life and death of a high mass star 2
... AFTER THAT, THEY LOSE THEIR MASS AND HEAT AND BEGIN TO DIE. THIS PROCESS TAKES BILLIONS AND BILLIONS OF YEARS. ...
... AFTER THAT, THEY LOSE THEIR MASS AND HEAT AND BEGIN TO DIE. THIS PROCESS TAKES BILLIONS AND BILLIONS OF YEARS. ...
The Life of a Star
... Stars that are some 3 or more times as massive as our Sun Outer layers of the star swell into a red supergiant The core begins to yield to gravity and starts to shrink As it shrinks, it grows hotter and denser, and a new series of nuclear reactions, temporarily halting the collapse The cor ...
... Stars that are some 3 or more times as massive as our Sun Outer layers of the star swell into a red supergiant The core begins to yield to gravity and starts to shrink As it shrinks, it grows hotter and denser, and a new series of nuclear reactions, temporarily halting the collapse The cor ...
Elements from Stardust
... repel each other. • But inside stars, where matter is in the plasma state, nuclei are close enough and moving fast enough to collide with each other. ...
... repel each other. • But inside stars, where matter is in the plasma state, nuclei are close enough and moving fast enough to collide with each other. ...
Astronomy
... Learning Target: Be able to explain what causes various types of stellar explosions Question of the day: Once you have your test back, use your book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting ...
... Learning Target: Be able to explain what causes various types of stellar explosions Question of the day: Once you have your test back, use your book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting ...
radioactive decay
... Neutron-to-proton (n/p) ratio and nuclear stability. To some degree, the stability of a nucleus can be correlated with its neutron-to-proton ratio. For light atoms 1/1 ratio, for heavier atoms closer ot 1.5/1 ...
... Neutron-to-proton (n/p) ratio and nuclear stability. To some degree, the stability of a nucleus can be correlated with its neutron-to-proton ratio. For light atoms 1/1 ratio, for heavier atoms closer ot 1.5/1 ...
Star Life Cycle Poster
... Star Life Cycle Poster You need to investigate the life cycle of stars and other objects in the universe. All work must be typed. You may work alone or with a partner and turn in one assignment. 1. Give a description or definition, in YOUR OWN WORDS, for the following terms. (1 pt. each) Black hole ...
... Star Life Cycle Poster You need to investigate the life cycle of stars and other objects in the universe. All work must be typed. You may work alone or with a partner and turn in one assignment. 1. Give a description or definition, in YOUR OWN WORDS, for the following terms. (1 pt. each) Black hole ...
NUCLEAR CHEMISTRY
... gamma rays, from nuclear reactors. Control rods – neutron-absorbing rods that help control the reaction by limiting free neutrons. Moderator – used to slow down the fast neutrons produced by fission Uranium-235 is usually the fuel Coolant is simply water which can absorb neutrons to become heavy wat ...
... gamma rays, from nuclear reactors. Control rods – neutron-absorbing rods that help control the reaction by limiting free neutrons. Moderator – used to slow down the fast neutrons produced by fission Uranium-235 is usually the fuel Coolant is simply water which can absorb neutrons to become heavy wat ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Some stars end their lives in cataclysmic explosions: spectacular supernovae, which briefly become the most brilliant objects in their home galaxies, visible from millions or even billions of light-years away. Supernovae are of several distinct types, as is evident from their spectra—the graphs astr ...
... Some stars end their lives in cataclysmic explosions: spectacular supernovae, which briefly become the most brilliant objects in their home galaxies, visible from millions or even billions of light-years away. Supernovae are of several distinct types, as is evident from their spectra—the graphs astr ...
NUCLEAR CHEMISTRY REVIEW SHEET
... _____38. Which of the following are deflected LEAST by a magnetic field? a. alpha particles b. beta particles c. gamma ray d. None of the above are deflected at all _____39. Three of the statements below about nuclear fission and nuclear fusion are true. Which one is NOT true? a. Nuclear fission is ...
... _____38. Which of the following are deflected LEAST by a magnetic field? a. alpha particles b. beta particles c. gamma ray d. None of the above are deflected at all _____39. Three of the statements below about nuclear fission and nuclear fusion are true. Which one is NOT true? a. Nuclear fission is ...
![Chapter Zero Section 0.2 [reprint from Jesperson 7th] Supernovas](http://s1.studyres.com/store/data/009810478_1-e5fd9db32afbb84e749a32319c4308af-300x300.png)
Chapter Zero Section 0.2 [reprint from Jesperson 7th] Supernovas
... 1. The speeding nuclei destroy many of the iron nuclei, creating a rich mixture of smaller particles such as helium nuclei and neutrons. 2. The temperature of the collapsing star reaches levels that cannot be achieved even in the most massive stars. At its culmination, the collapsing star disintegra ...
... 1. The speeding nuclei destroy many of the iron nuclei, creating a rich mixture of smaller particles such as helium nuclei and neutrons. 2. The temperature of the collapsing star reaches levels that cannot be achieved even in the most massive stars. At its culmination, the collapsing star disintegra ...
Evolution and nucleosynthesis of extremely metal
... taken as a mix of standard Big Bang material and supernova calculations as described in Paper I. The abundances of the elements heavier than Zn were taken equal to zero, however we note that this choice is mostly irrelevant to our results because the neutron-capture nucleosynthesis overwrites the me ...
... taken as a mix of standard Big Bang material and supernova calculations as described in Paper I. The abundances of the elements heavier than Zn were taken equal to zero, however we note that this choice is mostly irrelevant to our results because the neutron-capture nucleosynthesis overwrites the me ...
Star Life Cycle Worksheet Directions: Write in the correct stages of a
... 3. Nebula can form either an _______ star that is about the size of our Sun or a _________ star which can be over three times as big as our Sun! These stars stay in this period for most of their lives and they convert hydrogen to helium while generating lots of heat and light. 4. At the end of the l ...
... 3. Nebula can form either an _______ star that is about the size of our Sun or a _________ star which can be over three times as big as our Sun! These stars stay in this period for most of their lives and they convert hydrogen to helium while generating lots of heat and light. 4. At the end of the l ...
13. H Electric Fields Questions
... 10. A beam of protons enters a region of uniform magnetic field at right angles to the field. The protons follow a circular path in the magnetic field until a potential difference is applied across the deflecting plates. The deflected protons then hit a copper target. ...
... 10. A beam of protons enters a region of uniform magnetic field at right angles to the field. The protons follow a circular path in the magnetic field until a potential difference is applied across the deflecting plates. The deflected protons then hit a copper target. ...
AS2001
... • Q2: What changes to the particle content of the expanding Universe occur at the following epochs: • Annihilation: particles and anti-particles annihilate, producing photons. Small excess of particles (~1 per 109 photons) • Baryogenesis: free quarks confined by strong force in (colourless) groups ...
... • Q2: What changes to the particle content of the expanding Universe occur at the following epochs: • Annihilation: particles and anti-particles annihilate, producing photons. Small excess of particles (~1 per 109 photons) • Baryogenesis: free quarks confined by strong force in (colourless) groups ...
Forces in stars
... and a mass of 2 million million million million million kg (about 300 000 times that of the Earth). This enormous mass means a very high gravitational pull – a person weighing 600 N on the surface of the Earth would have the colossal weight of 16400N if they stood on the 'surface' of the Sun. As muc ...
... and a mass of 2 million million million million million kg (about 300 000 times that of the Earth). This enormous mass means a very high gravitational pull – a person weighing 600 N on the surface of the Earth would have the colossal weight of 16400N if they stood on the 'surface' of the Sun. As muc ...
Stellar balancing act — dynamic equilibrium. A star spends most of
... is squeezed down, electrons develop more “uncertainty” energy depending only on the density and independent of the temperature. The electrons’ resistance to being squeezed any closer together provides pressure independent of temperature. With this pressure, a star cannot regulate its temperature. Un ...
... is squeezed down, electrons develop more “uncertainty” energy depending only on the density and independent of the temperature. The electrons’ resistance to being squeezed any closer together provides pressure independent of temperature. With this pressure, a star cannot regulate its temperature. Un ...
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.