Space Test: Practice Questions and Answers 1. Who discovered
... It begins to fuse helium to form heavier elements like carbon and oxygen. 23. What is the first stage of a star after a nebula? A protostar is the first stage after a nebula. In a protostar ...
... It begins to fuse helium to form heavier elements like carbon and oxygen. 23. What is the first stage of a star after a nebula? A protostar is the first stage after a nebula. In a protostar ...
Can We Make A Star?
... • They are made of cosmic dust, mostly hydrogen and helium • They are very unstable • The are very violent • They give off an extremely large amount of energy ...
... • They are made of cosmic dust, mostly hydrogen and helium • They are very unstable • The are very violent • They give off an extremely large amount of energy ...
Due Date: Thursday, November 16, 2006
... If the Sun had been born as a high-mass star some 4.6 billion years ago, rather than as a low mass star, the planet Jupiter would probably have Earth-like conditions today, while earth would be hot like Venus. If the Sun was formed as a high-mass star 4.6 billion years ago, then the Sun would have e ...
... If the Sun had been born as a high-mass star some 4.6 billion years ago, rather than as a low mass star, the planet Jupiter would probably have Earth-like conditions today, while earth would be hot like Venus. If the Sun was formed as a high-mass star 4.6 billion years ago, then the Sun would have e ...
1 - Pitt County Schools
... What can astronomers learn by studying a star’s color? ___________________________________________________________________________ ___________________________________________________________________________ 2. How does distance affect parallax? _______________________________________________________ ...
... What can astronomers learn by studying a star’s color? ___________________________________________________________________________ ___________________________________________________________________________ 2. How does distance affect parallax? _______________________________________________________ ...
Nebular Theory worksheet 2017
... further proposed that our solar system was once a star surrounded by a dust cloud. It is currently theorized that our solar system (and others like it) formed from a collapsing nebula. A nebula is a swirling collection of gases (mostly hydrogen and helium) and dust particles (solid matter in the for ...
... further proposed that our solar system was once a star surrounded by a dust cloud. It is currently theorized that our solar system (and others like it) formed from a collapsing nebula. A nebula is a swirling collection of gases (mostly hydrogen and helium) and dust particles (solid matter in the for ...
Quiz Questions
... B. a shell of gases ejected after the helium fusion stage in lower mass stars C. the formation stages of planets around other stars than the Sun D. the cloud of gas produced by a supernova explosion 7. Which physical phenomenon keeps a white dwarf star from collapsing inwards upon itself? A. normal ...
... B. a shell of gases ejected after the helium fusion stage in lower mass stars C. the formation stages of planets around other stars than the Sun D. the cloud of gas produced by a supernova explosion 7. Which physical phenomenon keeps a white dwarf star from collapsing inwards upon itself? A. normal ...
File
... 22) What is a galaxy? 23) What are the three classifications of galaxies? What do each look like? Which is most common? 24) What shape is the Milky Way? 25) What is the local group? 26) How many stars are in the Milky Way? 27) Approximately how big is the Milky Way 28) The largest known galaxy is wh ...
... 22) What is a galaxy? 23) What are the three classifications of galaxies? What do each look like? Which is most common? 24) What shape is the Milky Way? 25) What is the local group? 26) How many stars are in the Milky Way? 27) Approximately how big is the Milky Way 28) The largest known galaxy is wh ...
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.