Supernovas 10/19
... Supernova 2014j – Jan 2014 In M82 (Ursa Major). Type Ia. Closest of this type observed in modern times. 11.5 million LY away. Discovered at undergrad session Univ Coll London (SN1972 e was 11 MLY but pre “modern”) ...
... Supernova 2014j – Jan 2014 In M82 (Ursa Major). Type Ia. Closest of this type observed in modern times. 11.5 million LY away. Discovered at undergrad session Univ Coll London (SN1972 e was 11 MLY but pre “modern”) ...
The Hidden Lives of Galaxies NSTA 2001
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
Astrobiology 101
... electrons and protons are fused into neutrons. This releases lots of energy in the form of neutrinos. The core cools and contracts; the inner shells rush to fill the void. As the core reaches nuclear density it become rigid and even bounces back a little. When the onrushing material feels this bounc ...
... electrons and protons are fused into neutrons. This releases lots of energy in the form of neutrinos. The core cools and contracts; the inner shells rush to fill the void. As the core reaches nuclear density it become rigid and even bounces back a little. When the onrushing material feels this bounc ...
ES High mass star life cycle plus black holes
... Now we are going to have a little practice quiz. On Thursday we watched a video about the life cycle of a low mass star. What I would you to attempt is to draw the life cycle of a low mass star. All stars start as a nebula and this is also the ending point for many stars so this a true cycle. Protos ...
... Now we are going to have a little practice quiz. On Thursday we watched a video about the life cycle of a low mass star. What I would you to attempt is to draw the life cycle of a low mass star. All stars start as a nebula and this is also the ending point for many stars so this a true cycle. Protos ...
Evolution of Massive Stars
... stars of lower initial mass. Like lower-mass stars, high-mass stars fuse hydrogen in their cores during their main sequence lifetime. Massive stars also spend 90% of the total lifetimes as stars located on the main sequence. The main sequence is also a time sequence – more massive stars complete the ...
... stars of lower initial mass. Like lower-mass stars, high-mass stars fuse hydrogen in their cores during their main sequence lifetime. Massive stars also spend 90% of the total lifetimes as stars located on the main sequence. The main sequence is also a time sequence – more massive stars complete the ...
Astr40 HWIII(new) - Empyrean Quest Publishers
... 20. A White Dwarf cannot be more massive than A. the sun. B. 1.4 solar masses. C. Jupiter. 21. A white dwarf in a companion sitiuation may gain enough mass to get hot enough for a sudden nuclear explosion called a nova. (T or F) 22. A supernova explosion for a companion white dwarf happens when it i ...
... 20. A White Dwarf cannot be more massive than A. the sun. B. 1.4 solar masses. C. Jupiter. 21. A white dwarf in a companion sitiuation may gain enough mass to get hot enough for a sudden nuclear explosion called a nova. (T or F) 22. A supernova explosion for a companion white dwarf happens when it i ...
a thermonuclear flame has almost completed TEN SECONDS AFTER IGNITION,
... Fred Hoyle of the University of Cambridge and Willy Fowler of Caltech conceived of the explosions as giant nuclear bombs. When a sunlike star exhausts its hydrogen fuel and then its helium, it turns to its carbon and oxygen. Not only can the fusion of these elements release a titanic pulse of energy ...
... Fred Hoyle of the University of Cambridge and Willy Fowler of Caltech conceived of the explosions as giant nuclear bombs. When a sunlike star exhausts its hydrogen fuel and then its helium, it turns to its carbon and oxygen. Not only can the fusion of these elements release a titanic pulse of energy ...
Friday, April 26
... a certain amount of matter, reaching about 1.4 solar masses • Very predictable; used as a standard candle – Estimate distances to galaxies where they occur ...
... a certain amount of matter, reaching about 1.4 solar masses • Very predictable; used as a standard candle – Estimate distances to galaxies where they occur ...
Bez tytułu slajdu
... Evolution of stars depend on their mass. Those above 8 Solar masses, at the end of the life, were all the termonuclear fuel is burn into iron, first collapse, and then explode into supernova. A part of the mass is expelled and the remnants form a core of about 20 km diameter made of neutrons. The ex ...
... Evolution of stars depend on their mass. Those above 8 Solar masses, at the end of the life, were all the termonuclear fuel is burn into iron, first collapse, and then explode into supernova. A part of the mass is expelled and the remnants form a core of about 20 km diameter made of neutrons. The ex ...
Supernovae and compact objects
... another route to supernova explosions, and another energy source: thermonuclear supernovae. Thermonuclear supernovae occur when a white dwarf that is supported by degeneracy pressure has mass added to it, pushing it above the Chandresekhar mass. There are two scenarios for how this might happen. Fir ...
... another route to supernova explosions, and another energy source: thermonuclear supernovae. Thermonuclear supernovae occur when a white dwarf that is supported by degeneracy pressure has mass added to it, pushing it above the Chandresekhar mass. There are two scenarios for how this might happen. Fir ...
Life Cycles of Stars
... Nebulae • Inert core left as white dwarf • Dwarf has such tiny surface area it takes billions of years to cool • Coolest (oldest?) known: 3900 K ...
... Nebulae • Inert core left as white dwarf • Dwarf has such tiny surface area it takes billions of years to cool • Coolest (oldest?) known: 3900 K ...
SUPERNOVA EMISSION FROM GAMMA RAYS TO THE INFRARED
... Supernovae are stellar explosions that produce emission in all electromagnetic bands for many decades or centuries. Except for the first few weeks, they are powered by radioactive decays from 56Co, 57Co and 44Ti. The computation of model spectra requires computing the degradation of gamma rays a ...
... Supernovae are stellar explosions that produce emission in all electromagnetic bands for many decades or centuries. Except for the first few weeks, they are powered by radioactive decays from 56Co, 57Co and 44Ti. The computation of model spectra requires computing the degradation of gamma rays a ...
The big bang left the universe with its first atoms
... electrons and protons are fused into neutrons. This releases lots of energy in the form of neutrinos. The core cools and contracts; the inner shells rush to fill the void. As the core reaches nuclear density it become rigid and even bounces back a little. When the onrushing material feels this bounc ...
... electrons and protons are fused into neutrons. This releases lots of energy in the form of neutrinos. The core cools and contracts; the inner shells rush to fill the void. As the core reaches nuclear density it become rigid and even bounces back a little. When the onrushing material feels this bounc ...
The Life Cycle of a Star
... Lowmass stars (red dwarfs) consume hydrogen at a very slow rate (~ 100 billion years). During this time, they lose significant mass, and eventually evaporate. The result is a very faint white dwarf. ...
... Lowmass stars (red dwarfs) consume hydrogen at a very slow rate (~ 100 billion years). During this time, they lose significant mass, and eventually evaporate. The result is a very faint white dwarf. ...
Where Did All The Elements Come From??
... electrons and protons are fused into neutrons. This releases lots of energy in the form of neutrinos. The core cools and contracts; the inner shells rush to fill the void. As the core reaches nuclear density it become rigid and even bounces back a little. When the onrushing material feels this bounc ...
... electrons and protons are fused into neutrons. This releases lots of energy in the form of neutrinos. The core cools and contracts; the inner shells rush to fill the void. As the core reaches nuclear density it become rigid and even bounces back a little. When the onrushing material feels this bounc ...
Supernovae
... • Neutrinos detected consistent with number expected from supernova in LMC in Feb 1987. • Probably type II SN because originator was massive B star (20 M) • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expansion of Universe)… thus they are ve ...
... • Neutrinos detected consistent with number expected from supernova in LMC in Feb 1987. • Probably type II SN because originator was massive B star (20 M) • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expansion of Universe)… thus they are ve ...
Wednesday, April 23 - Otterbein University
... • A shock wave travels through the star and blows off the outer layers, including the heavy elements – a supernova • A million times brighter than a nova!! • The actual explosion takes less than a second ...
... • A shock wave travels through the star and blows off the outer layers, including the heavy elements – a supernova • A million times brighter than a nova!! • The actual explosion takes less than a second ...
What is a Star? - Lisle CUSD 202
... As the white dwarf cools, the light it gives off will fade through the visible light spectrum, blue to red to back (no light). A black dwarf will continue to generate gravity and low energy transmissions (radio waves). ...
... As the white dwarf cools, the light it gives off will fade through the visible light spectrum, blue to red to back (no light). A black dwarf will continue to generate gravity and low energy transmissions (radio waves). ...
White Dwarf
... • The core of a giant star collapses as helium fuses. – Outer layers continue to expand – Loses over half its mass ...
... • The core of a giant star collapses as helium fuses. – Outer layers continue to expand – Loses over half its mass ...
Astronomy
... book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting, shock waves, temperatures at various important events, what is the cause of each stage and other important pieces. Do this on a full piece of ...
... book, notes and each other to correctly describe star formation, using terms such as nuclear fusion, protostar, Ttauri star, interstellar cloud, fragmenting, shock waves, temperatures at various important events, what is the cause of each stage and other important pieces. Do this on a full piece of ...
Nuclear Nomenclature
... • The production of neutrinos and the nucleosynthesis and ejection of heavy nuclei in Type II supernovae was confirmed by SN 1987a in the Large Magellenic Cloud, a nearby galaxy, on February 23, 1987. Neutrino detectors in Ohio and Japan detected a total of about 20 neutrinos even though this supern ...
... • The production of neutrinos and the nucleosynthesis and ejection of heavy nuclei in Type II supernovae was confirmed by SN 1987a in the Large Magellenic Cloud, a nearby galaxy, on February 23, 1987. Neutrino detectors in Ohio and Japan detected a total of about 20 neutrinos even though this supern ...
life cycle of stars notes
... • Energy output down – no fusion in the core • Core begins to collapse under gravity – this makes the core hotter and denser • Hotter core causes star to expand up to 100x ...
... • Energy output down – no fusion in the core • Core begins to collapse under gravity – this makes the core hotter and denser • Hotter core causes star to expand up to 100x ...
Star Life Cycle Powerpoin
... • When a massive Red Giant fuses all of the helium into carbon, fusion stops and the outer layers collapse on the core. ...
... • When a massive Red Giant fuses all of the helium into carbon, fusion stops and the outer layers collapse on the core. ...
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.