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... inward gravitational collapse is: a. Halted by degeneracy pressure in the core. b. Halted when the atoms are pushed up against one another and contraction stops. c. Finally balanced by outward thermal pressure from nuclear reactions. d. Finally balanced by radiation emitted in the photosphere. e. no ...
... inward gravitational collapse is: a. Halted by degeneracy pressure in the core. b. Halted when the atoms are pushed up against one another and contraction stops. c. Finally balanced by outward thermal pressure from nuclear reactions. d. Finally balanced by radiation emitted in the photosphere. e. no ...
Stellar Evolution Diagram Answer Key:
... White DwarfA giant star becomes a white dwarf when the star looses its outer gases and reveals its core. A white dwarf consists primarily of Carbon and can last for 100’s of billions of years. This is the final stage of small stars. These stars still glow because they are still very hot. Black dwarf ...
... White DwarfA giant star becomes a white dwarf when the star looses its outer gases and reveals its core. A white dwarf consists primarily of Carbon and can last for 100’s of billions of years. This is the final stage of small stars. These stars still glow because they are still very hot. Black dwarf ...
starevolution - Global Change Program
... supernova remnant is 6,500 light years away. Another beautiful example of a supernova remnant is the Cygnus Loop, lying about 2,500 light years away (on right). The evolution of even more massive stars produce other objects in our universe. Perhaps the most intriguing object that can form from a mas ...
... supernova remnant is 6,500 light years away. Another beautiful example of a supernova remnant is the Cygnus Loop, lying about 2,500 light years away (on right). The evolution of even more massive stars produce other objects in our universe. Perhaps the most intriguing object that can form from a mas ...
The Life Cycles of Stars MEDIUM STARS MASSIVE STARS
... Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star's spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is taking place ...
... Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star's spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is taking place ...
Chapter20
... The best explanation for novae is surface fusion on a white dwarf. White dwarfs no longer have any hydrogen to burn in a fusion reaction. A white dwarf in a binary system ‘steals’ extra hydrogen from its companion by tidal stripping. Hydrogen gas will build up on the surface of the white dwarf where ...
... The best explanation for novae is surface fusion on a white dwarf. White dwarfs no longer have any hydrogen to burn in a fusion reaction. A white dwarf in a binary system ‘steals’ extra hydrogen from its companion by tidal stripping. Hydrogen gas will build up on the surface of the white dwarf where ...
Supernovae
... monuclear reactions and prevent the runaway process. Eventually, the temperature increases to the level where the thermal and degenerate-electron pressure components become comparable and the material begins to expand, but at that time, the expansion is unable to quench the fast thermonuclear burni ...
... monuclear reactions and prevent the runaway process. Eventually, the temperature increases to the level where the thermal and degenerate-electron pressure components become comparable and the material begins to expand, but at that time, the expansion is unable to quench the fast thermonuclear burni ...
Lecture 22 - Seattle Central
... For solar-mass stars, we stopped at Carbon. Not enough gravitational pressure to go further. ...
... For solar-mass stars, we stopped at Carbon. Not enough gravitational pressure to go further. ...
ppt document
... magnetic field and a rotation, the resulting neutron star may still have that magnetic field and it will have a much higher rotational speed due to the collapse. The magnetic field may cause light to be emitted in a beam, and with the rotation this beam may rotate at a high angular speed. We have se ...
... magnetic field and a rotation, the resulting neutron star may still have that magnetic field and it will have a much higher rotational speed due to the collapse. The magnetic field may cause light to be emitted in a beam, and with the rotation this beam may rotate at a high angular speed. We have se ...
dark matter
... material from previous generations of stars it will contain, and the higher their metallicity. Stars can be broadly split into two populations: Population I stars formed recently & contain significant quantities of the heavier elements. The Sun is a Population I star. Population II stars formed in t ...
... material from previous generations of stars it will contain, and the higher their metallicity. Stars can be broadly split into two populations: Population I stars formed recently & contain significant quantities of the heavier elements. The Sun is a Population I star. Population II stars formed in t ...
S1E4 Extreme Stars
... mass, and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon Carbon ash is deposited in core and eventually a helium-burning shell develops. This shell is itself surrounded by a shell of hydrogen undergoing nuclear fusion. For a star with M< 1 Msun, the carbon ...
... mass, and eventually becomes hot enough (100 million Kelvin) for helium to begin to fuse into carbon Carbon ash is deposited in core and eventually a helium-burning shell develops. This shell is itself surrounded by a shell of hydrogen undergoing nuclear fusion. For a star with M< 1 Msun, the carbon ...
File
... • Formation begins with condensation of a large cloud of cold gas, ice, and dust called a nebula. • The nebula contracts, breaks into fragments, and increases in temperature. • When the center of the cloud reaches 2 million degrees F (1 million K), it becomes a protostar. • When the temperature reac ...
... • Formation begins with condensation of a large cloud of cold gas, ice, and dust called a nebula. • The nebula contracts, breaks into fragments, and increases in temperature. • When the center of the cloud reaches 2 million degrees F (1 million K), it becomes a protostar. • When the temperature reac ...
Core-collapse supernovae and their massive progenitors
... are high-mass progenitors that form a blackhole, for which fall-back onto the compact object reduces the overall observed energy (Zampieri et al. 2003). The direct detection of the progenitor star of SN 2005cs (8–12 M⊙), which is a faint ...
... are high-mass progenitors that form a blackhole, for which fall-back onto the compact object reduces the overall observed energy (Zampieri et al. 2003). The direct detection of the progenitor star of SN 2005cs (8–12 M⊙), which is a faint ...
Slide 1
... The sun is only going to have enough pressure to get to the point where it fuses carbon. After it stops, the rest of the sun collapsing down just isn’t hot enough to let it do more fusion. So what happens next? This is where it gets a bit ...
... The sun is only going to have enough pressure to get to the point where it fuses carbon. After it stops, the rest of the sun collapsing down just isn’t hot enough to let it do more fusion. So what happens next? This is where it gets a bit ...
Test #4 (Ch. 13-16) ASTR 10 You have 1 hour to take the exam, and
... 25. What evidence suggests that most of the mass of the Milky Way is in the form of dark matter? A. Theoretical models of galaxy formation suggest that a galaxy cannot form unless it has at least 10 times as much matter as we see in the Milky Way disk. B. Although dark matter emits no visible light, ...
... 25. What evidence suggests that most of the mass of the Milky Way is in the form of dark matter? A. Theoretical models of galaxy formation suggest that a galaxy cannot form unless it has at least 10 times as much matter as we see in the Milky Way disk. B. Although dark matter emits no visible light, ...
ppt - Wladimir Lyra
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
iClicker Questions
... Discovering the Universe, Eighth Edition by Neil F. Comins and William J. Kaufmann III Chapter 12 12-1. Protostars are not seen in visible light telescopes because: a) they don’t emit any radiation b) they are surrounded by clouds of gas and dust * c) they only emit infrared radiation d) they are al ...
... Discovering the Universe, Eighth Edition by Neil F. Comins and William J. Kaufmann III Chapter 12 12-1. Protostars are not seen in visible light telescopes because: a) they don’t emit any radiation b) they are surrounded by clouds of gas and dust * c) they only emit infrared radiation d) they are al ...
Weighing the universe—6 Dec AST207 F2010 12/6/2010
... • A Type II supernova is a massive star that explodes when it runs out of fuel and pressure is insufficient to counter gravity. • A Type I supernova is a white dwarf that explodes. – A WD and giant orbit each other. – Mass moves from the giant to the WD. – WD explodes when it gets so much mass f ...
... • A Type II supernova is a massive star that explodes when it runs out of fuel and pressure is insufficient to counter gravity. • A Type I supernova is a white dwarf that explodes. – A WD and giant orbit each other. – Mass moves from the giant to the WD. – WD explodes when it gets so much mass f ...
Introduction - Departamento de Astronomía
... Late infall of primordial gas etc Supernova-driven galactic winds etc ...
... Late infall of primordial gas etc Supernova-driven galactic winds etc ...
Micro_lect20
... • Supernova produce all of the heavier elements – Elements up to Iron can be produced by fusion – Elements heavier than Iron are produced by the neutrons and neutrinos interacting with nuclei during the supernova explosion ...
... • Supernova produce all of the heavier elements – Elements up to Iron can be produced by fusion – Elements heavier than Iron are produced by the neutrons and neutrinos interacting with nuclei during the supernova explosion ...
the life cycle of stars
... star that is the leftover center of an old star • No hydrogen left • Can shine for billions of years before they cool completely • RED DWARF – low-mass stars • Oldest stars in the universe ...
... star that is the leftover center of an old star • No hydrogen left • Can shine for billions of years before they cool completely • RED DWARF – low-mass stars • Oldest stars in the universe ...
Answer to question 1 - Northwestern University
... (2) Brighter standard candles A. Supernovae B. Red giants, globular clusters, brightest galaxy in a cluster ...
... (2) Brighter standard candles A. Supernovae B. Red giants, globular clusters, brightest galaxy in a cluster ...
Stellar Evolution
... eventually run out of fuel and collapse due to gravity Low Mass Stars – consume fuel at a slow rate, may remain on main-sequence for up to 100 billion years, end up collapsing into white dwarfs Medium Mass Stars – go into red-giant stage, followed by collapse to white dwarf by blowing out their oute ...
... eventually run out of fuel and collapse due to gravity Low Mass Stars – consume fuel at a slow rate, may remain on main-sequence for up to 100 billion years, end up collapsing into white dwarfs Medium Mass Stars – go into red-giant stage, followed by collapse to white dwarf by blowing out their oute ...
Chapter 2 Cosmic tombstones
... field A neutron star is formed, when a massive stellar core (> 1.4 M ) collapses, because it cannot support itself against its own weight. The continuing collapse is stopped by pressure of “neutron gas” produced from protons and electrons. Collapse leaves a newly formed neutron star very hot (milli ...
... field A neutron star is formed, when a massive stellar core (> 1.4 M ) collapses, because it cannot support itself against its own weight. The continuing collapse is stopped by pressure of “neutron gas” produced from protons and electrons. Collapse leaves a newly formed neutron star very hot (milli ...
Supernova
A supernova is a stellar explosion that briefly outshines an entire galaxy, radiating as much energy as the Sun or any ordinary star is expected to emit over its entire life span, before fading from view over several weeks or months. The extremely luminous burst of radiation expels much or all of a star's material at a velocity of up to 7007300000000000000♠30,000 km/s (10% of the speed of light), driving a shock wave into the surrounding interstellar medium. This shock wave sweeps up an expanding shell of gas and dust called a supernova remnant. Supernovae are potentially strong galactic sources of gravitational waves. A great proportion of primary cosmic rays comes from supernovae.Supernovae are more energetic than novae. Nova means ""new"" in Latin, referring to what appears to be a very bright new star shining in the celestial sphere; the prefix ""super-"" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky in 1931. It is pronounced /ˌsuːpərnoʊvə/ with the plural supernovae /ˌsuːpərnoʊviː/ or supernovas (abbreviated SN, plural SNe after ""supernovae"").Supernovae can be triggered in one of two ways: by the sudden re-ignition of nuclear fusion in a degenerate star; or by the gravitational collapse of the core of a massive star. In the first case, a degenerate white dwarf may accumulate sufficient material from a companion, either through accretion or via a merger, to raise its core temperature, ignite carbon fusion, and trigger runaway nuclear fusion, completely disrupting the star. In the second case, the core of a massive star may undergo sudden gravitational collapse, releasing gravitational potential energy that can create a supernova explosion.The most recent directly observed supernova in the Milky Way was Kepler's Star of 1604 (SN 1604); remnants of two more recent supernovae have been found retrospectively. Observations in other galaxies indicate that supernovae should occur on average about three times every century in the Milky Way, and that any galactic supernova would almost certainly be observable in modern astronomical equipment. Supernovae play a significant role in enriching the interstellar medium with higher mass elements. Furthermore, the expanding shock waves from supernova explosions can trigger the formation of new stars.