Lund Observatory Department of Astronomy and Theoretical Physics
... Department of Astronomy and Theoretical Physics LUND ...
... Department of Astronomy and Theoretical Physics LUND ...
Life Cycles of Stars
... megatons/second • Let’s relate that to human scales. What would that be at one kilometer distance? • 77 x 1015 tons/(150 x 106km)2 = 3 tons • Picture a truckload of explosives a km away giving off a one-second burst of heat and light to rival the Sun ...
... megatons/second • Let’s relate that to human scales. What would that be at one kilometer distance? • 77 x 1015 tons/(150 x 106km)2 = 3 tons • Picture a truckload of explosives a km away giving off a one-second burst of heat and light to rival the Sun ...
White dwarfs - University of Toronto
... dwarf surpasses the Chandrasekhar limit and undergoes core collapse. Since the white dwarf existed before the explosion, this can only happen in a binary system. When the companion star reaches the red giant stage, material from its outer layers accretes onto the white dwarf, increasing the WD’s mas ...
... dwarf surpasses the Chandrasekhar limit and undergoes core collapse. Since the white dwarf existed before the explosion, this can only happen in a binary system. When the companion star reaches the red giant stage, material from its outer layers accretes onto the white dwarf, increasing the WD’s mas ...
26.Meikle.Supernova_2002hh
... until the supernova has expanded sufficiently - this usually means waiting until it is at least 6 months old. Unfortunately, most supernovae are too far away so that by this time they are too faint to observe in detail. That is why the close proximity of SN 2002hh makes it such an important supernov ...
... until the supernova has expanded sufficiently - this usually means waiting until it is at least 6 months old. Unfortunately, most supernovae are too far away so that by this time they are too faint to observe in detail. That is why the close proximity of SN 2002hh makes it such an important supernov ...
Supernova: Five Stages in the Death of a Star
... After hitting the surface at 50 million km/h the shock blows the star apart. The core turns into a neutron star, a compact atomic nucleus with the mass of the Sun but 10 km in size. ...
... After hitting the surface at 50 million km/h the shock blows the star apart. The core turns into a neutron star, a compact atomic nucleus with the mass of the Sun but 10 km in size. ...
Endpoints of Stellar Evolution
... thus confirming our basic model for core-collapse SNe: > 99% of the total SN energy emerges in neutrinos! ...
... thus confirming our basic model for core-collapse SNe: > 99% of the total SN energy emerges in neutrinos! ...
l13
... All types of SNe apart from Type Ia are not observed in old stellar populations (such as elliptical galaxies). In particular Type II are observed mostly in the gas and dust rich arms of spiral galaxies. Star formation is ongoing and young stars are abundant. By contrast Type Ia SNe are found in all ...
... All types of SNe apart from Type Ia are not observed in old stellar populations (such as elliptical galaxies). In particular Type II are observed mostly in the gas and dust rich arms of spiral galaxies. Star formation is ongoing and young stars are abundant. By contrast Type Ia SNe are found in all ...
The Emerging Theory of Supernova Explosions
... Adam Burrows Princeton University Princeton NJ, USA ...
... Adam Burrows Princeton University Princeton NJ, USA ...
Stellar Evolution
... A very massive (> 8 Msun) star is building up elements through nuclear fusion up to which element(s)? ...
... A very massive (> 8 Msun) star is building up elements through nuclear fusion up to which element(s)? ...
Slide 1
... which occur for a single massive star and those which occur because of mass transfer onto a white dwarf in a binary system • Difference between the two types lies only in what gets the process started toward the explosion ...
... which occur for a single massive star and those which occur because of mass transfer onto a white dwarf in a binary system • Difference between the two types lies only in what gets the process started toward the explosion ...
The Evolution of Massive Stars
... Neutron Stars: a brief history • Basic physics understood in the 1930s • At that time, no known counterparts • In the 1950s and 1960s, more and more strange objects found, but where were the neutrons stars, or did they even exist? • The case of the Crab Nebula (supernova of 1054 AD) ...
... Neutron Stars: a brief history • Basic physics understood in the 1930s • At that time, no known counterparts • In the 1950s and 1960s, more and more strange objects found, but where were the neutrons stars, or did they even exist? • The case of the Crab Nebula (supernova of 1054 AD) ...
Supernovae, Neutron Stars, Black Holes
... Triggering the Formation of the Solar System --- New data from meteorites indicates that formation of the Solar System was triggered by a supernova. Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology One of the most amazing discoveries in space science is the unambiguous ev ...
... Triggering the Formation of the Solar System --- New data from meteorites indicates that formation of the Solar System was triggered by a supernova. Written by G. Jeffrey Taylor Hawai'i Institute of Geophysics and Planetology One of the most amazing discoveries in space science is the unambiguous ev ...
Supernova worksheet ()
... In any case, the Milky Way galaxy contains about 100 billion (1011) stars. Some are much more luminous than the Sun, and many are less luminous, but an acceptable approximation is that the average luminosity per star is 1 LSun . Therefore, the Milky Way has an approximate luminosity of 1011 * 1026 J ...
... In any case, the Milky Way galaxy contains about 100 billion (1011) stars. Some are much more luminous than the Sun, and many are less luminous, but an acceptable approximation is that the average luminosity per star is 1 LSun . Therefore, the Milky Way has an approximate luminosity of 1011 * 1026 J ...
Focus Week: Messengers of Supernova Explosions
... Texas A&M, Keiichi Maeda/IPMU). Recent developments in observational methods have led to the discovery of new types of supernovae, which are either extremely bright or faint (Peter ...
... Texas A&M, Keiichi Maeda/IPMU). Recent developments in observational methods have led to the discovery of new types of supernovae, which are either extremely bright or faint (Peter ...
Astronomy Learning Objectives and Study Questions for Chapter 13
... 5. As a massive star’s degenerate iron core collapses to nuclear density, core bounce creates a shock wave that blows the outer layers of the star apart as a _____. A. magnetar B. nova C. planetary nebula D. Type Ia supernova E. Type II supernova 6. When stars with initial masses between 8 and 25 M ...
... 5. As a massive star’s degenerate iron core collapses to nuclear density, core bounce creates a shock wave that blows the outer layers of the star apart as a _____. A. magnetar B. nova C. planetary nebula D. Type Ia supernova E. Type II supernova 6. When stars with initial masses between 8 and 25 M ...
Document
... • A neutron star spins very rapidly about its axis, due to conservation of angular momentum. • If the neutron star has a magnetic field, this field can form jets of ...
... • A neutron star spins very rapidly about its axis, due to conservation of angular momentum. • If the neutron star has a magnetic field, this field can form jets of ...
Supernova
... exceeds the electron repulsion, the core collapses immediately. – Energy in photons and neutrinos ...
... exceeds the electron repulsion, the core collapses immediately. – Energy in photons and neutrinos ...
Supernova - Mid-Pacific Institute
... Tycho Brahe and Johannes Kepler, discovered bright supernovae occurring in the Milky Way in 1572 and 1604. no supernova has been seen in our Galaxy since Kepler's. ...
... Tycho Brahe and Johannes Kepler, discovered bright supernovae occurring in the Milky Way in 1572 and 1604. no supernova has been seen in our Galaxy since Kepler's. ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Some stars end their lives in cataclysmic explosions: spectacular supernovae, which briefly become the most brilliant objects in their home galaxies, visible from millions or even billions of light-years away. Supernovae are of several distinct types, as is evident from their spectra—the graphs astr ...
... Some stars end their lives in cataclysmic explosions: spectacular supernovae, which briefly become the most brilliant objects in their home galaxies, visible from millions or even billions of light-years away. Supernovae are of several distinct types, as is evident from their spectra—the graphs astr ...
Introduction to Astrophysics Tutorial 4: Supernovae
... A second channel for stellar explosions involves an accreting white dwarf. When it approached MCh (but before actually reaching it), its C is ignited. Because of the high degeneracy (i.e. pressure weakly depends on temperature), the fusion process is a runaway one, burning the entire white dwarf, an ...
... A second channel for stellar explosions involves an accreting white dwarf. When it approached MCh (but before actually reaching it), its C is ignited. Because of the high degeneracy (i.e. pressure weakly depends on temperature), the fusion process is a runaway one, burning the entire white dwarf, an ...
stellar_explosions - UT Austin (Astronomy)
... Observationally, there are two classes of supernovae, which differ in their composition and their light curves (brightness vs. time—see Fig. 21.8, p. 561 in text). Type I: H-poor carbon detonation SN (former white dwarfs) Type II: H-rich core collapse SN (massive stars that burn up to iron) (You ...
... Observationally, there are two classes of supernovae, which differ in their composition and their light curves (brightness vs. time—see Fig. 21.8, p. 561 in text). Type I: H-poor carbon detonation SN (former white dwarfs) Type II: H-rich core collapse SN (massive stars that burn up to iron) (You ...
NOVAE and SUPERNOVAE
... Throughout history “new stars" have suddenly appeared in the night sky, then faded away. These objects were termed novae. Today, astronomers have determined that these new stars are actually stellar explosions. Nova explosions occur on the surface of white dwarfs, while supernova involve the ...
... Throughout history “new stars" have suddenly appeared in the night sky, then faded away. These objects were termed novae. Today, astronomers have determined that these new stars are actually stellar explosions. Nova explosions occur on the surface of white dwarfs, while supernova involve the ...
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.