar to our Sun can synthesize He, C, O. Massive stars (M* > 5 solar masses) can synthesize He, C, O, Ne. Mg, Si, S, Ar, Ca, Ti, Cr, Fe. Elements heavier than iron are made in supernova explosions from the combination of the abundant neutrons with heavy nuclei. Synthesized elements are disp ...
Document
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
AST 301 Introduction to Astronomy - University of Texas Astronomy
... Or in a star, it is mostly the free electrons that cause pressure, since it is too hot for atoms to hold onto their electrons. In a normal gas, the electrons’ motion is caused by heat. But at very high densities, the wave properties of the electrons become important, and the electrons must move fast ...
... Or in a star, it is mostly the free electrons that cause pressure, since it is too hot for atoms to hold onto their electrons. In a normal gas, the electrons’ motion is caused by heat. But at very high densities, the wave properties of the electrons become important, and the electrons must move fast ...
black hole - Purdue Physics
... brighter in a matter of days (Greeks didn’t have telescopes) • Totally different event than a supernova ...
... brighter in a matter of days (Greeks didn’t have telescopes) • Totally different event than a supernova ...
Report Sheet
... 36. What part of a star’s life cycle is the Eight Burst nebula? ____________________________ 37. Where did the carbon and oxygen in your body originally come from? ____________________________________ 38. What does the Law of Angular Momentum do to a White Dwarf? ____________________________________ ...
... 36. What part of a star’s life cycle is the Eight Burst nebula? ____________________________ 37. Where did the carbon and oxygen in your body originally come from? ____________________________________ 38. What does the Law of Angular Momentum do to a White Dwarf? ____________________________________ ...
Investigating Supernova Remnants - Chandra X
... internal pressure and its complete collapse is only prevented by quantum mechanics. Two electrons with the same “spin” are not allowed to occupy the same energy state. Since there are only two ways an electron can spin, only two electrons can occupy any single energy state; this is called the Pauli ...
... internal pressure and its complete collapse is only prevented by quantum mechanics. Two electrons with the same “spin” are not allowed to occupy the same energy state. Since there are only two ways an electron can spin, only two electrons can occupy any single energy state; this is called the Pauli ...
Life Cycle of a Star
... but a dense ball of neutrons. It is possible that this core will remain intact after the supernova, and be called a neutron star. However, if the original star was very massive (say 15 or more times the mass of our Sun), even the neutrons will not be able to survive the core collapse and a black hol ...
... but a dense ball of neutrons. It is possible that this core will remain intact after the supernova, and be called a neutron star. However, if the original star was very massive (say 15 or more times the mass of our Sun), even the neutrons will not be able to survive the core collapse and a black hol ...
Study Guide- Tools of Astronomy
... B. Which units are most and least helpful for distances in the Solar system? Explain your reasoning. 11. A. List AND Explain the steps of stellar evolution. B. List the type of fuel associated with each step. C. List the sequence of evolution for high and low mass stars. 12. List, in order, the step ...
... B. Which units are most and least helpful for distances in the Solar system? Explain your reasoning. 11. A. List AND Explain the steps of stellar evolution. B. List the type of fuel associated with each step. C. List the sequence of evolution for high and low mass stars. 12. List, in order, the step ...
Chapter 15. The Chandrasekhar Limit, Iron-56 and Core
... pressure and therefore do not have to keep their core temperatures high via nuclear reactions to keep from collapsing. Their pressure depends only on their density, which is already high. They do not have any form of nuclear energy generation and they radiate only their thermal energy, cooling off s ...
... pressure and therefore do not have to keep their core temperatures high via nuclear reactions to keep from collapsing. Their pressure depends only on their density, which is already high. They do not have any form of nuclear energy generation and they radiate only their thermal energy, cooling off s ...
The Big Four:
... • Effects on matter/light outside the horizon – gravitational attraction of other bodies – “dark star” with mass 3M Sun • distinguish from normal star, white dwarf, neutron star ...
... • Effects on matter/light outside the horizon – gravitational attraction of other bodies – “dark star” with mass 3M Sun • distinguish from normal star, white dwarf, neutron star ...
Matter and Atoms
... have a mass of 1 amu Neutrons have no charge Neutrons are the glue of the atom Atoms are held together by “the strong force”, weak forces, and electromagnetic ...
... have a mass of 1 amu Neutrons have no charge Neutrons are the glue of the atom Atoms are held together by “the strong force”, weak forces, and electromagnetic ...
Activity 1 - Mathematical and Scientific Methods
... Have 11 scored participation activities. Lowest 4 scores to be dropped. Math review counts as 2. 50 pts 10 quizzes; one with lowest score will be dropped. ...
... Have 11 scored participation activities. Lowest 4 scores to be dropped. Math review counts as 2. 50 pts 10 quizzes; one with lowest score will be dropped. ...
Nuclear Fusion Nuclear Physics Mass Number Structure of Matter
... Formation of elements heavier than Fe require an input of energy and cannot be produced by thermonuclear reactions Produced almost exclusively by neutron capture during final violent stages of stellar evolution (e.g. supernovae) ...
... Formation of elements heavier than Fe require an input of energy and cannot be produced by thermonuclear reactions Produced almost exclusively by neutron capture during final violent stages of stellar evolution (e.g. supernovae) ...
PH507 - University of Kent
... exp (-10.19 x 11,594/T) = 2xN2/ (8xN1) = 0.025 yields T = 32,000K ...
... exp (-10.19 x 11,594/T) = 2xN2/ (8xN1) = 0.025 yields T = 32,000K ...
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.