Stellar_Evol
... Massive Stars • Produce enough heat to fuse heavier elements • From many layers w/fusion of different elements ...
... Massive Stars • Produce enough heat to fuse heavier elements • From many layers w/fusion of different elements ...
Stellar Death High Mass Stars
... Core contracts - temperature increases Uncontrollable gravitational collapse vNuclei converted back into He He protons and neutrons proton + electron neutron + neutrino vCore Implodes Envelope Explodes Supernova ...
... Core contracts - temperature increases Uncontrollable gravitational collapse vNuclei converted back into He He protons and neutrons proton + electron neutron + neutrino vCore Implodes Envelope Explodes Supernova ...
ib atomic and nuclear physics definitions and concepts
... RADIOACTIVE DECAY: A random and spontaneous process in which unstable nuclei emit a particle (disintegrate). The rate decreases exponentially with time. NATURAL RADIOACTIVE DECAY: The emission of an alpha or beta particle. NUCLEAR STRONG FORCE: The force that holds the particles of a nucleus togethe ...
... RADIOACTIVE DECAY: A random and spontaneous process in which unstable nuclei emit a particle (disintegrate). The rate decreases exponentially with time. NATURAL RADIOACTIVE DECAY: The emission of an alpha or beta particle. NUCLEAR STRONG FORCE: The force that holds the particles of a nucleus togethe ...
Stellar Deaths - Mid
... outer shell burns He even quicker, making the Star becomes unstable. Ejects outer layers in pulses. "Planetary Nebula" (Historical name, nothing to do with planets.) - Once all the fuel has burned off, what’s left is a Carbon core called a “White Dwarf” ...
... outer shell burns He even quicker, making the Star becomes unstable. Ejects outer layers in pulses. "Planetary Nebula" (Historical name, nothing to do with planets.) - Once all the fuel has burned off, what’s left is a Carbon core called a “White Dwarf” ...
PHY-105: Final Stages of Stellar Evolution
... Refer to the class notes to make sure you understand what each term means. For a star like the Sun, we saw that this fraction is about 8%. What consequently happens to the star depends critically on mass, but we’ll look at typical cases. When the SC limit is reached, core begins to collapse causing ...
... Refer to the class notes to make sure you understand what each term means. For a star like the Sun, we saw that this fraction is about 8%. What consequently happens to the star depends critically on mass, but we’ll look at typical cases. When the SC limit is reached, core begins to collapse causing ...
Chapter 25 – Types of Radiation 1. Alpha Radiation Alpha decay
... Positron decay is the mirror image of beta decay and can be described as: a. Something inside the nucleus breaks down causing a proton to become a neutron. b. It emits a positron which goes zooming off. c. The atomic number goes down by one and the mass number remains unchanged. Here is a typical po ...
... Positron decay is the mirror image of beta decay and can be described as: a. Something inside the nucleus breaks down causing a proton to become a neutron. b. It emits a positron which goes zooming off. c. The atomic number goes down by one and the mass number remains unchanged. Here is a typical po ...
Science Centre Talk
... formed in a supernova explosion On the way, massive stars make pretty much all the elements heavier than oxygen (and quite a lot of the lighter ones): “we are stardust” ...
... formed in a supernova explosion On the way, massive stars make pretty much all the elements heavier than oxygen (and quite a lot of the lighter ones): “we are stardust” ...
Nuclear Fission & Fusion PPT
... •Bombarded Uranium-235 samples with neutrons expecting the Uranium-235 to capture neutrons •Instead, the products showed different chemical properties that they could not explain ...
... •Bombarded Uranium-235 samples with neutrons expecting the Uranium-235 to capture neutrons •Instead, the products showed different chemical properties that they could not explain ...
type II supernova
... • This sudden collapse of a massive star's core into a volume over a million times smaller than its original volume is really bad news for the star. The outer layers of the star come raining down onto the core. Somehow this collapse changes into an explosion: a type II supernova. The process by whic ...
... • This sudden collapse of a massive star's core into a volume over a million times smaller than its original volume is really bad news for the star. The outer layers of the star come raining down onto the core. Somehow this collapse changes into an explosion: a type II supernova. The process by whic ...
Vocabulary Review
... a large cloud of gas and dust in interstellar space; a region where a star is born ...
... a large cloud of gas and dust in interstellar space; a region where a star is born ...
Astronomy 20 Homework # 5 1.
... (a) Derive a formula for the b.h. luminosity as a function of its mass, assuming that its e ective area is 4RS2 , where RS is the Schwarzschild radius. (b) By setting L = c2 dM=dt, derive and solve the di erential equation for the evaporation time of a black hole with an initial mass of M0 . (c) E ...
... (a) Derive a formula for the b.h. luminosity as a function of its mass, assuming that its e ective area is 4RS2 , where RS is the Schwarzschild radius. (b) By setting L = c2 dM=dt, derive and solve the di erential equation for the evaporation time of a black hole with an initial mass of M0 . (c) E ...
the life cycle of stars
... the main-sequence. • This is the second and longest stage of its life. • Energy is generated in the core and causes the star to shine. • The size of the star changes very little as long as its supply of hydrogen nuclei fuse into helium nuclei. ...
... the main-sequence. • This is the second and longest stage of its life. • Energy is generated in the core and causes the star to shine. • The size of the star changes very little as long as its supply of hydrogen nuclei fuse into helium nuclei. ...
supernova!
... settle to the centre. It is merely a consequence of the fact that the progressively heavier elements are created near the centre, where the temperature progressively becomes high enough to do so! The outer envelope of the star is still the pristine material from which it was made (mainly Hydrogen an ...
... settle to the centre. It is merely a consequence of the fact that the progressively heavier elements are created near the centre, where the temperature progressively becomes high enough to do so! The outer envelope of the star is still the pristine material from which it was made (mainly Hydrogen an ...
Slide 1
... If mass from a red giant flows onto a white dwarf, explosive brightness changes of 10000× occur (novae), to 150,000 L. So much matter can flow onto the white dwarf star that the Chandrasekhar Limit (1.4 M) can be exceeded. Electron degeneracy is defeated! ...
... If mass from a red giant flows onto a white dwarf, explosive brightness changes of 10000× occur (novae), to 150,000 L. So much matter can flow onto the white dwarf star that the Chandrasekhar Limit (1.4 M) can be exceeded. Electron degeneracy is defeated! ...
Week 12, Lecture 2 – Nuclear Synthesis
... Big Bang Nucleosynsthesis Recall that we have a fundamental equivalence between mass and energy, which combined with the basic assump
... Big Bang Nucleosynsthesis Recall that we have a fundamental equivalence between mass and energy, which combined with the basic assump
Astronomy 115 Homework Set #1 – Due: Thursday, Feb
... Astronomy 201 Homework Set #5 – Due: Tuesday, March 24 ...
... Astronomy 201 Homework Set #5 – Due: Tuesday, March 24 ...
Chapter 25 Radioactivity
... Isotopes: atoms of the same element with different numbers of neutrons i.e 1214C and 1213C each has 12 protons which is the Atomic number. The mass number varies. It is the sum of the protons and neutrons. ...
... Isotopes: atoms of the same element with different numbers of neutrons i.e 1214C and 1213C each has 12 protons which is the Atomic number. The mass number varies. It is the sum of the protons and neutrons. ...
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.