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... 22. Massive stars cannot generate energy through iron fusion because a. iron fusion requires very high density. b. stars contain very little iron. c. no star can get hot enough for iron fusion. d. iron is the most tightly bound of all nuclei. e. massive stars supernova before they create an iron cor ...
... 22. Massive stars cannot generate energy through iron fusion because a. iron fusion requires very high density. b. stars contain very little iron. c. no star can get hot enough for iron fusion. d. iron is the most tightly bound of all nuclei. e. massive stars supernova before they create an iron cor ...
Here
... protons) combine to form 1 helium nucleus (which has two protons and two neutrons). • The details are a bit complex: In the Sun, 6 hydrogen nuclei are involved in a sequence that produces two hydrogen nuclei and one helium nucleus. This is the proton-proton chain. In more massive stars, a carbon ...
... protons) combine to form 1 helium nucleus (which has two protons and two neutrons). • The details are a bit complex: In the Sun, 6 hydrogen nuclei are involved in a sequence that produces two hydrogen nuclei and one helium nucleus. This is the proton-proton chain. In more massive stars, a carbon ...
Presentation available here - Lunar and Planetary Institute
... All core collapse explosions are asymmetric, maybe produced by magnetic jets. How can this be proved? Gamma-ray bursts are caused by jets of material moving at nearly the speed of light. Do they mark the birth of black holes? At least some gamma-ray bursts (and maybe all) arise in supernova ex ...
... All core collapse explosions are asymmetric, maybe produced by magnetic jets. How can this be proved? Gamma-ray bursts are caused by jets of material moving at nearly the speed of light. Do they mark the birth of black holes? At least some gamma-ray bursts (and maybe all) arise in supernova ex ...
The life of a Star (pages 468-471)
... 2. Explain how a nebula turns into a cloud leading to a star (3 steps)? 3. What happens when a star runs out of the fuels needed to produce energy? 4. What is a supernova? During this stage, what happens to the core of the star? When our Sun eventually swells into a red giant star, its outer layer ...
... 2. Explain how a nebula turns into a cloud leading to a star (3 steps)? 3. What happens when a star runs out of the fuels needed to produce energy? 4. What is a supernova? During this stage, what happens to the core of the star? When our Sun eventually swells into a red giant star, its outer layer ...
Announcements
... As the temperature decreased only electrons were left The heavier muon and tau particles stopped being created because there wasn’t enough energy density to produce them ...
... As the temperature decreased only electrons were left The heavier muon and tau particles stopped being created because there wasn’t enough energy density to produce them ...
Unit 5 - Stars
... For each helium atom created, place one bead next to it Continue this until all your Hydrogen supply is gone Write down how many Helium atoms there are Leave the 7 beads in the Helium quadrant. At this point 5 beads (energy) have been created in your Helium section. These are released in the form of ...
... For each helium atom created, place one bead next to it Continue this until all your Hydrogen supply is gone Write down how many Helium atoms there are Leave the 7 beads in the Helium quadrant. At this point 5 beads (energy) have been created in your Helium section. These are released in the form of ...
Star Types - University of Massachusetts Amherst
... Stars process Hydrogen and Helium into heavier elements (elements lighter than iron) during the nnuclear-burning phase of their lives. Elements heavier than iron are generated only in the deaths of high mass stars (supernovae). We were all once fuel for a stellar furnace. Parts of us were formed in ...
... Stars process Hydrogen and Helium into heavier elements (elements lighter than iron) during the nnuclear-burning phase of their lives. Elements heavier than iron are generated only in the deaths of high mass stars (supernovae). We were all once fuel for a stellar furnace. Parts of us were formed in ...
FINAL EXAM Name: ASTRONOMY II - 79202 Spring 1995
... Low metal abundances inhibit helium burning. High metal abundances accelerate helium burning. High metal abundances accelerate carbon burning. None of the above. ...
... Low metal abundances inhibit helium burning. High metal abundances accelerate helium burning. High metal abundances accelerate carbon burning. None of the above. ...
File - Mr. Catt`s Class
... 1. A binary system of a white dwarf and a newly formed red giant will result in the formation of an accretion disk around the white dwarf. The material in the disk comes from the red giant and is mostly hydrogen. 2. An accretion disk is a rotating disk of gas orbiting a star, formed by material fall ...
... 1. A binary system of a white dwarf and a newly formed red giant will result in the formation of an accretion disk around the white dwarf. The material in the disk comes from the red giant and is mostly hydrogen. 2. An accretion disk is a rotating disk of gas orbiting a star, formed by material fall ...
Chapter 10 The Deaths of Stars
... • The length of an object (as observed from “rest”) decreases in the direction of its motion as its speed increases. Length contraction • Clocks that you see as moving run more slowly than do clocks at rest. Biological processes slow down. Time dilation • Space and time cannot be considered as two s ...
... • The length of an object (as observed from “rest”) decreases in the direction of its motion as its speed increases. Length contraction • Clocks that you see as moving run more slowly than do clocks at rest. Biological processes slow down. Time dilation • Space and time cannot be considered as two s ...
Forging the elements
... As a cluster ages the ‘turn-off’ point moves further down the Main Sequence. This can be used to determine the age of a stellar cluster. ...
... As a cluster ages the ‘turn-off’ point moves further down the Main Sequence. This can be used to determine the age of a stellar cluster. ...
Chapter 10 The Bizarre Stellar Graveyard
... • What is a black hole? – A black hole is a massive object whose radius is so small that the escape velocity exceeds the speed of light. ...
... • What is a black hole? – A black hole is a massive object whose radius is so small that the escape velocity exceeds the speed of light. ...
A05715 ANY CALCULATOR Page 1 TURN OVER School of Physics
... Full marks for this Section may be obtained by correctly answering four questions. You may attempt more questions, but marks in excess of 40% will be disregarded. Section 2 consists of three questions and carries 60% of the marks. Answer two questions from this Section. If you answer more than two q ...
... Full marks for this Section may be obtained by correctly answering four questions. You may attempt more questions, but marks in excess of 40% will be disregarded. Section 2 consists of three questions and carries 60% of the marks. Answer two questions from this Section. If you answer more than two q ...
answers2008_09_BC
... but during supernova explosion there are lots of neutrons – add neutrons quickly (r-process) to produce neutron-rich unstable isotopes which then β-decay to stable nuclei stars which supernova also produce heavy elements through fusion (e.g. Si, S, Fe) and by high-temperature reactions during th ...
... but during supernova explosion there are lots of neutrons – add neutrons quickly (r-process) to produce neutron-rich unstable isotopes which then β-decay to stable nuclei stars which supernova also produce heavy elements through fusion (e.g. Si, S, Fe) and by high-temperature reactions during th ...
Powerpoint
... energy released during fusion) bounce around bumping into atoms and nuclei for 30,000-1,000,000* years until they finally ...
... energy released during fusion) bounce around bumping into atoms and nuclei for 30,000-1,000,000* years until they finally ...
Dark Matter: What is it?
... Neutrinos, they are very small. They have no charge and have no mass And do not interact at all. The earth is just a silly ball To them, through which they simply pass, Like dustmaids down a drafty hall Or photons through a pane of glass. ...
... Neutrinos, they are very small. They have no charge and have no mass And do not interact at all. The earth is just a silly ball To them, through which they simply pass, Like dustmaids down a drafty hall Or photons through a pane of glass. ...
answers2004_05_BC - Particle Physics and Particle Astrophysics
... of any electrostatic repulsion. If neutrons are rare and therefore are added to nuclei slowly, any unstable nucleus formed will decay before another neutron hits it. This s-process produces nuclei close to the line of maximum stability. In supernovae, neutrons can be added to nuclei very rapidly (r- ...
... of any electrostatic repulsion. If neutrons are rare and therefore are added to nuclei slowly, any unstable nucleus formed will decay before another neutron hits it. This s-process produces nuclei close to the line of maximum stability. In supernovae, neutrons can be added to nuclei very rapidly (r- ...
Test 3, February 7, 2007 - Brock physics
... 45. Harlow Shapley concluded that the Sun was not in the centre of the Milky Way Gal axy by (a) looking at the shape of the “milky band” across the sky. (b) mapping the distribution of stars in the galaxy. (c) mapping the distribution of gas clouds in the spiral arms. (d) mapping the distribution of ...
... 45. Harlow Shapley concluded that the Sun was not in the centre of the Milky Way Gal axy by (a) looking at the shape of the “milky band” across the sky. (b) mapping the distribution of stars in the galaxy. (c) mapping the distribution of gas clouds in the spiral arms. (d) mapping the distribution of ...
Measurement of the 52Fe mass via the precise proton
... help us judge the importance of each possible nuclear synthesis path. 52Fe is one of the nuclei at the N = Z line of which the precise masses can offer a sensitive test for the exchange symmetry between neutrons and protons in f p-shell [1, 2]. 52Fe is also very important in the study of astrophysica ...
... help us judge the importance of each possible nuclear synthesis path. 52Fe is one of the nuclei at the N = Z line of which the precise masses can offer a sensitive test for the exchange symmetry between neutrons and protons in f p-shell [1, 2]. 52Fe is also very important in the study of astrophysica ...
The correct answers are written in bold, italic and underlined. The
... The metal bar has no internal energy source and its "luminosity" and temperature are falling steadily. 13. What is the Chandrasekhar limit? • The maximum mass that a star can have on the main sequence without eventually exploding as a supernova • The minimum mass that a star can have to produce heli ...
... The metal bar has no internal energy source and its "luminosity" and temperature are falling steadily. 13. What is the Chandrasekhar limit? • The maximum mass that a star can have on the main sequence without eventually exploding as a supernova • The minimum mass that a star can have to produce heli ...
Life Cycle of a Star - Intervention Worksheet
... become later in its life; typically have the same ...
... become later in its life; typically have the same ...
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.