White Dwarf
... • At high density, the electromagnetic force between electrons holds the material of the core apart. • This compressed material is degenerate matter. – Core of giant stars – Sun mass in Earth size ...
... • At high density, the electromagnetic force between electrons holds the material of the core apart. • This compressed material is degenerate matter. – Core of giant stars – Sun mass in Earth size ...
Make one copy for each student on plain paper. Life Cycle of Star
... collapse leading to a massive explosion that can remain visible for months. ...
... collapse leading to a massive explosion that can remain visible for months. ...
Life Cycle of Star Pictures
... collapse leading to a massive explosion that can remain visible for months. ...
... collapse leading to a massive explosion that can remain visible for months. ...
Answers
... like star has become a red giant. In a sun-like star, fusion stops at this point once the 4He has been exhausted, leaving a high temperature, degenerate core as a white dwarf star. The timescale of helium fusion in a sun-like star is about 10% of the hydrogen burning phase, for the sun about 109 yea ...
... like star has become a red giant. In a sun-like star, fusion stops at this point once the 4He has been exhausted, leaving a high temperature, degenerate core as a white dwarf star. The timescale of helium fusion in a sun-like star is about 10% of the hydrogen burning phase, for the sun about 109 yea ...
Chapter 20 Review of Stars` Lifetime Review
... • There is a limit to the amount of pressure the degenerate electrons can produce • Therefore, there is an upper limit to the mass that a white dwarf can have • This limit is the Chandrasekhar limit ...
... • There is a limit to the amount of pressure the degenerate electrons can produce • Therefore, there is an upper limit to the mass that a white dwarf can have • This limit is the Chandrasekhar limit ...
Lecture 31 - 2 The Death of Stars: Stellar Recycling Phase 3 -
... energy which is sufficient to halt the collapse. Two basic reactions produce Carbon and Oxygen: 3 He → C + energy (the “triple alpha process”) C + He → O + energy These reactions continue for a time approximately equal to 10% of the main sequence lifetime until all of the Helium has been converted i ...
... energy which is sufficient to halt the collapse. Two basic reactions produce Carbon and Oxygen: 3 He → C + energy (the “triple alpha process”) C + He → O + energy These reactions continue for a time approximately equal to 10% of the main sequence lifetime until all of the Helium has been converted i ...
6.6
... Wolfgang Pauli and Enrico Fermi hypothesized the existence of a third particle in the products of a beta decay in 1933. This third very light particle would carry the remainder of the available energy. Fermi coined the word neutrino, the Italian word for “little ...
... Wolfgang Pauli and Enrico Fermi hypothesized the existence of a third particle in the products of a beta decay in 1933. This third very light particle would carry the remainder of the available energy. Fermi coined the word neutrino, the Italian word for “little ...
5 Elements of nuclear physics 5.1 Strong interaction and structure of atomic nuclei
... states of nuclei. The typical excitation energy is ∼ 1 MeV therefore these transitions may be accompanied by emission of gamma-ray lines. The weak interaction opens the way for mutual transformations of protons and neutrons. For example, a free neutron decays as n → p + e− + ν̃ ...
... states of nuclei. The typical excitation energy is ∼ 1 MeV therefore these transitions may be accompanied by emission of gamma-ray lines. The weak interaction opens the way for mutual transformations of protons and neutrons. For example, a free neutron decays as n → p + e− + ν̃ ...
Nebula – • The most abundant element in the universe is hydrogen
... A star is a sphere of super-hot gases, mostly hydrogen and helium that is held together by its own gravity. No two stars contain exactly the same elements in the same proportions. Stars are born by contraction of gasses inside a nebula. ...
... A star is a sphere of super-hot gases, mostly hydrogen and helium that is held together by its own gravity. No two stars contain exactly the same elements in the same proportions. Stars are born by contraction of gasses inside a nebula. ...
Physics 228 Today: April 22, 2012 Ch. 43 Nuclear
... and binding energy make a small difference, but usually if we ignore the inclusion of electrons it is not an issue, since the number of nucleons and electrons is constant for all processes we will consider here. The total nuclear binding energy is the total energy needed to separate a nucleus into i ...
... and binding energy make a small difference, but usually if we ignore the inclusion of electrons it is not an issue, since the number of nucleons and electrons is constant for all processes we will consider here. The total nuclear binding energy is the total energy needed to separate a nucleus into i ...
Stars II. Stellar Physics
... uniqueness of the solution is claimed in the Russel-VogtTheorem: For a star of given chemical composition and mass there exists only one equilibrium configuration which solves the boundary problem of stellar structure. [In this generality, the theorem is not proven. Local uniqueness can be shown, ho ...
... uniqueness of the solution is claimed in the Russel-VogtTheorem: For a star of given chemical composition and mass there exists only one equilibrium configuration which solves the boundary problem of stellar structure. [In this generality, the theorem is not proven. Local uniqueness can be shown, ho ...
Nuclear Chemistry - HCC Learning Web
... • A different unit is used for measuring the biological effects of radiation because the effects depend on the type and energy of the radiation • The sievert (Sv) is the SI unit of dose equivalent, H • The dose equivalent (in Sv) is a product of the absorbed dose (D) from some radiation source time ...
... • A different unit is used for measuring the biological effects of radiation because the effects depend on the type and energy of the radiation • The sievert (Sv) is the SI unit of dose equivalent, H • The dose equivalent (in Sv) is a product of the absorbed dose (D) from some radiation source time ...
ASTRONOMY 1102 1
... Core collapse SN: the death of a massive star; Carbon{detonation SN or Type Ia SN: the collapse of a WD pushed over the brink (maximum mass is Chandrasekhar Mass = 1.4 M ). This can happen because of accretion or a merger of two WD. The ejected envelope is seen for 104 years as a SN remnant. The f ...
... Core collapse SN: the death of a massive star; Carbon{detonation SN or Type Ia SN: the collapse of a WD pushed over the brink (maximum mass is Chandrasekhar Mass = 1.4 M ). This can happen because of accretion or a merger of two WD. The ejected envelope is seen for 104 years as a SN remnant. The f ...
Stellar Evolution Slideshow
... After a star explodes, sometimes only neutrons are left (Guess where the name “Neutron Stars” came from?) Also called Pulsars because they emit radio waves with incredible regularity. Appear to be rapidly rotating neutron star ...
... After a star explodes, sometimes only neutrons are left (Guess where the name “Neutron Stars” came from?) Also called Pulsars because they emit radio waves with incredible regularity. Appear to be rapidly rotating neutron star ...
White Dwarfs - Chandra X
... limit—it will collapse. In a binary star system this could happen if a nearby companion star dumps enough material onto a white dwarf to push it over the Chandrasekhar limit. The resulting collapse and explosion of the white dwarf is believed to be responsible for the so-called Type Ia supernovas. O ...
... limit—it will collapse. In a binary star system this could happen if a nearby companion star dumps enough material onto a white dwarf to push it over the Chandrasekhar limit. The resulting collapse and explosion of the white dwarf is believed to be responsible for the so-called Type Ia supernovas. O ...
Practice Homework 2: Properties of Stars 1. Star A is 100 times more
... 5. An Astronomer claims that he has found sodium in a certain star. Explain how he might have discovered it? 6. The Light in sun is created in the interior of the sun which is extremely hot and dense while the outer layers are relatively colder. What kind of spectrum it should produce? Helium in the ...
... 5. An Astronomer claims that he has found sodium in a certain star. Explain how he might have discovered it? 6. The Light in sun is created in the interior of the sun which is extremely hot and dense while the outer layers are relatively colder. What kind of spectrum it should produce? Helium in the ...
PHYS 221 Midterm Practice Summer 2012
... halfway between the spheres. What is not zero? One electrons (-e) and two protons (+e) are placed an equal distance r away from the origin in the configuration shown. If another proton were placed at the origin, what is the electric force felt by that proton. ...
... halfway between the spheres. What is not zero? One electrons (-e) and two protons (+e) are placed an equal distance r away from the origin in the configuration shown. If another proton were placed at the origin, what is the electric force felt by that proton. ...
PowerPoint version is here
... This is a special time • Wealth of new astronomical observations--require new nuclear data for a credible interpretation • New accelerators of radioactive nuclei to provide this data • Growing computational power to simulate the phenomena ...
... This is a special time • Wealth of new astronomical observations--require new nuclear data for a credible interpretation • New accelerators of radioactive nuclei to provide this data • Growing computational power to simulate the phenomena ...
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.