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PP 23-The Solar System
PP 23-The Solar System

Unit 8 Chapter 30
Unit 8 Chapter 30

sc_examII_fall_2002 - University of Maryland
sc_examII_fall_2002 - University of Maryland

... A. strong radiation emitted by a supergiant star. B. a distant galaxy that has recently been born. C. coming from very hot gas in a black hole’s accretion disk. D. what’s left after a pulsar stopped pulsing. E. matter and antimatter annihilation. 2. According to Einstein’s theory of general relativi ...
Answer
Answer

... 1. If you zoom in on the peaks of the luminosity and radius graphs, you will see that there are in fact two peaks. Suggest why you think this happens. The 1st peak occurs when hydrogen fusion stops. The trough between the peaks is when Helium fusion is occurring. The 2nd peak occurs when helium fusi ...
Sun and Other Stars Notes
Sun and Other Stars Notes

... -Fusing of 2 _______________________ nuclei= tremendous release of energy and a third atom of helium, this is called the proton-proton chain -Sun fuses ________________________ of material per second, very little mass is lost in the Sun, most is just converted into another element -Why is observatio ...
Lecture 11, PPT version
Lecture 11, PPT version

c - Fsusd
c - Fsusd

... 4) The planets and moons in our solar system are visible because they ______. a) emit their own light b) undergo nuclear fusion c) absorb light from the sun d) reflect light from the sun ...
Our Universe
Our Universe

Activity: Star Classification - d
Activity: Star Classification - d

... Part 1: Exploring with Classification  Each group will receive 1 set of 27 stars.  Every star has: a color, name, temperature, size, & luminosity value o The luminosity is compared to the sun's luminosity. If a star has a luminosity value of 5, then it is 5 times brighter than our sun. If a star h ...
Spectrum a Star….. - SFA Physics and Astronomy
Spectrum a Star….. - SFA Physics and Astronomy

... These two scientists found that burning chemicals over an open flame resulted in a spectrum with bright lines. ...
Today`s Powerpoint
Today`s Powerpoint

_____ 1. Which of the following statements is NOT true about stars
_____ 1. Which of the following statements is NOT true about stars

... 11. White dwarf is the _________________ stage of an average size star’s life cycle. Massive and super massive stars will not end at this stage. WHEN STARS GET OLD: PAGE 594 - 595 ...
Properties of Stars
Properties of Stars

145KB - NZQA
145KB - NZQA

... • blue / white giant • supernova • black hole. The birth stage is explained: A very large GMC condenses under gravity to become dense. As it condenses, the particles become hotter (due to friction) and eventually become hot enough to become a protostar. Rigel birth explained with associated energy c ...
91KB - NZQA
91KB - NZQA

White Dwarfs - Indiana University
White Dwarfs - Indiana University

Astronomy Quiz 12 “Stars
Astronomy Quiz 12 “Stars

Return both exam and scantron sheet when you
Return both exam and scantron sheet when you

... (b) Fusion of hydrogen and deuterium into 3 He. (c) Fusion of two protons into deuterium with a release of a positron, a neutrino and energy. (d) [None of the above.] 52. As four protons are replaced by one nucleus of 4 He in the fusion process the core temperain order to maintain the same pressure ...
28. What causes waves - Summer Science Safari
28. What causes waves - Summer Science Safari

... apparent magnitude how bright a star appears from earth galaxy largest grouping of stars in space absolute magnitude the actual brightness of a star parallax one of the ways we measure distances in space; apparent shift in a star’s location nebulae cloud of hyrdogen gas and dust; birthplace of stars ...
Investigate Stars and Galaxies - American Museum of Natural History
Investigate Stars and Galaxies - American Museum of Natural History

... 1. Read the panel: “Formation and Evolution of Stars”. What universal force causes star formation? 2. Look at the wall panels illustrating the “Lives of Stars” and describe different-mass stars at the different stages of their development in the appropriate box: ...
A-105 Homework 1
A-105 Homework 1

Part 2 - MGNet
Part 2 - MGNet

DR 19.2 - Cobb Learning
DR 19.2 - Cobb Learning

EXAM II REVIEW - University of Maryland: Department of
EXAM II REVIEW - University of Maryland: Department of

Final Exam, Dec. 19, 2015 - Physics@Brock
Final Exam, Dec. 19, 2015 - Physics@Brock

... 4. What percentage of the known stars are the main sequence stars? (a) About 1%. (b) About 10%. (c) About 50%. (d) [None of the above.] 5. The spectroscopic parallax is a method of determining (a) a star’s chemical composition. (b) a star’s temperature. (c) a star’s distance from parallax angle. (d) ...
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Type II supernova



A Type II supernova (plural: supernovae or supernovas) results from the rapid collapse and violent explosion of a massive star. A star must have at least 8 times, and no more than 40–50 times, the mass of the Sun (M☉) for this type of explosion. It is distinguished from other types of supernovae by the presence of hydrogen in its spectrum. Type II supernovae are mainly observed in the spiral arms of galaxies and in H II regions, but not in elliptical galaxies.Stars generate energy by the nuclear fusion of elements. Unlike the Sun, massive stars possess the mass needed to fuse elements that have an atomic mass greater than hydrogen and helium, albeit at increasingly higher temperatures and pressures, causing increasingly shorter stellar life spans. The degeneracy pressure of electrons and the energy generated by these fusion reactions are sufficient to counter the force of gravity and prevent the star from collapsing, maintaining stellar equilibrium. The star fuses increasingly higher mass elements, starting with hydrogen and then helium, progressing up through the periodic table until a core of iron and nickel is produced. Fusion of iron or nickel produces no net energy output, so no further fusion can take place, leaving the nickel-iron core inert. Due to the lack of energy output allowing outward pressure, equilibrium is broken.When the mass of the inert core exceeds the Chandrasekhar limit of about 1.4 M☉, electron degeneracy alone is no longer sufficient to counter gravity and maintain stellar equilibrium. A cataclysmic implosion takes place within seconds, in which the outer core reaches an inward velocity of up to 23% of the speed of light and the inner core reaches temperatures of up to 100 billion kelvin. Neutrons and neutrinos are formed via reversed beta-decay, releasing about 1046 joules (100 foes) in a ten-second burst. The collapse is halted by neutron degeneracy, causing the implosion to rebound and bounce outward. The energy of this expanding shock wave is sufficient to accelerate the surrounding stellar material to escape velocity, forming a supernova explosion, while the shock wave and extremely high temperature and pressure briefly allow for theproduction of elements heavier than iron. Depending on initial size of the star, the remnants of the core form a neutron star or a black hole. Because of the underlying mechanism, the resulting nova is also described as a core-collapse supernova.There exist several categories of Type II supernova explosions, which are categorized based on the resulting light curve—a graph of luminosity versus time—following the explosion. Type II-L supernovae show a steady (linear) decline of the light curve following the explosion, whereas Type II-P display a period of slower decline (a plateau) in their light curve followed by a normal decay. Type Ib and Ic supernovae are a type of core-collapse supernova for a massive star that has shed its outer envelope of hydrogen and (for Type Ic) helium. As a result, they appear to be lacking in these elements.
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