When Stars Go Boom
... they don’t release energy. So, if a star gets to the point where it forms an iron core, it is in trouble. Big trouble. The huge gravitational forces in these massive stars commence to crush the core of the star in less than a second, triggering a massive explosion called a supernova. The explosions ...
... they don’t release energy. So, if a star gets to the point where it forms an iron core, it is in trouble. Big trouble. The huge gravitational forces in these massive stars commence to crush the core of the star in less than a second, triggering a massive explosion called a supernova. The explosions ...
ASTRONOMY 120
... Roughly how big (in A.U.) will the Sun become when it enters the red-giant phase? (3 points) A star like the Sun will evolve into a red giant with a size about 100 times its current size. This is equivalent to about 70 million km, or almost half an AU. 5. Chaisson Review and Discussion 20.8 Do all s ...
... Roughly how big (in A.U.) will the Sun become when it enters the red-giant phase? (3 points) A star like the Sun will evolve into a red giant with a size about 100 times its current size. This is equivalent to about 70 million km, or almost half an AU. 5. Chaisson Review and Discussion 20.8 Do all s ...
Life (Briefly) Near a Supernova
... Even the cosmically modest energy output of the Sun is still too huge to imagine, let alone that of a Sun gone supernova. So one approach to making the quantities comprehensible is to scale things down a bit. What would it take to produce the radiation flux of the sun at a distance of one kilometer? ...
... Even the cosmically modest energy output of the Sun is still too huge to imagine, let alone that of a Sun gone supernova. So one approach to making the quantities comprehensible is to scale things down a bit. What would it take to produce the radiation flux of the sun at a distance of one kilometer? ...
Review: How does a star`s mass determine its life story?
... Energy released is enough to destroy the star completely, an there is NO neutron star left behind. ...
... Energy released is enough to destroy the star completely, an there is NO neutron star left behind. ...
Powerpoint - Physics and Astronomy
... b) repeated helium fusion flashes in red giants. c) rapid collapse of a protostar into a massive O star. d) the explosion of a low-mass star. e) the birth of a massive star in a new cluster. Explanation: Sudden, rapid fusion of new fuel dumped onto a white dwarf causes the star to flare up, and for ...
... b) repeated helium fusion flashes in red giants. c) rapid collapse of a protostar into a massive O star. d) the explosion of a low-mass star. e) the birth of a massive star in a new cluster. Explanation: Sudden, rapid fusion of new fuel dumped onto a white dwarf causes the star to flare up, and for ...
evolution of low
... • Chandrasekhar (Cambridge 1930) . white dwarfs are supported by electron degeneracy pressure . white dwarfs have a maximum mass of 1.4 M¯ • most white dwarfs have a mass very close to M ∼ 0.6 M¯: MWD = 0.58 ± 0.02 M¯ • most are made of carbon and oxygen (CO white ...
... • Chandrasekhar (Cambridge 1930) . white dwarfs are supported by electron degeneracy pressure . white dwarfs have a maximum mass of 1.4 M¯ • most white dwarfs have a mass very close to M ∼ 0.6 M¯: MWD = 0.58 ± 0.02 M¯ • most are made of carbon and oxygen (CO white ...
jackie822 beanerbutt777 life cycle of a star
... http://library.thinkquest.org/3103/nonshocked/topics/blackdwarfs/images/blackdwarfimg.gif ...
... http://library.thinkquest.org/3103/nonshocked/topics/blackdwarfs/images/blackdwarfimg.gif ...
Universe of Learning Science Briefing: Our Home, the Milky Way
... The Milky Way is Full of Exoplanets! Studying exoplanets helps us to answer many of humanity’s, and NASA’s, biggest questions ...
... The Milky Way is Full of Exoplanets! Studying exoplanets helps us to answer many of humanity’s, and NASA’s, biggest questions ...
Evolution of low
... Evolution of 4Mo Stars • For stars less than 6Mo these last slides describe the evolution pretty well. There are some differences in the details that depend on the initial main-sequence mass. • For stars that start with 4Mo, it gets hot enough in the cores to (1) avoid the helium flash and (2) to ...
... Evolution of 4Mo Stars • For stars less than 6Mo these last slides describe the evolution pretty well. There are some differences in the details that depend on the initial main-sequence mass. • For stars that start with 4Mo, it gets hot enough in the cores to (1) avoid the helium flash and (2) to ...
Document
... any particle, no matter how energetic, can escape. The radius of the event horizon (proportional to the mass) is very small, only 30 kilometers for a non-spinning black hole with the mass of 10 Suns. ...
... any particle, no matter how energetic, can escape. The radius of the event horizon (proportional to the mass) is very small, only 30 kilometers for a non-spinning black hole with the mass of 10 Suns. ...
test - Scioly.org
... 40. Gas pressure and densities are much lower in giant stars than dwarfs. a. True b. False 41. When a star is in free-fall collapse, it is a protostar. a. True b. False 42. A star becomes a main sequence star when it is obtaining all its radiated energy from nuclear fusion of hydrogen to oxygen. a. ...
... 40. Gas pressure and densities are much lower in giant stars than dwarfs. a. True b. False 41. When a star is in free-fall collapse, it is a protostar. a. True b. False 42. A star becomes a main sequence star when it is obtaining all its radiated energy from nuclear fusion of hydrogen to oxygen. a. ...
RED GIANTS
... • As the protostar heats up, enough thermal energy is radiated away from surface to allow collapse to continue. – energy is transported to surface first via convection – as core gets even hotter, transport via radiation takes over ...
... • As the protostar heats up, enough thermal energy is radiated away from surface to allow collapse to continue. – energy is transported to surface first via convection – as core gets even hotter, transport via radiation takes over ...
Astronomy 110 Announcements: Life and Death of a Low Mass Star
... • Continuing contraction of core leads to greater & greater luminosity, however, it never gets hot enough to fuse carbon • Star collapses to a dense, small, hot object: white dwarf ...
... • Continuing contraction of core leads to greater & greater luminosity, however, it never gets hot enough to fuse carbon • Star collapses to a dense, small, hot object: white dwarf ...
Expected Coalescence Rates of NS/NS Binaries for Ground Based
... NS : fraction of massive binaries that remain bounded after the second supernova P( ): probability for a newly formed NS/NS to coalesce in a timescale 0 : minimum coalescence time * : mean timescale required for the newly formed massive system to evolve into two NSs ...
... NS : fraction of massive binaries that remain bounded after the second supernova P( ): probability for a newly formed NS/NS to coalesce in a timescale 0 : minimum coalescence time * : mean timescale required for the newly formed massive system to evolve into two NSs ...
JimH This is Your Life - The Atlanta Astronomy Club
... •Diameter- 10 km in diameter •3> Mass > 1.4 times that of our Sun. •One teaspoonful would weigh a billion tons! ...
... •Diameter- 10 km in diameter •3> Mass > 1.4 times that of our Sun. •One teaspoonful would weigh a billion tons! ...
Progenitors and Hydrodynamics of Type II and lb Supernovae
... increasing pr3) must decelerate. One place where pr3 increases dramatically is at the interface between the helium core and the hydrogen envelope (Fig. 7), This increase is largely responsible for the formation of the "reverse shock" that gives rise to the RT instability referenced above (Bethe 1990 ...
... increasing pr3) must decelerate. One place where pr3 increases dramatically is at the interface between the helium core and the hydrogen envelope (Fig. 7), This increase is largely responsible for the formation of the "reverse shock" that gives rise to the RT instability referenced above (Bethe 1990 ...
Common Stages 7 to 9
... While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
... While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
Lecture19
... White dwarfs are supported by electron degeneracy pressure, which is why they don’t contract and burn their core material. They have no fusion going on; they cool and fade away. Usually made of carbon, but sometimes helium (very low mass stars can’t even burn helium). ...
... White dwarfs are supported by electron degeneracy pressure, which is why they don’t contract and burn their core material. They have no fusion going on; they cool and fade away. Usually made of carbon, but sometimes helium (very low mass stars can’t even burn helium). ...
PowerPoint Presentation - Center for Gravitational Wave Physics
... Assume that the Ia rate tracks the stellar mass and star formation rate as measured by Mannucci et al., then measure the constants from local galaxies to get (Scannapieco & L.B. ‘05) ...
... Assume that the Ia rate tracks the stellar mass and star formation rate as measured by Mannucci et al., then measure the constants from local galaxies to get (Scannapieco & L.B. ‘05) ...
Stars: from Adolescence to Old Age
... Shell burning starts •outer layers of star expand •core continues to contract ...
... Shell burning starts •outer layers of star expand •core continues to contract ...
Stars: from Adolescence to Old Age
... terms of star lifetimes!) create conditions where the pressure and gravity are out of sync and the pulsations continue for a time • Larger, more luminous stars will pulsate with longer periods than the smaller, fainter stars – because gravity takes longer to pull the more extended outer layers of th ...
... terms of star lifetimes!) create conditions where the pressure and gravity are out of sync and the pulsations continue for a time • Larger, more luminous stars will pulsate with longer periods than the smaller, fainter stars – because gravity takes longer to pull the more extended outer layers of th ...
8.4 White Dwarfs
... star does not necessarily have to be aligned with the rotation axis (like the Earth), they can be inclined from each other as shown below. The rotating neutron star has two sources of radiation: 1) non-thermal synchrotron radiation emitted from particles trapped in the magnetic field of the neutron ...
... star does not necessarily have to be aligned with the rotation axis (like the Earth), they can be inclined from each other as shown below. The rotating neutron star has two sources of radiation: 1) non-thermal synchrotron radiation emitted from particles trapped in the magnetic field of the neutron ...
Evolution of High Mass Stars
... Massive stars will have very different evolutionary endpoints (remnants: neutron star or black hole vs white dwarf) ...
... Massive stars will have very different evolutionary endpoints (remnants: neutron star or black hole vs white dwarf) ...
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.