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pdf of paper
pdf of paper

... protons. Amazingly enough, another heliwn nucleus collides \\ith this shortlived target, leading to the formation of carbon. The process would seem about as likely as crossing a stream by stepping fleetingly on a log. A delicate match between the energies of helium, the unstable berylJium and the re ...
n,n - Osaka University
n,n - Osaka University

... The r-process makes ~half the nuclides heavier than iron, and all nuclides heavier than 209Bi. It is thought to occur in ~second in the bubble just outside the nascent neutron star, in a hot n wind. The r-process requires a neutron density ~1020 cm-3 in order to have it go fast enough to circumvent ...
Supernovae and compact objects
Supernovae and compact objects

... very closely in a binary system. If they are sufficiently close, they will emit gravitational radiation as they orbit, which will remove energy from the orbit and cause them to eventually collide and merge. This is referred to as the double-degenerate scenario, since it involves two degenerate stars ...
The Death of High Mass Stars
The Death of High Mass Stars

... hundred light years across) in our Galaxy (the Interstellar Medium stuff between the stars). The atoms and molecules in these clouds are moving with speeds according to the temperature of the cloud. If the cloud is cold enough, the particles will begin to come together due to the attractive force of ...
“Reach for the Stars” Practice Exam
“Reach for the Stars” Practice Exam

Lecture 10a Neutron Star and Black Holes (Test 2 overview)
Lecture 10a Neutron Star and Black Holes (Test 2 overview)

... unbound “free” electrons for every Fe •  Electrons are “degenerate” as so close together. This causes them to provide most of the pressure resisting gravity •  Enormous stress. If electrons “give way” leaves “hole” in center of star PHYS 162 ...
The correct answers are written in bold, italic and underlined. The
The correct answers are written in bold, italic and underlined. The

... 9. What causes a Type I supernova? • In a binary star system, a giant star filling its Roche lobe dumps gas onto a white dwarf, bringing the white dwarf up to the Chandrasekhar mass limit. • The core of a massive star is gradually transformed into iron by thermonuclear fusion reactions until it coll ...
Some Elements of Nuclear Physics Physics 3070 Spring, 2003
Some Elements of Nuclear Physics Physics 3070 Spring, 2003

Astronomy 112: The Physics of Stars Class 8 Notes: Nuclear
Astronomy 112: The Physics of Stars Class 8 Notes: Nuclear

... Z C, where A is the atomic weight, Z is the atomic number, and C is the symbol for that element. This is slightly redundant, since a chemical symbol C uniquely identifies the atomic number Z. However, writing out the numbers explicitly makes it easier to keep track of the charges, and to assure ours ...
Lifetimes of stars
Lifetimes of stars

Slide 1
Slide 1

... remain trapped inside it -- they get scrunched up. This increases the strength of the magnetic field by a huge factor (1010 to 1012). What provides the energy for a pulsar? The root source is the rapid rotation of the neutron star, which results from the collapse of a much larger, rotating core. Aga ...
ppt - Slides by Prof Christian
ppt - Slides by Prof Christian

... WDs with more than ~ 1.4 solar masses can not exist! Chandrasekhar Limit = 1.4 Msun ...
Frank Timmes (ASU)
Frank Timmes (ASU)

Stages in the Life of a Star
Stages in the Life of a Star

... uses up the hydrogen in its core. This compresses and heats the core. (B)The heated core ignites the surrounding gas to make a shell source, and the outer layers of the star expand, turning it into a red giant. ...
GoldCreation
GoldCreation

Star Life Guided Notes
Star Life Guided Notes

... determines the fate of a star. gravityand _____ fusion The two forces acting on a star are ____ When a star reaches the end of its life it begins to helium and it ______. fuse ______ swells planetary When fusion stops a typical star will producenebula a __ white dwarf and become a ______ _____. Even ...
Neutron Stars
Neutron Stars

... The energy source for the repeated gamma-ray bursts (SGRs) from some neutron stars is what? A: fusion of hydrogen on the surface B: energy released by material accreting onto the surface. C: the result of reconfigurations of the strong magnetic fields ...
Star Life Cycles WS
Star Life Cycles WS

... *(hint – they follow in order with the tutorial) ...
He fusion
He fusion

... Energy released per fusion = 3.96 x 10-12 J ...
Ay 102: Homework 5 (Blast waves, Supernova Remnant) S. R. Kulkarni
Ay 102: Homework 5 (Blast waves, Supernova Remnant) S. R. Kulkarni

... 1050 erg and mass of ejecta (predominantly heavy elements) could be as much as 0.1 M . Redo the calculations for phase 1 and phase 2. 3. Stellar Winds Consider a star with a strong stellar wind: Ṁ = 10−6 M yr−1 and terminal velocity, vw = 103 km s−1 embedded in a medium with density, n0 . As befo ...
Can We Make A Star?
Can We Make A Star?

... move so that the gasses will react with each other • Then we just sit way back and wait until the gasses explode into a fireball ...
Structure of the Sun, our nearest star
Structure of the Sun, our nearest star

lecture19 - Stony Brook University
lecture19 - Stony Brook University

... that are moving away from us with huge speeds, using the observed Doppler shifts of known spectral lines. This indicates that they are very very far away (we will make this connection between recessional velocity and distance clear later – it’s called the Hubble expansion of the universe). From the ...
“Astronomy Picture of the Day” Leads to a Research Breakthrough
“Astronomy Picture of the Day” Leads to a Research Breakthrough

1.4 Whiteboard Review!
1.4 Whiteboard Review!

... • When a nucleus undergoes alpha decay, what will happen to the mass? the atomic number? ...
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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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