PowerPoint - Chandra X
... the explosion of a massive star in the Large Magellanic Cloud, a small galaxy about 160,000 light years from Earth. The colors in this image show low energy X-rays (red), intermediate energy X-rays (green) and high energy X-rays (blue). ...
... the explosion of a massive star in the Large Magellanic Cloud, a small galaxy about 160,000 light years from Earth. The colors in this image show low energy X-rays (red), intermediate energy X-rays (green) and high energy X-rays (blue). ...
Chapter20
... 13. Observations have identified faint, distant galaxies at the locations of a number of gammaray bursts. 14. Both gamma ray bursts and supernovae are thought to occur when the core of a massive star collapses. 15. Most of the energy is released in the form of neutrinos. 16. The bright radio emissio ...
... 13. Observations have identified faint, distant galaxies at the locations of a number of gammaray bursts. 14. Both gamma ray bursts and supernovae are thought to occur when the core of a massive star collapses. 15. Most of the energy is released in the form of neutrinos. 16. The bright radio emissio ...
![Star Cycle [Recovered]](http://s1.studyres.com/store/data/008086481_1-2d8d14aa9163345f6c20c4baab23c80a-300x300.png)
Star Cycle [Recovered]
... explosion A ___________________ is an _________________ that marks the end of a very massive star’s life. When it occurs, the exploding star can outshine all of the other stars in the galaxy in total for several days and may leave behind only a crushed core. ...
... explosion A ___________________ is an _________________ that marks the end of a very massive star’s life. When it occurs, the exploding star can outshine all of the other stars in the galaxy in total for several days and may leave behind only a crushed core. ...
6.2 - Hockerill Students
... get the diagram shown here Can you see that the stable nuclides of the lighter elements have approximately equal numbers of protons and neutrons? However, as Z increases the `stability line' curves upwards. Heavier nuclei need more and more neutrons to be stable. Can we explain why? ...
... get the diagram shown here Can you see that the stable nuclides of the lighter elements have approximately equal numbers of protons and neutrons? However, as Z increases the `stability line' curves upwards. Heavier nuclei need more and more neutrons to be stable. Can we explain why? ...
Characteristics of Stars
... Copy this down to your notebook. Leave enough space for notes in square Distance ...
... Copy this down to your notebook. Leave enough space for notes in square Distance ...
PP and CNO-Cycle Nucleosynthesis
... K. This is consistent with the observed (and theoretical) core temperature of the sun. Another factor that may affect barrier penetration is electron screening, which is intuitively conceptualized as a ‘decrease’ in Coulombic repulsion due to the background ‘sea’ of electrons present in high-tempera ...
... K. This is consistent with the observed (and theoretical) core temperature of the sun. Another factor that may affect barrier penetration is electron screening, which is intuitively conceptualized as a ‘decrease’ in Coulombic repulsion due to the background ‘sea’ of electrons present in high-tempera ...
Booklet 5 – Stellar Processes and Evolution
... 5.3 Evolution All stars, irrespective of their initial mass, spend the majority of their life consuming hydrogen. This period, which can last tens of billions of years, is the most stable time in the stellar lifecycle. The lifetime of a star depends largely on its mass. Somewhat counter intuitively ...
... 5.3 Evolution All stars, irrespective of their initial mass, spend the majority of their life consuming hydrogen. This period, which can last tens of billions of years, is the most stable time in the stellar lifecycle. The lifetime of a star depends largely on its mass. Somewhat counter intuitively ...
12. Nuclear Reactions in Nature
... percentage by mass of the earth's crust and as a percentage by mass of our solar system. Notice that the scale is logarithmic and the data spans almost eleven orders of magnitude. The earth is ...
... percentage by mass of the earth's crust and as a percentage by mass of our solar system. Notice that the scale is logarithmic and the data spans almost eleven orders of magnitude. The earth is ...
42 SCIENTIFIC AMERICAN OCTOBER 2006 TEN
... reaches the density of an atomic nucleus. Like a crystal vase falling onto a concrete floor, the collapsing material releases enough gravitational potential energy to blow the rest of the star apart. An alternative emerged in 1960, when Fred Hoyle of the University of Cambridge and Willy Fowler of C ...
... reaches the density of an atomic nucleus. Like a crystal vase falling onto a concrete floor, the collapsing material releases enough gravitational potential energy to blow the rest of the star apart. An alternative emerged in 1960, when Fred Hoyle of the University of Cambridge and Willy Fowler of C ...
Supernova - Mid-Pacific Institute
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
... A white dwarf cannot be more massive than about 1.4 solar masses and remain stable. if the white dwarf's companion star expands to become a red giant, some of its matter may be drawn away and sucked onto the surface of the white dwarf. ...
Stellar Evolution
... After the red giant phase, massive stars contract again allowing the core to become hot enough to fuse elements into iron. When this occurs the star’s mass is so immense, it can no longer support it causing a sudden, violent, collapse. At this moment, the entire outer portion of the star is blown of ...
... After the red giant phase, massive stars contract again allowing the core to become hot enough to fuse elements into iron. When this occurs the star’s mass is so immense, it can no longer support it causing a sudden, violent, collapse. At this moment, the entire outer portion of the star is blown of ...
Slide 1
... Explanation: Microquasars, bizarre binary star systems generating high-energy radiation and blasting out jets of particles at nearly the speed of light, live in our Milky Way galaxy. The energetic microquasar systems seem to consist of a very compact object, either a neutron star or a black hole, f ...
... Explanation: Microquasars, bizarre binary star systems generating high-energy radiation and blasting out jets of particles at nearly the speed of light, live in our Milky Way galaxy. The energetic microquasar systems seem to consist of a very compact object, either a neutron star or a black hole, f ...
Note
... How to Make Heavy Metals: neutron-capture processes Main s-process •Low mass stars r-process •Double shell burning – High neutron flux – Type II Supernovae (massive •Makes SrYZr, Ba, etc. stars) – No time for b-decay – Eu, Gd, Dy, some Sr, Y, Zr, Ba, La… ...
... How to Make Heavy Metals: neutron-capture processes Main s-process •Low mass stars r-process •Double shell burning – High neutron flux – Type II Supernovae (massive •Makes SrYZr, Ba, etc. stars) – No time for b-decay – Eu, Gd, Dy, some Sr, Y, Zr, Ba, La… ...
ppt-nuclear - SandersScienceStuff
... has had. You can then divide your original mass of sample by 2 as many times as you have half lives. • If you are trying to solve for the half life of your sample, take the remaining mass and count how many times you have to multiple it by 2 to get your original mass. That will tell you how many hal ...
... has had. You can then divide your original mass of sample by 2 as many times as you have half lives. • If you are trying to solve for the half life of your sample, take the remaining mass and count how many times you have to multiple it by 2 to get your original mass. That will tell you how many hal ...
The Evolutionary Cycle of Stars
... White Dwarf The final evolutionary state whose mass is not too high. This is the last stage of stellar evolution. ...
... White Dwarf The final evolutionary state whose mass is not too high. This is the last stage of stellar evolution. ...
Parallax
... layers to expand and cool Star becomes a giant Helium nuclei fuse to form a core of Carbon ...
... layers to expand and cool Star becomes a giant Helium nuclei fuse to form a core of Carbon ...
Stars - Red, Blue, Old, New pt.4
... until just a few meters of the outer part-that’s normal matter, so the white dwarf does radiate according to its surface temp • 70,000-5000 K ...
... until just a few meters of the outer part-that’s normal matter, so the white dwarf does radiate according to its surface temp • 70,000-5000 K ...
Chapter 7 Worksheet
... Why is the release of neutrons, kypton-92 and barium-141 in the induced uranium-235 reactions important? C The release of neutrons in the uranium-235 reaction is important because the neutrons trigger more fission reactions to occur. Each reaction produces 3 neutrons which can cause three additional ...
... Why is the release of neutrons, kypton-92 and barium-141 in the induced uranium-235 reactions important? C The release of neutrons in the uranium-235 reaction is important because the neutrons trigger more fission reactions to occur. Each reaction produces 3 neutrons which can cause three additional ...
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.