Helium Production in Big Bang Weighing a Galaxy12 Nov 11/12/2010
... • When T is between 10BK and 3BK, the density drops so that – number of collisions falls & neutrons and protons are no longer in equilibrium. – Protons no longer change into neutrons. Neutrons decay into protons. ...
... • When T is between 10BK and 3BK, the density drops so that – number of collisions falls & neutrons and protons are no longer in equilibrium. – Protons no longer change into neutrons. Neutrons decay into protons. ...
Can the sun make it rain, or (Will astronomy help us
... • Light elements formed in the first 3 minutes • Heavies formed in stars later and now • Dust (grains) formed in cool parts of giant stars • Molecules formed on dust grains • Planets condensed from stellar environment • Biological processes differentiated elements ...
... • Light elements formed in the first 3 minutes • Heavies formed in stars later and now • Dust (grains) formed in cool parts of giant stars • Molecules formed on dust grains • Planets condensed from stellar environment • Biological processes differentiated elements ...
Stellar evolution
... • The implosion produces enough energy to create a supernova. • The supernova can last weeks or months, and release as much energy as the sun does in its entire lifespan. • The supernova is a main source of heavy elements in the universe. • The remaining core will collapse into either a neutron star ...
... • The implosion produces enough energy to create a supernova. • The supernova can last weeks or months, and release as much energy as the sun does in its entire lifespan. • The supernova is a main source of heavy elements in the universe. • The remaining core will collapse into either a neutron star ...
The first step towards getting somewhere is to decide you are not
... The first step towards getting somewhere is to decide you are not going to stay where you are. ...
... The first step towards getting somewhere is to decide you are not going to stay where you are. ...
Spin-spin splitting in NMR spectrum
... transmission of r-ray from a source through an absorber as a function of velocity V between th ...
... transmission of r-ray from a source through an absorber as a function of velocity V between th ...
A Star is Born – Worksheet and Key – Ben Kwok
... Are white dwarfs very hot or very cold? What comes after a white dwarf? What is a supergiant star? Is the lifespan of a supergiant longer or shorter than that of a main sequence? 13. How big can a supergiant get? 14. What are 2 characteristics of a neutron star? 15. How many black holes have been fo ...
... Are white dwarfs very hot or very cold? What comes after a white dwarf? What is a supergiant star? Is the lifespan of a supergiant longer or shorter than that of a main sequence? 13. How big can a supergiant get? 14. What are 2 characteristics of a neutron star? 15. How many black holes have been fo ...
Stellar Remnants
... Density much greater than Earth •Earth = 5.5 grams/cc •WD = tons/cc •composition depends on mass of progenitor •helium •carbon •carbon-oxygen •oxygen-neon-magnesium ...
... Density much greater than Earth •Earth = 5.5 grams/cc •WD = tons/cc •composition depends on mass of progenitor •helium •carbon •carbon-oxygen •oxygen-neon-magnesium ...
The Life Cycle of a Star
... the Carbon into Iron, there is no more fuel left to consume. The Core of the supergiant will then collapse in less than a second, causing a massive explosion called a supernova. In a supernova, a massive shockwave is produced that blows away the outer layers of the star. Supernova shine brighter the ...
... the Carbon into Iron, there is no more fuel left to consume. The Core of the supergiant will then collapse in less than a second, causing a massive explosion called a supernova. In a supernova, a massive shockwave is produced that blows away the outer layers of the star. Supernova shine brighter the ...
Jeopardy - Two Rivers High School
... The sun is a medium star so fusion will eventually stop and it will begin to expand as a red giant. The outside planetary nebula will drift away and what remains is a white dwarf that will ultimately die out. ...
... The sun is a medium star so fusion will eventually stop and it will begin to expand as a red giant. The outside planetary nebula will drift away and what remains is a white dwarf that will ultimately die out. ...
vuorinen_neutron_stars
... 2. but not impossible if you systematically use 1st principles results at low and high density 3. Discovering massive stars places strong constraints on nuclear matter EoS due to tension with soft pQCD pressure 4. pQCD constraint useful even if no quark matter present in stars ...
... 2. but not impossible if you systematically use 1st principles results at low and high density 3. Discovering massive stars places strong constraints on nuclear matter EoS due to tension with soft pQCD pressure 4. pQCD constraint useful even if no quark matter present in stars ...
1. The gravitational force is the fundamental force that exists
... C) All nuclei with atomic number greater than 83 are unstable. As the nucleus gets larger, the short– range strong force begins to be overpowered by the long–range electrostatic repulsion. D ) All nuclei with atomic number less than 83 are unstable. These very light elements just don’t have enough m ...
... C) All nuclei with atomic number greater than 83 are unstable. As the nucleus gets larger, the short– range strong force begins to be overpowered by the long–range electrostatic repulsion. D ) All nuclei with atomic number less than 83 are unstable. These very light elements just don’t have enough m ...
What is the Universe made of?
... dwarf, the effect is known as gravitational micro-lensing. By observing many stars over a period of time to see how their appearance changes, scientists hope to detect the presence of massive objects lying between the Earth and the stars – objects that could not normally be detected. ...
... dwarf, the effect is known as gravitational micro-lensing. By observing many stars over a period of time to see how their appearance changes, scientists hope to detect the presence of massive objects lying between the Earth and the stars – objects that could not normally be detected. ...
Diapositiva 1
... • Half-lives of nuclei involved in violent stellar events (waiting points nuclei in rp processes). ...
... • Half-lives of nuclei involved in violent stellar events (waiting points nuclei in rp processes). ...
Sample exam 2
... Essay questions — choose three of the following questions; circle the numbers of the ones chosen, so I know which ones to grade. Please answer each question in sentence/paragraph format or a drawing, depending on what is asked. 11. The Sun started off its trajectory on the Hertzsprung-Russell diagra ...
... Essay questions — choose three of the following questions; circle the numbers of the ones chosen, so I know which ones to grade. Please answer each question in sentence/paragraph format or a drawing, depending on what is asked. 11. The Sun started off its trajectory on the Hertzsprung-Russell diagra ...
Eventually, H burns outward in a shell
... increasingly more complicated, but more stable nuclei. • Up until iron (Fe). Mass (= energy) per Nucleon ...
... increasingly more complicated, but more stable nuclei. • Up until iron (Fe). Mass (= energy) per Nucleon ...
Unit 1
... • a. The neutrino are of the wrong type (mostly muon neutrinos and no electron neutrinos) • b. The neutrinos are about twice as energetic on average than is predicted by theoretical models of the Sun. • c. Only about 1/3 of the expected number of neutrinos is observed, compared to theoretical models ...
... • a. The neutrino are of the wrong type (mostly muon neutrinos and no electron neutrinos) • b. The neutrinos are about twice as energetic on average than is predicted by theoretical models of the Sun. • c. Only about 1/3 of the expected number of neutrinos is observed, compared to theoretical models ...
Stability of hot neutron stars
... The problem of damping of stellar oscillations in presence of a Urca shell is solved analytically in a plane symmetrical approximation. Low-amplitude oscillations are considered. Oscillatory pressure perturbations induce beta reactions of the electron capture and decay in the thin layer around the U ...
... The problem of damping of stellar oscillations in presence of a Urca shell is solved analytically in a plane symmetrical approximation. Low-amplitude oscillations are considered. Oscillatory pressure perturbations induce beta reactions of the electron capture and decay in the thin layer around the U ...
formation of stars
... (b) A nova [new star] forms from a white dwarf that has flared up brilliantly, brightening a hundred a hundred to a million times. A nova may be the result of the bombardment by a companion star. Novas fade to their former luminosity in a few years at ...
... (b) A nova [new star] forms from a white dwarf that has flared up brilliantly, brightening a hundred a hundred to a million times. A nova may be the result of the bombardment by a companion star. Novas fade to their former luminosity in a few years at ...
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.