The supernova of AD1181 – an update
... a “guest star” (kexing); this is the usual oriental term for a star-like object. Neither of the Japanese records gives any indication of the period of visibility of the star. However, the two independent records from South and North China affirm a lengthy duration. As the supernova was circumpolar, ...
... a “guest star” (kexing); this is the usual oriental term for a star-like object. Neither of the Japanese records gives any indication of the period of visibility of the star. However, the two independent records from South and North China affirm a lengthy duration. As the supernova was circumpolar, ...
Quiz 1 Review
... 13. Describe the red giant stage of a low mass star. When all of the hydrogen is fused in the core the star expands to fuse any remaining hydrogen in the outer layers…this is why the star gets so big…it turns red because as it expands the outer layers cool down. Once all of the hydrogen in the outer ...
... 13. Describe the red giant stage of a low mass star. When all of the hydrogen is fused in the core the star expands to fuse any remaining hydrogen in the outer layers…this is why the star gets so big…it turns red because as it expands the outer layers cool down. Once all of the hydrogen in the outer ...
The Origin of the Elements - Indiana University Astronomy
... Large stars also fuse hydrogen into helium, and helium into carbon But their larger masses lead to higher temperatures, which allow fusion of carbon into magnesium, etc. ...
... Large stars also fuse hydrogen into helium, and helium into carbon But their larger masses lead to higher temperatures, which allow fusion of carbon into magnesium, etc. ...
Sample Test 22
... 4. This collision between the infalling material and the rebounding core produces two effects: (a) Enough energy is produced to fuse iron into heavier elements. (b) Shock waves are sent outward that throw off the outer layers of the supergiant. These shock waves may be further heated by neutrinos es ...
... 4. This collision between the infalling material and the rebounding core produces two effects: (a) Enough energy is produced to fuse iron into heavier elements. (b) Shock waves are sent outward that throw off the outer layers of the supergiant. These shock waves may be further heated by neutrinos es ...
astronomy - Scioly.org
... - Very rare, very massive, with extremely short lifespans (first to leave main seq.) - 0.00003% of local stars are of spectral type O. - Most output is in the ultraviolet range - Main-sequence star, spectral class B, luminosity class V - Extremely luminous, short lifespans, rarely found far from are ...
... - Very rare, very massive, with extremely short lifespans (first to leave main seq.) - 0.00003% of local stars are of spectral type O. - Most output is in the ultraviolet range - Main-sequence star, spectral class B, luminosity class V - Extremely luminous, short lifespans, rarely found far from are ...
Lecture 18 Gamma-Ray Bursts
... LSGRBs are found in star-forming galaxies. Their location within those galaxies is associated with the light with a tighter correlation than even Type Iip supernovae (but maybe not Type Ic). ...
... LSGRBs are found in star-forming galaxies. Their location within those galaxies is associated with the light with a tighter correlation than even Type Iip supernovae (but maybe not Type Ic). ...
Nature paper - University of Southampton
... The correlation in Fig. 1 between Pspin and Porb among BeXs is highly significant, but the data have large scatter. Despite this scatter, however, the one-dimensional projections of the data onto the log(Porb) and log(Pspin) axes both suggest that the BeX population might be bimodal. More specifical ...
... The correlation in Fig. 1 between Pspin and Porb among BeXs is highly significant, but the data have large scatter. Despite this scatter, however, the one-dimensional projections of the data onto the log(Porb) and log(Pspin) axes both suggest that the BeX population might be bimodal. More specifical ...
Supernovae - University of Texas Astronomy Home Page
... All supernovae directly observed since 1604 (with the possible exception of Cas A), and hence all supernovae seen by modern astronomers, have been in other galaxies. Any single galaxy hosts a supernova only rarely. Supernovae occur roughly once per 100 years for spiral galaxies like the Milky Way. A ...
... All supernovae directly observed since 1604 (with the possible exception of Cas A), and hence all supernovae seen by modern astronomers, have been in other galaxies. Any single galaxy hosts a supernova only rarely. Supernovae occur roughly once per 100 years for spiral galaxies like the Milky Way. A ...
Absolute magnitude of type Ia supernovae
... last stage of a star’s evolution. Since its brightness temporarily reach to a few hundreds million times of our sun’s, we can find it from fairly far distance. It rarely occurs once in a hundred years at a galaxy, but there are many galaxies in the Universe, therefore by observing everywhere, a supe ...
... last stage of a star’s evolution. Since its brightness temporarily reach to a few hundreds million times of our sun’s, we can find it from fairly far distance. It rarely occurs once in a hundred years at a galaxy, but there are many galaxies in the Universe, therefore by observing everywhere, a supe ...
Black Hole
... It took almost eight months to fade away from the sky. It sparkled like a star in the sky. Today we know it was a `Supernova'. ...
... It took almost eight months to fade away from the sky. It sparkled like a star in the sky. Today we know it was a `Supernova'. ...
Red Supergiants as the Progenitors of Type IIP Supernova
... act as seeds of secondary Rayleigh-Taylor instabilities at the composition interfaces of the exploding star. At about 100 s dense Rayleigh-Taylor fingers containing the metals (C, O, Si, iron-group elements) have grown out of a compressed shell of matter left behind by the shock passing through the S ...
... act as seeds of secondary Rayleigh-Taylor instabilities at the composition interfaces of the exploding star. At about 100 s dense Rayleigh-Taylor fingers containing the metals (C, O, Si, iron-group elements) have grown out of a compressed shell of matter left behind by the shock passing through the S ...
The Solar System
... Supernova Neutron Star or Black Hole. • Nuclear fusion continues in shells to iron. • Unstable, collapses in <1s. Bounce off rigid core detonates star – Supernova! • Shines as bright as a galaxy for a few days! We are Stardust from Supernovae! GENS4001 Astronomy ...
... Supernova Neutron Star or Black Hole. • Nuclear fusion continues in shells to iron. • Unstable, collapses in <1s. Bounce off rigid core detonates star – Supernova! • Shines as bright as a galaxy for a few days! We are Stardust from Supernovae! GENS4001 Astronomy ...
Announcements - Lick Observatory
... • In the early 1900s `novae’ were sometimes observed in other galaxies and were used to help set the distances to galaxies. • But, when it became clear that even the nearest galaxies were much further away than anyone had thought this suggested that the extragalactic `nova’ were much brighter than G ...
... • In the early 1900s `novae’ were sometimes observed in other galaxies and were used to help set the distances to galaxies. • But, when it became clear that even the nearest galaxies were much further away than anyone had thought this suggested that the extragalactic `nova’ were much brighter than G ...
Lecture 10: Stellar Evolution
... stories of stars comes from comparing mathematical models of stars with observations • Star clusters are particularly useful because they contain stars of different mass that were born about the same time ...
... stories of stars comes from comparing mathematical models of stars with observations • Star clusters are particularly useful because they contain stars of different mass that were born about the same time ...
Name Date Life and Death of a Star 2015 1. In the main
... B. how they generate energy C. their brightness 41. A magnetar is a type of pulsar that generates energy by A. an extremely strong magnetic field B. rotation C. gravitational contraction 42. Our sun will eventually become a supernova. A. TRUE B. FALSE 43. "High mass stars" eventually become SUPERGIA ...
... B. how they generate energy C. their brightness 41. A magnetar is a type of pulsar that generates energy by A. an extremely strong magnetic field B. rotation C. gravitational contraction 42. Our sun will eventually become a supernova. A. TRUE B. FALSE 43. "High mass stars" eventually become SUPERGIA ...
AY5 Announcements
... of the Sun (as bright as a small galaxy) • Many rare elements will be manufactured in non-equilibrium reactions* ...
... of the Sun (as bright as a small galaxy) • Many rare elements will be manufactured in non-equilibrium reactions* ...
Test 3, February 7, 2007 - Brock physics
... 33. The structure of a red giant resulting from a high mass star as one goes from its core to the surface is (a) uranium, gold, iron, silicon, carbon, helium, hydrogen. (b) gold, iron, silicon, carbon, helium, hydrogen. (c) carbon, hydrogen, helium, iron. (d) iron, silicon, oxygen, carbon, helium, h ...
... 33. The structure of a red giant resulting from a high mass star as one goes from its core to the surface is (a) uranium, gold, iron, silicon, carbon, helium, hydrogen. (b) gold, iron, silicon, carbon, helium, hydrogen. (c) carbon, hydrogen, helium, iron. (d) iron, silicon, oxygen, carbon, helium, h ...
The Life Cycle of Stars Introduction Stars are huge spheres of very
... Stars are huge spheres of very hot gas that emit light and other radiation. They are formed from clouds of dust and gas, or nebulas, and go through different stages as they age. They are located various distances from Earth. We use a light-year to describe the distance from Earth to far away objects ...
... Stars are huge spheres of very hot gas that emit light and other radiation. They are formed from clouds of dust and gas, or nebulas, and go through different stages as they age. They are located various distances from Earth. We use a light-year to describe the distance from Earth to far away objects ...
Stardeath
... C. Neutron star, white dwarf, brown dwarf. D. White dwarf, brown dwarf, neutron star. 2. The outward force keeping a degenerate white dwarf star from collapsing is: A. degenerate electron "gas" pressure. B. internal pressure from heat. C. its rapid spinning. D. pressure from the outward flow of neut ...
... C. Neutron star, white dwarf, brown dwarf. D. White dwarf, brown dwarf, neutron star. 2. The outward force keeping a degenerate white dwarf star from collapsing is: A. degenerate electron "gas" pressure. B. internal pressure from heat. C. its rapid spinning. D. pressure from the outward flow of neut ...
ASTR-1020: Astronomy II Course Lecture Notes - Faculty
... 1. Supernovae are classified based primarily upon their spectra and their light curves (i.e., how brightness changes with time). We have already discussed a few different types. We now present the complete supernova classification scheme. The primary classification is based upon the appearance of hy ...
... 1. Supernovae are classified based primarily upon their spectra and their light curves (i.e., how brightness changes with time). We have already discussed a few different types. We now present the complete supernova classification scheme. The primary classification is based upon the appearance of hy ...
GRB Progenitors and their environments
... X-ray outburst lasting ~600s. • Subsequent observations classify this supernova as a type Ib. • Many models of initial X-ray outburst, most focusing on shock breakout. • Frey et al., modeling shock breakout, could match the duration/shape with binary CE ejection, but not the luminosity – is it a sho ...
... X-ray outburst lasting ~600s. • Subsequent observations classify this supernova as a type Ib. • Many models of initial X-ray outburst, most focusing on shock breakout. • Frey et al., modeling shock breakout, could match the duration/shape with binary CE ejection, but not the luminosity – is it a sho ...
Brock physics - Brock University
... (c) the radius of the region around a neutron star within which X-ray bursts occur. (d) * the radius of the region around a black hole within which not even light can escape. 35. Neutron stars with masses greater than about 3 solar masses do not exist because neutron degeneracy pressure is not stron ...
... (c) the radius of the region around a neutron star within which X-ray bursts occur. (d) * the radius of the region around a black hole within which not even light can escape. 35. Neutron stars with masses greater than about 3 solar masses do not exist because neutron degeneracy pressure is not stron ...
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.