File
... • The total amount of energy radiated by a supernova is equal to the amount of energy our sun will radiate during its entire 10 billion year lifetime. ...
... • The total amount of energy radiated by a supernova is equal to the amount of energy our sun will radiate during its entire 10 billion year lifetime. ...
Friday, January 27, 2017 First exam a week from today. Review
... SN 1987A - 1st of 1987 (also most important, but that is not what the “A” means). Currently discover several per day. Individual groups discover batches, give them their own names, and may or may not announce ...
... SN 1987A - 1st of 1987 (also most important, but that is not what the “A” means). Currently discover several per day. Individual groups discover batches, give them their own names, and may or may not announce ...
Hubblecast Episode 64: It All Ends with a Bang! — The incineration of
... 11. Now this is really cutting-‐edge science, and astronomers continue to study distant supernovae to better understand the expansion of the cosmos. And Hubble plays a big part in this game. It just ...
... 11. Now this is really cutting-‐edge science, and astronomers continue to study distant supernovae to better understand the expansion of the cosmos. And Hubble plays a big part in this game. It just ...
Supernova
... Supernova Remnants • The supernova core collapse is at 200 billion K. • The photons are energetic enough to break up iron nuclei. • The particles from the broken nuclei fuse with iron to create heavy elements. • This matter goes to form new ...
... Supernova Remnants • The supernova core collapse is at 200 billion K. • The photons are energetic enough to break up iron nuclei. • The particles from the broken nuclei fuse with iron to create heavy elements. • This matter goes to form new ...
supernova!
... These super-bright stars were first recognized as a special class by Fritz Zwicky, in the 1930s. (He also foresaw neutron stars and dark matter.) He was quite a character. ...
... These super-bright stars were first recognized as a special class by Fritz Zwicky, in the 1930s. (He also foresaw neutron stars and dark matter.) He was quite a character. ...
CoreCollapse13
... ejecta has increase again (starting at about 13.5 years) – sign of additional energy input ...
... ejecta has increase again (starting at about 13.5 years) – sign of additional energy input ...
Comet Pan-Starrs 12 March 2013
... Fe disintegrates into protons and neutrons Protons and electrons combine to form neutrons This takes heat out of the star Without pressure support the core collapses Gravitational potential energy is converted to heat, and the outer part of the star is ejected • The core may stabilize as a neutron ...
... Fe disintegrates into protons and neutrons Protons and electrons combine to form neutrons This takes heat out of the star Without pressure support the core collapses Gravitational potential energy is converted to heat, and the outer part of the star is ejected • The core may stabilize as a neutron ...
Type Ia Supernovae as distance indicators
... Model of a type Ia supernova. The blue surface shows deflagration; the white surface shows detonation. ...
... Model of a type Ia supernova. The blue surface shows deflagration; the white surface shows detonation. ...
Supernova’s
... • Starts off with a blue white color • Expands, cools, turns yellow • Pulsates for few months • Turns into Red Supergiant Star – 1,000 larger than our Sun ...
... • Starts off with a blue white color • Expands, cools, turns yellow • Pulsates for few months • Turns into Red Supergiant Star – 1,000 larger than our Sun ...
21_LectureOutline
... A supernova is a one-time event—once it happens, there is little or nothing left of the progenitor star. There are two different types of supernovae, both equally common: • Type I, which is a carbon-detonation supernova, and • Type II, which is the death of a high-mass star just described ...
... A supernova is a one-time event—once it happens, there is little or nothing left of the progenitor star. There are two different types of supernovae, both equally common: • Type I, which is a carbon-detonation supernova, and • Type II, which is the death of a high-mass star just described ...
Nova & SuperNova - Heart of the Valley Astronomers
... • Electron degeneracy is a stellar application of the Pauli Exclusion Principle, as is neutron degeneracy. • No two electrons can occupy identical states, even under the pressure of a collapsing star of several solar masses. • For stellar masses less than about 1.44 solar masses, the energy from the ...
... • Electron degeneracy is a stellar application of the Pauli Exclusion Principle, as is neutron degeneracy. • No two electrons can occupy identical states, even under the pressure of a collapsing star of several solar masses. • For stellar masses less than about 1.44 solar masses, the energy from the ...
SN 2004dj
... consistent with a B-type star; 2) Such an extremely blue and bright star is most likely to be a luminous blue variable, but it did not show significant light variations on a time scale of few years; 3) The high reddening would imply an unrealistic high luminosity for a SN 2004dj as a type II-P SN. ...
... consistent with a B-type star; 2) Such an extremely blue and bright star is most likely to be a luminous blue variable, but it did not show significant light variations on a time scale of few years; 3) The high reddening would imply an unrealistic high luminosity for a SN 2004dj as a type II-P SN. ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Supernovae are not alike. For decades, astronomers had known that supernovae fell into different types based on their light curves, that is, their pattern of rising and falling brightness. Later, they found these types actually corresponded to different physical circumstances triggering the explosio ...
... Supernovae are not alike. For decades, astronomers had known that supernovae fell into different types based on their light curves, that is, their pattern of rising and falling brightness. Later, they found these types actually corresponded to different physical circumstances triggering the explosio ...
astro-ph/0504597 PDF
... luminosity of SNIIP stops declining shortly after maximum forming plateau 2-3 months long. SNIIL, on the other hand, show a linear, uninterrupted luminosity decline. Indeed there is no clear spectral differences between these two types, but their progenitors do differ by the amount of H they have in ...
... luminosity of SNIIP stops declining shortly after maximum forming plateau 2-3 months long. SNIIL, on the other hand, show a linear, uninterrupted luminosity decline. Indeed there is no clear spectral differences between these two types, but their progenitors do differ by the amount of H they have in ...
Ch. 21
... A supernova is incredibly luminous, as can be seen from these curves – more than a million times as bright as a nova. ...
... A supernova is incredibly luminous, as can be seen from these curves – more than a million times as bright as a nova. ...
Stellar Explosions
... A supernova is incredibly luminous, as can be seen from these curves – more than a million times as bright as a nova. ...
... A supernova is incredibly luminous, as can be seen from these curves – more than a million times as bright as a nova. ...
The Death of Stars
... becomes much more luminous. Up to 10 billions times brighter than the Sun! • Rivals the entire galaxy in brightness for a few weeks! Fades over months to years. Two main classes: Type I: no hydrogen lines Type II: hydrogen lines visible (in spectra) Also, Type I seen in all kinds of galaxies, while ...
... becomes much more luminous. Up to 10 billions times brighter than the Sun! • Rivals the entire galaxy in brightness for a few weeks! Fades over months to years. Two main classes: Type I: no hydrogen lines Type II: hydrogen lines visible (in spectra) Also, Type I seen in all kinds of galaxies, while ...
Name - CLC Charter School
... exploding, as an effect of the large transfer of matter and energy, there is a very different kind of star left. This star is called a spinning neutron star. Neutron stars produce radio waves in a steady stream or in random bursts. But if a star is massive enough, it can leave behind something more. ...
... exploding, as an effect of the large transfer of matter and energy, there is a very different kind of star left. This star is called a spinning neutron star. Neutron stars produce radio waves in a steady stream or in random bursts. But if a star is massive enough, it can leave behind something more. ...
cassiopeia a - Chandra X
... HOW: The supernova that created Cas A is thought to have occurred when a star about 25 times as massive as the Sun ran out of fuel for nuclear power. Its core then collapsed to form an ultra-dense object called a neutron star, and the outer layers of the star were ejected at enormous speeds (see ill ...
... HOW: The supernova that created Cas A is thought to have occurred when a star about 25 times as massive as the Sun ran out of fuel for nuclear power. Its core then collapsed to form an ultra-dense object called a neutron star, and the outer layers of the star were ejected at enormous speeds (see ill ...
type II supernova
... neutrinos, whereas only 1% is converted into the kinetic and heat energy of the ejecta (i.e., outer gas layers). Yet enough light is emitted by a supernova to make it as bright as a billion Suns. The most famous historical Type II SN became visible on July 4, 1054 and was noted by astronomers in Imp ...
... neutrinos, whereas only 1% is converted into the kinetic and heat energy of the ejecta (i.e., outer gas layers). Yet enough light is emitted by a supernova to make it as bright as a billion Suns. The most famous historical Type II SN became visible on July 4, 1054 and was noted by astronomers in Imp ...
Topic 6 Introduction
... – Type II - evidence of H emission lines, sub-classification on light curves • Type II P - flat plateau part of light curve • Type II L - linear light curve ...
... – Type II - evidence of H emission lines, sub-classification on light curves • Type II P - flat plateau part of light curve • Type II L - linear light curve ...
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.