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核物质对称能 - 交叉学科理论研究中心
核物质对称能 - 交叉学科理论研究中心

...  The symmetry energy at subsaturation densities have been relatively wellconstrained. But at very low densities, the clustering could be important and how does it affect the symmetry energy?  All the constraints on the high density Esym come from HIC’s (FOPI), and all of them are based on transpor ...
Nuclear Physics
Nuclear Physics

School of Physics Multiwavelength Observations of Evolved Stars Research project in Astrophysics
School of Physics Multiwavelength Observations of Evolved Stars Research project in Astrophysics

... The project involves observation and theoretical modelling of stellar systems containing evolved giant stars with masses similar to that of our own Sun. Although supernovae are showy objects, stars with mass similar to our Sun are much more plentiful and when they evolve to the red giant stage they ...
β-Decay Half-Lives of 110 Neutron-Rich Nuclei across the N = 82
β-Decay Half-Lives of 110 Neutron-Rich Nuclei across the N = 82

... Introduction.—The origin of the heavy elements from iron to uranium is one of the main open questions in science. The slow neutron-capture (s) process of nucleosynthesis [1,2], occurring primarily in helium-burning zones of stars, produces about half of the heavy element abundance in the universe. T ...
Document
Document

... heating the star. In the case of an ideal gas, one half the radiated energy will go into Egrav , and the other half into Ei . Note also from (10.1.9), that since Egrav < 0, the total energy of a star will be negative (which means the star is bound). Only if the star is completely relativistically de ...
Nobel Prize in Physics for Accelerating Universe
Nobel Prize in Physics for Accelerating Universe

... • “Similar” means that the fraction of heavy water is same as in our oceans. • Heavy water is D2O instead of H2O, where D is deuterium which has a nucleus with one proton and one neutron. • The comet comes from the Kupier belt (30-50 AU) while most comets come from the Oort cloud (> 5000 AU). ...
Integrative Studies 410 Our Place in the Universe
Integrative Studies 410 Our Place in the Universe

... • Since the 17th century we use a scheme that lists stars by constellation – in order of their apparent brightness – labeled alphabetically in Greek alphabet – Alpha Centauri is the brightest star in constellation ...
Time From the Perspective of a Particle Physicist
Time From the Perspective of a Particle Physicist

... Cosmology. Hubble law  Universe is expanding, gives universe’s age, depends on Hubble “constant” changes with time. Closed universe has gravity slowing the expansion so it starts to contract. Open universe expands forever. Early universe was very hot and when matter was created. First electrons, pr ...
Stellar Evolution – Life of a Star
Stellar Evolution – Life of a Star

... • White Dwarfs are also burning, but these stars burn heavier elements (e.g. C). Each burning creates and burns a heavier element (e.g, Ne, O, Si, S and Fe). The burning raises the core temperature and each elemental burning period is shorter than the previous. Fusion cannot continue after Fe, inter ...
Lesson Plan: Supernova`s
Lesson Plan: Supernova`s

... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
Page 1 of 4 KEY PSCI 1055 Test #4 (Form A) KEY Spring 2008
Page 1 of 4 KEY PSCI 1055 Test #4 (Form A) KEY Spring 2008

... 6. (10 points) An old manuscript is found and carbon-14 dating is used to estimate its age. Carbon-14 decays to N-14 with a half-life of 5730 years. A measurement of the abundance of these two nuclides indicates there is 4 parts of carbon-14 to 12 parts of nitrogen-14. a. How many parts of carbon-1 ...
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... The gas also starts out hot, and initially is kept hot by the white dwarf, but it will also cool off over time. So the lifetime of a PN is relatively short, just a few 10s of thousands of years. ...
Calculating Main Sequence Lifetimes
Calculating Main Sequence Lifetimes

... Since ancient times, the brightness of a star is indicated by "magnitudes": 1, 2 and so on, with dim stars having larger magnitudes. Don’t confuse the relative magnitude with absolute magnitude. The relative magnitude measures the brightness of a star as it appears in the sky and it depends on the b ...
What is a Star - Optics Institute of Southern California
What is a Star - Optics Institute of Southern California

... greater than several solar masses) are convective deep in their cores, and are radiative in their outer layers. Low mass stars (i.e., mass comparable to the Sun and below) are convective in their outer layers and radiative in their cores. Intermediate mass stars (spectral type A) may be radiative th ...
Chapter 12 Stellar Evolution
Chapter 12 Stellar Evolution

... flash. The star expands into a red giant as the core continues to collapse. The envelope blows off, leaving a white dwarf to gradually cool. ...
– 1 – 1. Nucleosynthetic Yields From Various Sources
– 1 – 1. Nucleosynthetic Yields From Various Sources

... Free neutrons decay with a mean lifetime of ∼15 min via the last of the three reactions listed above. Depending on whether there is enough time for the various unstable isotopes that may be produced to decay, one can end up with different isotopic compositions. This is not only the case for the neut ...
Star Life Cycle Computer Lab
Star Life Cycle Computer Lab

... 10. Do the Interactive Equilibrium Lab and Practice Quizzes. 11. After their life on the main sequence, what happens to massive stars? 12. What is the 3rd fuel that stars can use after Hydrogen and Helium? The Beginning of the End 13. When a star is fusing helium, what stage of its life is it consid ...
Lecture 10 - Concord University
Lecture 10 - Concord University

... The scenario that leads to nova explosions can produce an even wilder phenomenon. In the early 1900s `novae’ were sometimes observed in other galaxies and were used to help set the distances to galaxies. But, when it became clear that even the nearest galaxies were much further away than anyone ...
Supernovae — Oct 21 10/21/2011 • Outline
Supernovae — Oct 21 10/21/2011 • Outline

... Where were the elements in the baby made? • Carbon was made and expelled by giants • Iron was made in massive stars and expelled by supernovae • Heavier elements were made in supernovae & in giants, where there are free neutrons. Nuclei capture neutrons. ...
the atomic model - Biology2014-7
the atomic model - Biology2014-7

... of nature has been unified The electromagnetic, strong and weak forces form GUT Theory ...
ASTR 1050: Survey of Astronomy
ASTR 1050: Survey of Astronomy

... b. the energy they collect is not electromagnetic radiation. c. radio waves have long wavelengths. d. interference from cell phone satellites. e. none of the above. 24. Given good observations of an eclipsing binary, which of the below can we determine? a. the period of the orbit. b. the inclination ...
powerpoint
powerpoint

... • Eventually, the helium core ignites • Carbon and Oxygen are produced from “Helium burning” ...
Background Science - Faulkes Telescope Project
Background Science - Faulkes Telescope Project

White Dwarfs, Neutron Stars, and Black Holes
White Dwarfs, Neutron Stars, and Black Holes

... In order to compress it, we must change the energy of large numbers of electrons. However, only a few electrons (those in the highest occupied levels) can have their energies changed by small amounts. Therefore, the degenerate matter resists compression; it is extremely rigid. It easily conducts bot ...
Chapter 15 (Star Lives)
Chapter 15 (Star Lives)

... D. are at different stages of their lives. 2. In making a model of a star, an astronomer does NOT have to know or assume: A. that the energy given off is produced in the interior. B. the mass of the star. C. the chemical composition of the star. D. the distance to that star. 3. For a star like our s ...
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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.
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