Fall Semester Final Study Guide 2014 Chapter 1 Introduction to
... 36. What is Charle’s law? 37. True or False Solids can be compressed. 38. What do solids, liquids, and gases have in common? 39. What happens to gas particles when the pressure of a gas increases? 40. A measure of the average kinetic energy of the particles in an object is called____________. 41. Wh ...
... 36. What is Charle’s law? 37. True or False Solids can be compressed. 38. What do solids, liquids, and gases have in common? 39. What happens to gas particles when the pressure of a gas increases? 40. A measure of the average kinetic energy of the particles in an object is called____________. 41. Wh ...
Angular momentum evolution
... • Several thousands of rotational periods now available for solar-type and low-mass stars from ~1 Myr to a ~10 Gyr (0.2-1.2 Msun) • Kepler still expected to yield many more rotational periods for field stars • Several tens of vsini measurements available for VLM stars and brown dwarfs ...
... • Several thousands of rotational periods now available for solar-type and low-mass stars from ~1 Myr to a ~10 Gyr (0.2-1.2 Msun) • Kepler still expected to yield many more rotational periods for field stars • Several tens of vsini measurements available for VLM stars and brown dwarfs ...
Electromagnetic pulse from final gravitational stellar collapse
... In such cases, the MEMP is the only electromagnetic signal associated with the gravitational collapse. One of the unexpected secondary results is the finding that, in general, there exist two classes of neutron stars: the first class is made up of solitary neutron stars which do not have the opportu ...
... In such cases, the MEMP is the only electromagnetic signal associated with the gravitational collapse. One of the unexpected secondary results is the finding that, in general, there exist two classes of neutron stars: the first class is made up of solitary neutron stars which do not have the opportu ...
Lecture 9
... They all have large cross-sections and fast reaction rates ⇒ deuterium efficiently converts to 4 He. ...
... They all have large cross-sections and fast reaction rates ⇒ deuterium efficiently converts to 4 He. ...
their evolution, nucleosynthesis and dusty end
... FRUITY and MONASH models vs Grains (measurements from Avila et al. 2012) ...
... FRUITY and MONASH models vs Grains (measurements from Avila et al. 2012) ...
Diapositiva 1
... Description of nuclear properties with an ‘universal’ density-dependent force (Gogny) and state-of-the-art beyond-mean-field calculations. Combination of configuration mixing (GCM) techniques with symmetry restored wave functions (particle number and angular momentum projections) Some recent a ...
... Description of nuclear properties with an ‘universal’ density-dependent force (Gogny) and state-of-the-art beyond-mean-field calculations. Combination of configuration mixing (GCM) techniques with symmetry restored wave functions (particle number and angular momentum projections) Some recent a ...
Lecture5
... Note: 1 year ~ 3 x 107 sec., c = 3 x 108 m/sec, L☉ = 4 x 1026 J/sec., M☉= 1.9891 x 1030 kg ...
... Note: 1 year ~ 3 x 107 sec., c = 3 x 108 m/sec, L☉ = 4 x 1026 J/sec., M☉= 1.9891 x 1030 kg ...
Slide 1
... Thermal instability: the local density and pressure drops, while the temperature increases. Our solution is based on the detailed treatment of the EOS, coupling the beta-equilibrium and the neutrino trapping effects, as well as including the information of the chemical composition in the process of ...
... Thermal instability: the local density and pressure drops, while the temperature increases. Our solution is based on the detailed treatment of the EOS, coupling the beta-equilibrium and the neutrino trapping effects, as well as including the information of the chemical composition in the process of ...
5.3 Convective transport
... These expressions are rather useless for our purposes so we need to reform them into something more useful. We want to get an expression for what happens to the gas if we add just a small amount of energy dq, and that involves both that we know something about the gas itself and how it changes its p ...
... These expressions are rather useless for our purposes so we need to reform them into something more useful. We want to get an expression for what happens to the gas if we add just a small amount of energy dq, and that involves both that we know something about the gas itself and how it changes its p ...
Stellar Evolution II
... • Fusion in the core continues through many more stages than for low mass stars • Heavier elements are produced: – carbon, – oxygen, – neon, – silicon, – and so on up to iron ...
... • Fusion in the core continues through many more stages than for low mass stars • Heavier elements are produced: – carbon, – oxygen, – neon, – silicon, – and so on up to iron ...
Unit 1 - bilingual project fiñana
... It takes the Earth one year to orbit the Sun. The Earth is not upright, it is tilted. When the North Pole end of the Earth´s axis is tilted towards the Sun, it is summer in the Northern hemisphere. The days are long and the nights are short. At this time the South Pole is tilted away from the Sun, a ...
... It takes the Earth one year to orbit the Sun. The Earth is not upright, it is tilted. When the North Pole end of the Earth´s axis is tilted towards the Sun, it is summer in the Northern hemisphere. The days are long and the nights are short. At this time the South Pole is tilted away from the Sun, a ...
Slide 1
... match the current luminosity and radius of the Sun One input to models is ratio of mass fraction of H ( = X) to mass fraction of heavy elements (= Z) Mass fraction of He ( = Y) follows from X + Y + Z = 1 Z is the sum of the mass fraction of all elements heavier than He (the “metals”) Z is dominated ...
... match the current luminosity and radius of the Sun One input to models is ratio of mass fraction of H ( = X) to mass fraction of heavy elements (= Z) Mass fraction of He ( = Y) follows from X + Y + Z = 1 Z is the sum of the mass fraction of all elements heavier than He (the “metals”) Z is dominated ...
arXiv:astro-ph/0612072v1 4 Dec 2006 Theory of core
... even more energy loss, because the electron capture rate on free protons is significantly larger than on neutron-rich nuclei due to the higher Q-values of the latter. A large fraction of the neutrinos produced by these electron captures behind the shock leave the star quickly in what is called the n ...
... even more energy loss, because the electron capture rate on free protons is significantly larger than on neutron-rich nuclei due to the higher Q-values of the latter. A large fraction of the neutrinos produced by these electron captures behind the shock leave the star quickly in what is called the n ...
NGC 3370 Spiral Galaxy - University of Kentucky
... hour or so during the supernova explosion. • When the shock wave of material collides with the molecular clouds, it sets off star formation AND also seeds the cloud with new elements. • The result is that when new stars form, they have more heavy elements than the previous generation of stars. ...
... hour or so during the supernova explosion. • When the shock wave of material collides with the molecular clouds, it sets off star formation AND also seeds the cloud with new elements. • The result is that when new stars form, they have more heavy elements than the previous generation of stars. ...
Chapter_7
... • We can directly measure the Earth, Moon and some asteroids from the radioactivity of their rocks (about 4.6 billion years old). • The Sun’s age is similar based on it’s current brightness and it’s presumed rate nuclear fuel ...
... • We can directly measure the Earth, Moon and some asteroids from the radioactivity of their rocks (about 4.6 billion years old). • The Sun’s age is similar based on it’s current brightness and it’s presumed rate nuclear fuel ...
The Helium Flash • When the temperature of a stellar core reaches T
... star’s total mass or core mass does not affect the star’s effective temperature, except through determining the envelope mass. • Both helium-core burning and hydrogen shell-burning contribute to the luminosity of a horizontal branch star. In stars with small envelope masses, the luminosity from helium ...
... star’s total mass or core mass does not affect the star’s effective temperature, except through determining the envelope mass. • Both helium-core burning and hydrogen shell-burning contribute to the luminosity of a horizontal branch star. In stars with small envelope masses, the luminosity from helium ...
Kristen Turiano
... an icy body that releases gas or dust. Most travel around the sun in long, oval orbits. consists of a solid nucleus (the core) cloudy atmosphere called the coma one or two tails. most are too small or too faint to be seen without a telescope. Some can be seen for several weeks as they pass close to ...
... an icy body that releases gas or dust. Most travel around the sun in long, oval orbits. consists of a solid nucleus (the core) cloudy atmosphere called the coma one or two tails. most are too small or too faint to be seen without a telescope. Some can be seen for several weeks as they pass close to ...
L8 Condensation
... In order to compute which elements condense where, we assume that changes in temperature and density occur on a relatively long timescale compared to the chemical reaction timescale. This is a reasonable assumption at least for the inner part of the disk where temperatures and gas densities are high ...
... In order to compute which elements condense where, we assume that changes in temperature and density occur on a relatively long timescale compared to the chemical reaction timescale. This is a reasonable assumption at least for the inner part of the disk where temperatures and gas densities are high ...