Compact Objects
... If a stellar core has mass greater than the Chandrasehkar limit (1.4 Msun), electron degeneracy pressure cannot support it ...
... If a stellar core has mass greater than the Chandrasehkar limit (1.4 Msun), electron degeneracy pressure cannot support it ...
Notes on White Dwarfs and Neutron Stars.
... White dwarfs get their name from fact that many of them have high surface temperatures (e.g., 16,000K for 40 Eridani B, the first white dwarf discovered) and thus appear white in color. But their surface temperatures are low compared to the temperatures of the interiors of these stars, which may be ...
... White dwarfs get their name from fact that many of them have high surface temperatures (e.g., 16,000K for 40 Eridani B, the first white dwarf discovered) and thus appear white in color. But their surface temperatures are low compared to the temperatures of the interiors of these stars, which may be ...
Nuclear Interactions in Supernovae .
... • When helium is formed from fusing hydrogen, it is gathered closer to the core, and this layering process continues until there is no more fuel source. • But what happens when there is no more ...
... • When helium is formed from fusing hydrogen, it is gathered closer to the core, and this layering process continues until there is no more fuel source. • But what happens when there is no more ...
Einstein
... can no longer work since electrons cannot go faster than c – the speed of light Chandrasekhar found that this happens when a white dwarf’s mass reaches 1.4 M ...
... can no longer work since electrons cannot go faster than c – the speed of light Chandrasekhar found that this happens when a white dwarf’s mass reaches 1.4 M ...
Section C - Astrophysics
... It occurs because the Pauli exclusion principle allows only one electron per quantum state (or 2 per energy state, as the electron has a choice of two spin states). The number of available states per unit volume is limited for a confined set of particles. The exclusion principle thus prevents the pa ...
... It occurs because the Pauli exclusion principle allows only one electron per quantum state (or 2 per energy state, as the electron has a choice of two spin states). The number of available states per unit volume is limited for a confined set of particles. The exclusion principle thus prevents the pa ...
f - E-Course
... The mean kinetic energy of an electron, even at absolute zero, is two orders of magnitude greater than the mean kinetic energy of an ordinary gas ...
... The mean kinetic energy of an electron, even at absolute zero, is two orders of magnitude greater than the mean kinetic energy of an ordinary gas ...
The Physics of Neutron Stars
... An example of observational evidence for a starquake will be briefly described, and a discussion of the changes to the universe if the neutron and proton were closer in mass will then occur. ...
... An example of observational evidence for a starquake will be briefly described, and a discussion of the changes to the universe if the neutron and proton were closer in mass will then occur. ...
Fundamentals of Physical Chemistry
... substance (mol) n = m/M (m- mass, M – molar mass) n = N/NA ( N – number of particles, NA – Avogadro constant; NA = 6.022x1023 mol-1 for H2O (M= 18 g mol-1) the mass of one mole is 18 g and the mass of one molecule ...
... substance (mol) n = m/M (m- mass, M – molar mass) n = N/NA ( N – number of particles, NA – Avogadro constant; NA = 6.022x1023 mol-1 for H2O (M= 18 g mol-1) the mass of one mole is 18 g and the mass of one molecule ...
Chapter 3 PowerPoint Notes
... matter in which the material has no definite shape and no definite volume (Takes the shape and volume of its container). • Molecules/Atoms are spread apart and can be compressed. ...
... matter in which the material has no definite shape and no definite volume (Takes the shape and volume of its container). • Molecules/Atoms are spread apart and can be compressed. ...
Astronomy 114 Problem Set # 6 Due: 11 Apr 2007 SOLUTIONS 1
... 1 Why is the temperature of a star’s core so important in determining which nuclear reactions can occur there? Fusion reactions occur when the strong force, the force that binds the neutrons and protons, binds two nuclei in two initially separate atoms. The strong force acts at very short distances. ...
... 1 Why is the temperature of a star’s core so important in determining which nuclear reactions can occur there? Fusion reactions occur when the strong force, the force that binds the neutrons and protons, binds two nuclei in two initially separate atoms. The strong force acts at very short distances. ...
Life cycle of Stars Notes
... Stage 5: Neutron Stars • Formed by core collapse of very massive star. • This star is so heavy due to protons and electrons being converted to neutrons in a very small space. • Neutron degeneracy pressure of neutrons supports star against gravity. ...
... Stage 5: Neutron Stars • Formed by core collapse of very massive star. • This star is so heavy due to protons and electrons being converted to neutrons in a very small space. • Neutron degeneracy pressure of neutrons supports star against gravity. ...
Lecture 9: Hydrostatic Equilibrium
... surface of the star. Winds are a common feature of massive stars. Also, at some point, the radiation pressure may make it impossible to form a more luminous star than a certain limit. This is known as the Eddington limit and we’ll talk about it more later. It sets a limit on the luminosity that an o ...
... surface of the star. Winds are a common feature of massive stars. Also, at some point, the radiation pressure may make it impossible to form a more luminous star than a certain limit. This is known as the Eddington limit and we’ll talk about it more later. It sets a limit on the luminosity that an o ...
Physics 161 Homework 8 - Solutions Wednesday
... of electrons, Ne and the volume of the white dwarf, V , as ne = Ne /V . Now, as we’ve seen, the total number of electrons is Ne = (Z/A) M /mp , where mp is the proton mass. So, taking Z/A ≈ 1/2 for a white dwarf, we find ...
... of electrons, Ne and the volume of the white dwarf, V , as ne = Ne /V . Now, as we’ve seen, the total number of electrons is Ne = (Z/A) M /mp , where mp is the proton mass. So, taking Z/A ≈ 1/2 for a white dwarf, we find ...
star model
... • A star, with no hidden energy sources, c.omposed of a perfect gas, contracts and heat up as it radiates energy Stars have a negative “heat capacity” = they heat up when their total energy decreases. ...
... • A star, with no hidden energy sources, c.omposed of a perfect gas, contracts and heat up as it radiates energy Stars have a negative “heat capacity” = they heat up when their total energy decreases. ...
Pre-AP Chemistry Kinetic Theory and Heat Quiz
... coexist. The critical point is the point at which phases of matter __become ill defined__. The critical temperature is the temperature above which what cannot happen? a gas cannot be compressed into a liquid The critical pressure is the pressure it takes to _compress a gas into a liquid at the criti ...
... coexist. The critical point is the point at which phases of matter __become ill defined__. The critical temperature is the temperature above which what cannot happen? a gas cannot be compressed into a liquid The critical pressure is the pressure it takes to _compress a gas into a liquid at the criti ...
Unit 1 Inorganic Flashcards
... This is the lowest possible electronic configuration the electrons in an atom can adopt. When an electron moves down to its ground state, energy is given out. ...
... This is the lowest possible electronic configuration the electrons in an atom can adopt. When an electron moves down to its ground state, energy is given out. ...
Electromagnetic Spectrum Wavelength Wavenumber Frequency
... This is the lowest possible electronic configuration the electrons in an atom can adopt. When an electron moves down to its ground state, energy is given out. ...
... This is the lowest possible electronic configuration the electrons in an atom can adopt. When an electron moves down to its ground state, energy is given out. ...
Lecture 22 - Seattle Central
... The iron core gets crushed so that it’s no longer iron, the electrons and protons combine into neutrons, the volume of the core reduces by a factor of 1018 Outer core falls in at about 25% of the speed of light, the core temp rises to ...
... The iron core gets crushed so that it’s no longer iron, the electrons and protons combine into neutrons, the volume of the core reduces by a factor of 1018 Outer core falls in at about 25% of the speed of light, the core temp rises to ...
STUDY GUIDE FOR CHAPTER 1
... D. As material from the outer layers falls on the core eventually it gets so massive that neutron degeneracy pressure cannot hold it up. E. Then it collapses and becomes a black hole. F. As the rest of the outer layers of the star fall onto the black hole they form an accretion disk. G. It is possib ...
... D. As material from the outer layers falls on the core eventually it gets so massive that neutron degeneracy pressure cannot hold it up. E. Then it collapses and becomes a black hole. F. As the rest of the outer layers of the star fall onto the black hole they form an accretion disk. G. It is possib ...
Atomic Theory (Or a quick Chemistry Review)
... Atomic Theory Q: What does science study? A: The natural world, the physical universe Q: What are the components of the P.U? A: matter, energy, forces ...
... Atomic Theory Q: What does science study? A: The natural world, the physical universe Q: What are the components of the P.U? A: matter, energy, forces ...
Four Homework Assignments
... Assuming that the average temperature and central temperature (Tc ) are always proportional (not always a good assumption, but ...), that a star’s radius on the main sequence is proportional to M 0.8 , that γ = 5/3, and that n = 3.0, derive the central temperature of a main sequence star as a functi ...
... Assuming that the average temperature and central temperature (Tc ) are always proportional (not always a good assumption, but ...), that a star’s radius on the main sequence is proportional to M 0.8 , that γ = 5/3, and that n = 3.0, derive the central temperature of a main sequence star as a functi ...
Review Sheet Filled Out
... Electrons closest to the nucleus have the least amount of energy Electrons farthest away from the nucleus have the most energy – valence e Have a negative charge Have insignificant mass and volume Reside in the 99.996% of the atom outside the nucleus Can’t tell where an electron is at any ...
... Electrons closest to the nucleus have the least amount of energy Electrons farthest away from the nucleus have the most energy – valence e Have a negative charge Have insignificant mass and volume Reside in the 99.996% of the atom outside the nucleus Can’t tell where an electron is at any ...