Huge Quantum Gravity Effects in the Solar System
... exponentially amplify quantum uncertainties [10, 11, 12, 13] to become huge uncertainties in the positions of the planets. Because these effects involve both quantum uncertainties and the uncertain gravitational fields produced by the Sun and planets at their uncertain positions, they are truly larg ...
... exponentially amplify quantum uncertainties [10, 11, 12, 13] to become huge uncertainties in the positions of the planets. Because these effects involve both quantum uncertainties and the uncertain gravitational fields produced by the Sun and planets at their uncertain positions, they are truly larg ...
Ch_1_v2
... 15. Explain in terms of the scientific method why the discovery of Neptune was so important in confirming the law of gravity. 16. Change the units in which a quantity is expressed from those of one system of units to those of another system. 17. Use metric prefixes for small and large numbers. 18. U ...
... 15. Explain in terms of the scientific method why the discovery of Neptune was so important in confirming the law of gravity. 16. Change the units in which a quantity is expressed from those of one system of units to those of another system. 17. Use metric prefixes for small and large numbers. 18. U ...
Life on Our Evolving Planet slides
... The National Academy of Sciences says that it is the role of science to provide plausible natural explanations of natural phenomena. The ultimate question for Earth System History is: How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting ...
... The National Academy of Sciences says that it is the role of science to provide plausible natural explanations of natural phenomena. The ultimate question for Earth System History is: How did a giant cloud of cold dilute gas and dust evolve into astronauts in a spacecraft orbiting a planet orbiting ...
1_Introduction
... t=0: The Big Bang Why do we care that this happened? If the universe had remained dense, it wouldn’t have cooled enough for nuclei, atoms, galaxies, and us to form. (Speaking to an audience of humans, I make no apologies ...
... t=0: The Big Bang Why do we care that this happened? If the universe had remained dense, it wouldn’t have cooled enough for nuclei, atoms, galaxies, and us to form. (Speaking to an audience of humans, I make no apologies ...
here
... • The Solar System refers to the Sun and the surrounding planets, asteroids, comets, etc. • The scale of things: – It takes light about 11 hours to travel across the Solar system. This is 0.001265 years. – It takes light about 4.3 years to travel from the Sun to the nearest star. – It takes light ab ...
... • The Solar System refers to the Sun and the surrounding planets, asteroids, comets, etc. • The scale of things: – It takes light about 11 hours to travel across the Solar system. This is 0.001265 years. – It takes light about 4.3 years to travel from the Sun to the nearest star. – It takes light ab ...
6 Big Bang Nucleosynthesis - Course Pages of Physics Department
... reactions involving three or more incoming nuclei to occur at any appreciable rate. The heavier nuclei have to be built sequentially from lighter nuclei in two-particle reactions, so that deuterium is formed first in the reaction n + p → d + γ. Only when deuterons are available can helium nuclei be ...
... reactions involving three or more incoming nuclei to occur at any appreciable rate. The heavier nuclei have to be built sequentially from lighter nuclei in two-particle reactions, so that deuterium is formed first in the reaction n + p → d + γ. Only when deuterons are available can helium nuclei be ...
here
... • The Solar System refers to the Sun and the surrounding planets, asteroids, comets, etc. • The scale of things: – It takes light about 11 hours to travel across the Solar system. This is 0.001265 years. – It takes light about 4.3 years to travel from the Sun to the nearest star. – It takes light ab ...
... • The Solar System refers to the Sun and the surrounding planets, asteroids, comets, etc. • The scale of things: – It takes light about 11 hours to travel across the Solar system. This is 0.001265 years. – It takes light about 4.3 years to travel from the Sun to the nearest star. – It takes light ab ...
pptx
... Main sequence stars fuse hydrogen to helium in core Red giants (and subgiants) fuse hydrogen to helium in shell outside helium core Stars have nearly constant ...
... Main sequence stars fuse hydrogen to helium in core Red giants (and subgiants) fuse hydrogen to helium in shell outside helium core Stars have nearly constant ...
The Sun and the Stars
... The angular separations and orbital paths are only apparent because in general the orbit is inclined to the plane of the sky, so we see the orbit in projection ...
... The angular separations and orbital paths are only apparent because in general the orbit is inclined to the plane of the sky, so we see the orbit in projection ...
–1– Solutions to PH6820 Midterm 1. Define the following: molecular
... Solution: Red-shifted self-absorption implies infall, blueshifted self-absorption implies outflows. These sources have redshifted self-absorption (i.e. exhibit infall): L1172, L1251a, L1251b, L1152. The following show blue-shifted self-absorption (i.e. exhibit outflow): L43, L146 and L1262. The foll ...
... Solution: Red-shifted self-absorption implies infall, blueshifted self-absorption implies outflows. These sources have redshifted self-absorption (i.e. exhibit infall): L1172, L1251a, L1251b, L1152. The following show blue-shifted self-absorption (i.e. exhibit outflow): L43, L146 and L1262. The foll ...
Star Light, Star Bright
... How many stars can you see on a clear night? About 5,000 stars are visible from Earth without the use of a telescope, but you can only see a fraction of them from any particular viewing point at any particular time. With the help of a powerful telescope, it's possible to see more than 3 billion of t ...
... How many stars can you see on a clear night? About 5,000 stars are visible from Earth without the use of a telescope, but you can only see a fraction of them from any particular viewing point at any particular time. With the help of a powerful telescope, it's possible to see more than 3 billion of t ...
Document
... with the nuclear binding energy B(Z,N) Some features of this equation: • in NSE there is a mix of free nucleons and nuclei • higher density favors (heavier) nuclei • higher temperature favors free nucleons (or lighter nuclei) • nuclei with high binding energy are strongly favored ...
... with the nuclear binding energy B(Z,N) Some features of this equation: • in NSE there is a mix of free nucleons and nuclei • higher density favors (heavier) nuclei • higher temperature favors free nucleons (or lighter nuclei) • nuclei with high binding energy are strongly favored ...
sun.galaxy.notes
... • It is difficult to know for sure because it is impossible to see our galaxy from the outside • You can see the Milky Way stretching across the night sky as a faint band of light • All of the stars you can see in the night sky belong to the Milky Way ...
... • It is difficult to know for sure because it is impossible to see our galaxy from the outside • You can see the Milky Way stretching across the night sky as a faint band of light • All of the stars you can see in the night sky belong to the Milky Way ...
Andrew Sonnenschein: The level of poetry…
... neutrinos, being invisible particles, can carry away the energy without our seeing them, and this balances the equation. This occurred during the thirties, then during the fifties, working with reactors where an infinite number of neutrinos were created due to the continuous nuclear reactions, it wa ...
... neutrinos, being invisible particles, can carry away the energy without our seeing them, and this balances the equation. This occurred during the thirties, then during the fifties, working with reactors where an infinite number of neutrinos were created due to the continuous nuclear reactions, it wa ...
Stellar Temperatures
... Stellar temperatures range from ~3000 K to ~100,000 K (although there are exceptions). To zeroth order, they can be considered blackbodies, with stellar absorption lines on top. There is a great variety of stellar absorption lines; the strength of any individual line is determined by the star’s • T ...
... Stellar temperatures range from ~3000 K to ~100,000 K (although there are exceptions). To zeroth order, they can be considered blackbodies, with stellar absorption lines on top. There is a great variety of stellar absorption lines; the strength of any individual line is determined by the star’s • T ...
Thermonuclear supernovae and cosmology
... instabilities on lowest scales determine integral burning rate → star expansion → local conditions at the flame, governing instabilities, and burning rate. Gibson scale~ 104 cm, numerical resolution 5x104 cm. Early simulations of 70s-early 90s: 1D spherical, DDT by hand. Current mainstream 3D simu ...
... instabilities on lowest scales determine integral burning rate → star expansion → local conditions at the flame, governing instabilities, and burning rate. Gibson scale~ 104 cm, numerical resolution 5x104 cm. Early simulations of 70s-early 90s: 1D spherical, DDT by hand. Current mainstream 3D simu ...
Luminosity of sun
... Lower mass: lower core pressure, lower core temperature. Can counter-act the pressure from gravity with a lower ...
... Lower mass: lower core pressure, lower core temperature. Can counter-act the pressure from gravity with a lower ...
PHYS3380_110215_bw - The University of Texas at Dallas
... product. The core convection zone of these stars is overlaid by a radiation zone that is in thermal equilibrium and undergoes little or no mixing. •In stars of less than about 10 solar masses, the outer envelope of the star contains a region where partial ionization of hydrogen and helium raises the ...
... product. The core convection zone of these stars is overlaid by a radiation zone that is in thermal equilibrium and undergoes little or no mixing. •In stars of less than about 10 solar masses, the outer envelope of the star contains a region where partial ionization of hydrogen and helium raises the ...
Search for Planetary Candidates within the OGLE Stars
... Planet definition Based on the object’s mass According to the IAU WORKING GROUP ON EXTRASOLAR PLANETS (WGESP): stars: objects capable of thermonuclear fusion of hydrogen (>0.075 Msun); Brown dwarf: capable of deuterium burning (0.013
... Planet definition Based on the object’s mass According to the IAU WORKING GROUP ON EXTRASOLAR PLANETS (WGESP): stars: objects capable of thermonuclear fusion of hydrogen (>0.075 Msun); Brown dwarf: capable of deuterium burning (0.013
