Nucleosynthesis and the death of stars
... • Could stars in principle live forever simply by contracting gravitationally and increasing their temperature to ignite the next heavier source of nuclear fuel whenever they run out? – No. The strong interaction’s range is smaller than the diameters of all but the smaller nuclei, but the range of t ...
... • Could stars in principle live forever simply by contracting gravitationally and increasing their temperature to ignite the next heavier source of nuclear fuel whenever they run out? – No. The strong interaction’s range is smaller than the diameters of all but the smaller nuclei, but the range of t ...
Nuclear Structure, Nuclear Force
... • There are about 270 stable nuclides and about 100 different elements. • 2.7 stable isotopes per element • There are larger than average number of stable isotopes with nuclei with Z equal 2, 8, 20, 28, 50, 82 and 126 (last is theoretical for now) • "Magic Numbers" - closed shell structure, very muc ...
... • There are about 270 stable nuclides and about 100 different elements. • 2.7 stable isotopes per element • There are larger than average number of stable isotopes with nuclei with Z equal 2, 8, 20, 28, 50, 82 and 126 (last is theoretical for now) • "Magic Numbers" - closed shell structure, very muc ...
Determining Abundances
... • [Fe/H] = -1.0 is the same as 1/10 solar • [Fe/H] = -2.0 is the same as 1/100 solar • [m/Fe] = log N(m)/N(Fe)star – log N(m)/N(Fe)Sun • [Ca/Fe] = +0.3 means twice the number of Ca atoms per Fe atom ...
... • [Fe/H] = -1.0 is the same as 1/10 solar • [Fe/H] = -2.0 is the same as 1/100 solar • [m/Fe] = log N(m)/N(Fe)star – log N(m)/N(Fe)Sun • [Ca/Fe] = +0.3 means twice the number of Ca atoms per Fe atom ...
More detailed notes - Particle Physics and Particle Astrophysics
... quickly. Eventually the cloud becomes opaque enough to trap some of the radiation, increasing its internal pressure and temperature, and slowing the collapse. Evolutionary tracks for pre-main-sequence stars of various masses are shown in the HR diagram on the right. The key stages are labelled 1-4 o ...
... quickly. Eventually the cloud becomes opaque enough to trap some of the radiation, increasing its internal pressure and temperature, and slowing the collapse. Evolutionary tracks for pre-main-sequence stars of various masses are shown in the HR diagram on the right. The key stages are labelled 1-4 o ...
STARS
... • Core runs out of He, and is no longer able to fuse the remaining heavier elements • The star blows its outer layer away • The core remains behind and burns as a white dwarf • Eventually it cools to become a black dwarf ...
... • Core runs out of He, and is no longer able to fuse the remaining heavier elements • The star blows its outer layer away • The core remains behind and burns as a white dwarf • Eventually it cools to become a black dwarf ...
Chapter 13
... the hypernova formation of black holes. 23. Which are the two most popular candidates for gamma-ray bursters? A) formation of uranium in the core of a supergiant, and collisions of white dwarfs B) mergers of two black holes, and merger of a neutron star and a white dwarf C) hypernova making a black ...
... the hypernova formation of black holes. 23. Which are the two most popular candidates for gamma-ray bursters? A) formation of uranium in the core of a supergiant, and collisions of white dwarfs B) mergers of two black holes, and merger of a neutron star and a white dwarf C) hypernova making a black ...
1 - Stellar Life Cycle
... center of the new star, this heats stops the rest of the star from collapsing. The balance between gravity trying to make the star shrink and heat holding it up is called Thermodynamic Equilibrium. The star then stays almost exactly the same for a long time (about 10 billion years for a star lik ...
... center of the new star, this heats stops the rest of the star from collapsing. The balance between gravity trying to make the star shrink and heat holding it up is called Thermodynamic Equilibrium. The star then stays almost exactly the same for a long time (about 10 billion years for a star lik ...
Lecture 16, PPT version
... • Extraordinarily bright, so can use them to measure distances to galaxies that are very far away: b = L / (4 d2) • Supernovae are the source of all heavy chemical elements! • The heavy chemical elements are produced during the explosion itself, when there is more than enough energy to fuse nuclei ...
... • Extraordinarily bright, so can use them to measure distances to galaxies that are very far away: b = L / (4 d2) • Supernovae are the source of all heavy chemical elements! • The heavy chemical elements are produced during the explosion itself, when there is more than enough energy to fuse nuclei ...
The Evolution of Stars - hrsbstaff.ednet.ns.ca
... Massive stars have the shortest life span, a mere 7 million years. They burn through their hydrogen very quickly at a very high temperature. The temperature is so hot that once the hydrogen fuses to helium, the helium then fuses to carbon, silicon and finally iron. ...
... Massive stars have the shortest life span, a mere 7 million years. They burn through their hydrogen very quickly at a very high temperature. The temperature is so hot that once the hydrogen fuses to helium, the helium then fuses to carbon, silicon and finally iron. ...
5Stars_Part_Two
... Black Holes: 1. If the mass of the neutron star is bigger than about 2 or 3 solar masses, it don’t care about no neutron exclusion principle. 2. Gravity collapses the neutron star even further. 3. The star becomes a black hole - an object from which even light cannot escape. 4. Light is really fast ...
... Black Holes: 1. If the mass of the neutron star is bigger than about 2 or 3 solar masses, it don’t care about no neutron exclusion principle. 2. Gravity collapses the neutron star even further. 3. The star becomes a black hole - an object from which even light cannot escape. 4. Light is really fast ...
The life cycle of the Sun – HR Diagram
... conductivity of degenerate electron gas allows burning to spread quickly through the core. The increase in temperature does not cause an increase in pressure, and so the heat energy increases the rate of the triple alpha process generating more energy, further increasing the temperature – HELIUM FLA ...
... conductivity of degenerate electron gas allows burning to spread quickly through the core. The increase in temperature does not cause an increase in pressure, and so the heat energy increases the rate of the triple alpha process generating more energy, further increasing the temperature – HELIUM FLA ...
Define Electric Field Strength Electric field
... The number of protons found in the nucleus of an atom The mass number, the sum of the number of neutrons and protons in an atomic nucleus Isotopes are different forms of the same element which have the same number of protons but different numbers of neutrons in their nuclei Spontaneous emission of a ...
... The number of protons found in the nucleus of an atom The mass number, the sum of the number of neutrons and protons in an atomic nucleus Isotopes are different forms of the same element which have the same number of protons but different numbers of neutrons in their nuclei Spontaneous emission of a ...
Astronomy 103 Exam 2 Review
... B. Each observer will see the other's clock to be running fast with respect to the observer's own clock. C. Both observers agree: since the clocks are not moving with respect to each other the clocks run at the same speed and read the same Lme. D. Both observers agree: the clock near Earth i ...
... B. Each observer will see the other's clock to be running fast with respect to the observer's own clock. C. Both observers agree: since the clocks are not moving with respect to each other the clocks run at the same speed and read the same Lme. D. Both observers agree: the clock near Earth i ...
Physics Projects Brochure (Word Document)
... adequate shielding from cosmic ray events that could interfere with the measurements of rare neutrino interactions. It detects antineutrinos from many of the nuclear power plants located in Japan (antineutrinos are formed during radioactive decay), but the flux of antineutrinos is so small that only ...
... adequate shielding from cosmic ray events that could interfere with the measurements of rare neutrino interactions. It detects antineutrinos from many of the nuclear power plants located in Japan (antineutrinos are formed during radioactive decay), but the flux of antineutrinos is so small that only ...
NEUTRON STAR?
... dwarfs are smaller in size than less massive ones. More specifically, why does gravity compress white dwarfs to different sizes? • I absolutely loved the part on neutron stars and on how powerful their density was. That power is almost unimaginable to me. Other than that, I found the reading to be p ...
... dwarfs are smaller in size than less massive ones. More specifically, why does gravity compress white dwarfs to different sizes? • I absolutely loved the part on neutron stars and on how powerful their density was. That power is almost unimaginable to me. Other than that, I found the reading to be p ...
What is a white dwarf?
... Shrinkage of White Dwarfs • Quantum mechanics says that electrons in the same place cannot be in the same state • Adding mass to a white dwarf increases its gravity, forcing electrons into a smaller space • In order to avoid being in the same state in the same place some of the electrons need to ...
... Shrinkage of White Dwarfs • Quantum mechanics says that electrons in the same place cannot be in the same state • Adding mass to a white dwarf increases its gravity, forcing electrons into a smaller space • In order to avoid being in the same state in the same place some of the electrons need to ...
Click here to the PowerPoint
... You might be given a data table of different sizes and lifespans of stars, and be asked to either DESCRIBE the pattern (really easy) or SUGGEST WHY there are differences (see purple box above) ...
... You might be given a data table of different sizes and lifespans of stars, and be asked to either DESCRIBE the pattern (really easy) or SUGGEST WHY there are differences (see purple box above) ...
File
... layers and propels them outward, greatly assisted by the plentiful neutrinos (only a very tiny fraction of which actually interact with the gas). The star explodes, achieving within one day a stupendous optical luminosity rivaling the brightness of a billion normal stars. ...
... layers and propels them outward, greatly assisted by the plentiful neutrinos (only a very tiny fraction of which actually interact with the gas). The star explodes, achieving within one day a stupendous optical luminosity rivaling the brightness of a billion normal stars. ...
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.