Bohr Model Notes - Northwest ISD Moodle
... Electrons are placed in energy levels (orbitals) outside the nucleus. 2 electrons can fit in the first energy level. 8 electrons can fit in the second energy level. 18 electrons can fit in the third energy level. Valence Electrons – electrons found in the outermost energy levels. Magnesium has ...
... Electrons are placed in energy levels (orbitals) outside the nucleus. 2 electrons can fit in the first energy level. 8 electrons can fit in the second energy level. 18 electrons can fit in the third energy level. Valence Electrons – electrons found in the outermost energy levels. Magnesium has ...
Stellar Structure — Polytrope models for White Dwarf density profiles
... Equation (4) for the pressure applies at densities that are not too high. At even higher densities, the electrons are so confined that they become relativistic. The expression for a highly degenerate relativistic quantum gas with a density ne is also polytropic. It is p= ...
... Equation (4) for the pressure applies at densities that are not too high. At even higher densities, the electrons are so confined that they become relativistic. The expression for a highly degenerate relativistic quantum gas with a density ne is also polytropic. It is p= ...
14.1 Introduction - University of Cambridge
... We do not have to look very far to find a white dwarf. Sirius (α CMa) is the brightest star in the sky, and the fifth closest to the Sun, at a distance of only 2.6 pc. In 1862 the telescope maker Alvan Clark, while testing an 18-inch refractor lens, discovered that Sirius has a very faint companion: ...
... We do not have to look very far to find a white dwarf. Sirius (α CMa) is the brightest star in the sky, and the fifth closest to the Sun, at a distance of only 2.6 pc. In 1862 the telescope maker Alvan Clark, while testing an 18-inch refractor lens, discovered that Sirius has a very faint companion: ...
Introduction to Astronomy
... – A fundamental limit to the number of electrons that can be squeezed into a given volume – When this limit is reached, there appears a “pressure” that keeps any more electrons from entering the volume – This “electron pressure” supports the white dwarf against its own gravity ...
... – A fundamental limit to the number of electrons that can be squeezed into a given volume – When this limit is reached, there appears a “pressure” that keeps any more electrons from entering the volume – This “electron pressure” supports the white dwarf against its own gravity ...
states of matter
... But what happens if you raise the temperature to super-high levels… between 1000°C and 1,000,000,000°C ? ...
... But what happens if you raise the temperature to super-high levels… between 1000°C and 1,000,000,000°C ? ...
states of matter - www .alexandria .k12 .mn .us
... ionized gas. A plasma is a very good conductor of electricity and is affected by magnetic fields. Plasmas, like gases • Plasma is the have an indefinite common state shape and an of matter indefinite volume. ...
... ionized gas. A plasma is a very good conductor of electricity and is affected by magnetic fields. Plasmas, like gases • Plasma is the have an indefinite common state shape and an of matter indefinite volume. ...
Stellar Structure - Astronomy Centre
... • Now have 3 equations, 5 variables (P, ρ, M, T, μ) – but can obtain some general results without more equations. • Boundary conditions: take P = ρ = 0 at the surface. • Can then find lower limit for the central pressure (Theorem I): ...
... • Now have 3 equations, 5 variables (P, ρ, M, T, μ) – but can obtain some general results without more equations. • Boundary conditions: take P = ρ = 0 at the surface. • Can then find lower limit for the central pressure (Theorem I): ...
chemI.final.rev.probs
... 6. What is the mass of an object that has a density of 0.83 g/mL and displaces 23 mL of water? ...
... 6. What is the mass of an object that has a density of 0.83 g/mL and displaces 23 mL of water? ...
Deaths of Stars - Chabot College
... charged particles moving close to the speed of light around magnetic fields. Slow down over time Fastest signal oscillation in ...
... charged particles moving close to the speed of light around magnetic fields. Slow down over time Fastest signal oscillation in ...
Today in Astronomy 142
... ! Quantum mechanics: degeneracy pressure sets in under extreme states of compression and/or low temperatures. This is the means of support for objects with no fusion: dead stars (white dwarfs, neutron stars), stillborn stars (brown dwarfs), and the cores of giant planets (Jupiter, Saturn). Astronomy ...
... ! Quantum mechanics: degeneracy pressure sets in under extreme states of compression and/or low temperatures. This is the means of support for objects with no fusion: dead stars (white dwarfs, neutron stars), stillborn stars (brown dwarfs), and the cores of giant planets (Jupiter, Saturn). Astronomy ...
White Dwarfs & Other Ends March 21 − Stars with < 2 M
... White dwarf • Degenerate gas • Pressure is not greater at hotter temperature • Baseballs move because they are close together • Quantum mechanics: uncertainty relation • Speed × confinement = Planck’s constant • Pressure is greater if gas is confined to smaller region • In a smaller star, baseballs ...
... White dwarf • Degenerate gas • Pressure is not greater at hotter temperature • Baseballs move because they are close together • Quantum mechanics: uncertainty relation • Speed × confinement = Planck’s constant • Pressure is greater if gas is confined to smaller region • In a smaller star, baseballs ...
PREVIEW-Reading Quiz 06 - Chapter 12
... These stars become more luminous because the degenerate helium or carbon cores continue to grow due to particle pressure. Stars follow the Stefan-Boltzmann law: The higher luminosities generated by the shell fusion makes the star expand enormously, and the increase in radius offsets the decrease in ...
... These stars become more luminous because the degenerate helium or carbon cores continue to grow due to particle pressure. Stars follow the Stefan-Boltzmann law: The higher luminosities generated by the shell fusion makes the star expand enormously, and the increase in radius offsets the decrease in ...
Scales of the Universe
... Mass and Luminosity: L ~ M3.5 • The more massive the star the larger its weight • The larger the weight, the larger the pressure • The larger the pressure, the higher the temperature • The higher the temperature, the more energetic the nuclear reaction • The more energetic the nuclear reactions, the ...
... Mass and Luminosity: L ~ M3.5 • The more massive the star the larger its weight • The larger the weight, the larger the pressure • The larger the pressure, the higher the temperature • The higher the temperature, the more energetic the nuclear reaction • The more energetic the nuclear reactions, the ...
Atomic Structure Mini Lab
... To understand how the number of protons, neutrons and electrons determine the properties of atoms Procedure: Obtain a baggie from your instructor Baggies contain the following: White bead represents a proton Purple bead represents a neutron Blue bead represents an electron Count the number of proton ...
... To understand how the number of protons, neutrons and electrons determine the properties of atoms Procedure: Obtain a baggie from your instructor Baggies contain the following: White bead represents a proton Purple bead represents a neutron Blue bead represents an electron Count the number of proton ...
Astronomy 112: Physics of Stars Problem set 2: Due April 29 1. Time
... Assume the mean free path of photons in the sun is 0.1 cm. What is the average change in temperature across this distance? The anisotropy of radiation in the stellar interior is very small. This is why radiation in the solar interior is close to that of a black body. (b) How much energy leaves each ...
... Assume the mean free path of photons in the sun is 0.1 cm. What is the average change in temperature across this distance? The anisotropy of radiation in the stellar interior is very small. This is why radiation in the solar interior is close to that of a black body. (b) How much energy leaves each ...
Comet Pan-Starrs 12 March 2013
... • Higher Tc larger velocities • Larger velocities overcome larger electric repulsion (~atomic number2) • Further nuclear reactions can occur ...
... • Higher Tc larger velocities • Larger velocities overcome larger electric repulsion (~atomic number2) • Further nuclear reactions can occur ...
Contents of the Universe
... and T. • Main sequence stars are found in a band from the upper left to the lower right. • Giant and supergiant stars are found in the upper right corner. • Tiny white dwarf stars are found in the lower left corner of the HR diagram. ...
... and T. • Main sequence stars are found in a band from the upper left to the lower right. • Giant and supergiant stars are found in the upper right corner. • Tiny white dwarf stars are found in the lower left corner of the HR diagram. ...
PS #1 Solutions - Stars and Stellar Explosions 1. Opacity sources
... gas law is a reasonable assumption. Note that you do not need any quantum mechanics for this problem. It’s purely classical. a) Provide a quantitative relation between the temperature and density of a star which indicates when we can treat it as a gas (rather than a liquid) throughout its interior, ...
... gas law is a reasonable assumption. Note that you do not need any quantum mechanics for this problem. It’s purely classical. a) Provide a quantitative relation between the temperature and density of a star which indicates when we can treat it as a gas (rather than a liquid) throughout its interior, ...
Stellar balancing act — dynamic equilibrium. A star spends most of
... Quantum pressure — Electrons cannot occupy the same region of space if they have the same energy. As matter is squeezed down, electrons develop more “uncertainty” energy depending only on the density and independent of the temperature. The electrons’ resistance to being squeezed any closer together ...
... Quantum pressure — Electrons cannot occupy the same region of space if they have the same energy. As matter is squeezed down, electrons develop more “uncertainty” energy depending only on the density and independent of the temperature. The electrons’ resistance to being squeezed any closer together ...
Science Centre Talk
... Cooling by photodisintegration γ+56Fe↔134He+4n and electron capture p++e-→n+νe ...
... Cooling by photodisintegration γ+56Fe↔134He+4n and electron capture p++e-→n+νe ...
Elements and Atoms
... Atomic Number: Number of protons and it is also the number of electrons in an atom of an element. Element’s Symbol: An abbreviation for the element. Elements Name ...
... Atomic Number: Number of protons and it is also the number of electrons in an atom of an element. Element’s Symbol: An abbreviation for the element. Elements Name ...
STATES OF MATTER
... STATES OF MATTER LIQUID Particles of liquids are tightly packed, but are far enough apart to slide over one another. Liquids have an indefinite shape and a definite volume. ...
... STATES OF MATTER LIQUID Particles of liquids are tightly packed, but are far enough apart to slide over one another. Liquids have an indefinite shape and a definite volume. ...