Brock physics - Brock University
... (d) * much, much greater than the average density of the Earth. 22. The main factor preventing the further collapse of a white dwarf is (a) extremely high core temperature. (b) extremely low core temperature. (c) * electron degeneracy pressure. (d) neutron degeneracy pressure. (e) [White dwarfs have ...
... (d) * much, much greater than the average density of the Earth. 22. The main factor preventing the further collapse of a white dwarf is (a) extremely high core temperature. (b) extremely low core temperature. (c) * electron degeneracy pressure. (d) neutron degeneracy pressure. (e) [White dwarfs have ...
The Sun-Earth-Moon System
... star becomes hot enough for fusion to begin. • The star becomes stable because the pressure caused by fusion balances out gravity. ...
... star becomes hot enough for fusion to begin. • The star becomes stable because the pressure caused by fusion balances out gravity. ...
Determining the Distance to the Moon Triangulation
... produced by steady fusion (less abundant elements we didn’t discuss, like Cl, Na, made in reactions that aren’t important energy makers). Heavier elements (such as lead, gold, copper, silver, etc.) by "neutron capture" in core, even heavier ones (uranium, plutonium, etc.) in supernova itself. ...
... produced by steady fusion (less abundant elements we didn’t discuss, like Cl, Na, made in reactions that aren’t important energy makers). Heavier elements (such as lead, gold, copper, silver, etc.) by "neutron capture" in core, even heavier ones (uranium, plutonium, etc.) in supernova itself. ...
The light curves for a nova look like the following.
... The s-process works as long as the decay time for unstable isotopes is longer than the capture time. Up to the element bismuth (atomic number 83), the s-process works, but above this point the more massive nuclei that can be built from bismuth are unstable. 2) r-process (r means rapid) In this proce ...
... The s-process works as long as the decay time for unstable isotopes is longer than the capture time. Up to the element bismuth (atomic number 83), the s-process works, but above this point the more massive nuclei that can be built from bismuth are unstable. 2) r-process (r means rapid) In this proce ...
9.1: THE SUN IN BULK PHYS 1401: Descriptive Astronomy Notes
... Nuclear Fusion ✦ The only possible way to account for the amount of energy produced by the sun ✦ In general: Two nuclei are forced to join together, to form a third, different nucleus ✦ Energy is released according to E = mc2 ✦ As fusion occurs in the sun's core, it slowly loses mass (that is conver ...
... Nuclear Fusion ✦ The only possible way to account for the amount of energy produced by the sun ✦ In general: Two nuclei are forced to join together, to form a third, different nucleus ✦ Energy is released according to E = mc2 ✦ As fusion occurs in the sun's core, it slowly loses mass (that is conver ...
Nuclear Magnetic Resonance
... Magnetic Shielding • If all protons absorbed the same amount of energy in a given magnetic field, not much information could be obtained. • But protons are surrounded by electrons that shield them from the external field. • Circulating electrons create an induced magnetic field that opposes the ext ...
... Magnetic Shielding • If all protons absorbed the same amount of energy in a given magnetic field, not much information could be obtained. • But protons are surrounded by electrons that shield them from the external field. • Circulating electrons create an induced magnetic field that opposes the ext ...
proton 8x106 ms
... 2. Calculate the work done on a proton which is placed in a 3kV electric field. 3. In a particle accelerator, electric fields are used to accelerate sub atomic particles. By equating work done and kinetic energy, find the velocity of each of the following when placed in a 14kV electric field, assumi ...
... 2. Calculate the work done on a proton which is placed in a 3kV electric field. 3. In a particle accelerator, electric fields are used to accelerate sub atomic particles. By equating work done and kinetic energy, find the velocity of each of the following when placed in a 14kV electric field, assumi ...
Weathering, Erosion and Mass Movement
... Fusion is combining of lightweight nuclei into heavier nuclei, such as four hydrogen nuclei combining to form a helium nucleus. ...
... Fusion is combining of lightweight nuclei into heavier nuclei, such as four hydrogen nuclei combining to form a helium nucleus. ...
File
... The explosion called a supernova occurs after a large star has become a red supergiant. When the star stops expanding because it can no longer create enough energy to support its own mass, it collapses completely and makes a giant explosion. A supernova is brighter than all the stars in the galaxy c ...
... The explosion called a supernova occurs after a large star has become a red supergiant. When the star stops expanding because it can no longer create enough energy to support its own mass, it collapses completely and makes a giant explosion. A supernova is brighter than all the stars in the galaxy c ...
Ay123 Fall 2011 STELLAR STRUCTURE AND EVOLUTION Problem Set 1
... as a function of the total stellar mass (expressed in units of M⊙ ). At what mass does the radiation pressure become comparable to the ideal-gas pressure ? e. Write down an explicit expression for the total gravitational potential energy of this toy star, and verify that the virial theorem is exactl ...
... as a function of the total stellar mass (expressed in units of M⊙ ). At what mass does the radiation pressure become comparable to the ideal-gas pressure ? e. Write down an explicit expression for the total gravitational potential energy of this toy star, and verify that the virial theorem is exactl ...
Stellar Evolution: After the Main Sequence
... surrounded by a shell through which hydrogen fusion works its way outward in the star • The core shrinks and becomes hotter, while the star’s outer layers expand and cool • The result is a red giant star ...
... surrounded by a shell through which hydrogen fusion works its way outward in the star • The core shrinks and becomes hotter, while the star’s outer layers expand and cool • The result is a red giant star ...
Unit 11: Stellar Evolution
... The core temperature becomes so high that the nuclei themselves are broken down into individual protons and neutrons absorbing still more energy. At still-higher temperatures, electrons and protons combine to produce neutrons and neutrinos; again, an energy-absorbing reaction. Because the number of ...
... The core temperature becomes so high that the nuclei themselves are broken down into individual protons and neutrons absorbing still more energy. At still-higher temperatures, electrons and protons combine to produce neutrons and neutrinos; again, an energy-absorbing reaction. Because the number of ...
The Life Cycles of Stars, Part I
... Imagine an enormous cloud of gas and dust many light-years across. Gravity, as it always does, tries to pull the materials together. A few grains of dust collect a few more, then a few more, then more still. Eventually, enough gas and dust has been collected into a giant ball that, at the center of ...
... Imagine an enormous cloud of gas and dust many light-years across. Gravity, as it always does, tries to pull the materials together. A few grains of dust collect a few more, then a few more, then more still. Eventually, enough gas and dust has been collected into a giant ball that, at the center of ...
Where Do Chemical Elements Come From?
... both which elements and how much of each element was produced over time. The net result is that most scientists accepted the idea that some elements were created during Big Bang (big bang nucleosynthesis) and that many elements continued to be created by stellar nucleosynthesis. B2FH were able to id ...
... both which elements and how much of each element was produced over time. The net result is that most scientists accepted the idea that some elements were created during Big Bang (big bang nucleosynthesis) and that many elements continued to be created by stellar nucleosynthesis. B2FH were able to id ...
Pulsars - Chabot College
... Essay Questions for the exam… (a) What is a pulsar? Where does it get its ...
... Essay Questions for the exam… (a) What is a pulsar? Where does it get its ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... Sometimes there’s just no way to know. We observe supernovae now where the type is in doubt; the lightcurve and spectrum are consistent with both types. This is also true of remnants observed from historical supernoave. 2. Consider a binary system consisting of a main sequence star and a white dwarf ...
... Sometimes there’s just no way to know. We observe supernovae now where the type is in doubt; the lightcurve and spectrum are consistent with both types. This is also true of remnants observed from historical supernoave. 2. Consider a binary system consisting of a main sequence star and a white dwarf ...
Life Cycle of Stars - Lab Science Schedule
... may have a mass of several tons. White dwarfs still shine with a cool, white light. When the last of its energy is gone it becomes a dead star. How long this takes depends on the mass of the star when it was first formed. The smaller the starting mass of a star, the longer it will live. IV. Massive ...
... may have a mass of several tons. White dwarfs still shine with a cool, white light. When the last of its energy is gone it becomes a dead star. How long this takes depends on the mass of the star when it was first formed. The smaller the starting mass of a star, the longer it will live. IV. Massive ...
Stars - Moodle
... • After the main sequence, stars with a mass much greater than the sun can burn and create larger and larger elements • When it gets to iron, it takes too much energy to create other elements so it collapses • This causes a ___________________, this is when heavier elements are made ...
... • After the main sequence, stars with a mass much greater than the sun can burn and create larger and larger elements • When it gets to iron, it takes too much energy to create other elements so it collapses • This causes a ___________________, this is when heavier elements are made ...
s-process
... Significant production of r-process elements began when the metallicity of the Galaxy reached [Fe/H] = -3. The heavy n-capture elements were formed predominantly by the r-process at metallicities below [Fe/H] = -2.1. Elements from the s-process appear at a metallicity of [Fe/H] = -2.1, when low-mass ...
... Significant production of r-process elements began when the metallicity of the Galaxy reached [Fe/H] = -3. The heavy n-capture elements were formed predominantly by the r-process at metallicities below [Fe/H] = -2.1. Elements from the s-process appear at a metallicity of [Fe/H] = -2.1, when low-mass ...
The Milky Way
... high-energy particles At this time, no star capable of producing a supernova is less than 50 ly away. The most massive star known (~ 100 solar masses) is ~ 25,000 ly from ...
... high-energy particles At this time, no star capable of producing a supernova is less than 50 ly away. The most massive star known (~ 100 solar masses) is ~ 25,000 ly from ...
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.