The rebirth of Supernova 1987A a study of the ejecta-ring collision
... The explosion of a star is one of the most spectacular events in the universe. A supernova (SN) becomes as bright as its entire host galaxy before it starts to fade and an explosion in our own Galaxy, the Milky Way, may even be visible in daylight. However, over the past thousand years only a few ev ...
... The explosion of a star is one of the most spectacular events in the universe. A supernova (SN) becomes as bright as its entire host galaxy before it starts to fade and an explosion in our own Galaxy, the Milky Way, may even be visible in daylight. However, over the past thousand years only a few ev ...
Astrophysics in a Nutshell, Second Edition
... undergo after the main sequence, and the properties of their compact remnants—white dwarfs, neutron stars, and black holes. We then study the phenomena that can occur when such compact objects accrete material from a companion star in a binary pair. ...
... undergo after the main sequence, and the properties of their compact remnants—white dwarfs, neutron stars, and black holes. We then study the phenomena that can occur when such compact objects accrete material from a companion star in a binary pair. ...
Aldebaran
... nuclear reaction in its atoms. When the gases and dust of the nebula contracted, a protostar was formed. Gravity caused the protostar to condense further and heat up. Nuclear reactions occurred when the temperature in the center of the protostar reached about 10 million degrees, and the star was bor ...
... nuclear reaction in its atoms. When the gases and dust of the nebula contracted, a protostar was formed. Gravity caused the protostar to condense further and heat up. Nuclear reactions occurred when the temperature in the center of the protostar reached about 10 million degrees, and the star was bor ...
Lab 7
... star chart printed on a page, we often forget about the three-dimensional nature of the universe. In this exercise, you will construct (with welding rods and Styrofoam balls) a model of nearby space including many of the nearest stars. Of course, you will need information on where to place the stars ...
... star chart printed on a page, we often forget about the three-dimensional nature of the universe. In this exercise, you will construct (with welding rods and Styrofoam balls) a model of nearby space including many of the nearest stars. Of course, you will need information on where to place the stars ...
Nuclear astrophysics: the unfinished quest for the origin of the
... The determination of the chemical composition of a distant star is not a trivial task. It basically relies on the analysis of the electromagnetic radiation emitted at different wavelengths (so-called spectra). For the case of the Solar System abundances, several sources of information, that combine ...
... The determination of the chemical composition of a distant star is not a trivial task. It basically relies on the analysis of the electromagnetic radiation emitted at different wavelengths (so-called spectra). For the case of the Solar System abundances, several sources of information, that combine ...
Neutrinos and Nucleosynthesis
... the fate of a massive star. When a massive star runs out of burning fuel it starts to collapse under its own gravitational pressure. A possible remnant of such a supernova is a neutron star. In this environment, after the supernova has happened, the nucleosynthesis process starts. Two possible sites ...
... the fate of a massive star. When a massive star runs out of burning fuel it starts to collapse under its own gravitational pressure. A possible remnant of such a supernova is a neutron star. In this environment, after the supernova has happened, the nucleosynthesis process starts. Two possible sites ...
AST1100 Lecture Notes
... less than one tenth of the number of stars in the Milky Way and are located at a distance of about 160 000ly (LMC) and 200 000ly (SMC) from the Sun. In 1908, Henrietta Leavitt at Harvard University discovered about 2400 of these pulsating stars in the SMC. The pulsation period of these stars were fo ...
... less than one tenth of the number of stars in the Milky Way and are located at a distance of about 160 000ly (LMC) and 200 000ly (SMC) from the Sun. In 1908, Henrietta Leavitt at Harvard University discovered about 2400 of these pulsating stars in the SMC. The pulsation period of these stars were fo ...
17_Testbank
... 33) Consider the star to which the arrow points. How is it currently generating energy? A) by gravitational contraction B) by hydrogen shell burning around an inert helium core C) by core hydrogen fusion D) by core helium fusion combined with hydrogen shell burning E) by both hydrogen and helium sh ...
... 33) Consider the star to which the arrow points. How is it currently generating energy? A) by gravitational contraction B) by hydrogen shell burning around an inert helium core C) by core hydrogen fusion D) by core helium fusion combined with hydrogen shell burning E) by both hydrogen and helium sh ...
AST1100 Lecture Notes
... less than one tenth of the number of stars in the Milky Way and are located at a distance of about 160 000ly (LMC) and 200 000ly (SMC) from the Sun. In 1908, Henrietta Leavitt at Harvard University discovered about 2400 of these pulsating stars in the SMC. The pulsation period of these stars were fo ...
... less than one tenth of the number of stars in the Milky Way and are located at a distance of about 160 000ly (LMC) and 200 000ly (SMC) from the Sun. In 1908, Henrietta Leavitt at Harvard University discovered about 2400 of these pulsating stars in the SMC. The pulsation period of these stars were fo ...
Module 4.1 - The Scale of the Universe [slide 1] We now turn to
... the distance indicators relevant to each other. And this is what's known as the distance ladder. Locally, those will be various stellar types of indicators, say, based on pulsating stars or star clusters and things like that, then properties of nearby galaxies, using their scaling relations and so o ...
... the distance indicators relevant to each other. And this is what's known as the distance ladder. Locally, those will be various stellar types of indicators, say, based on pulsating stars or star clusters and things like that, then properties of nearby galaxies, using their scaling relations and so o ...
Zapartas_deMink_Izzard_AA_2017
... robustness of our results by running various simulations to account for the uncertainties in our standard assumptions. We find that a significant fraction, 15+98 %, of core-collapse supernovae are ‘late’, that is, they occur 50-200 Myrs after birth, when all massive single stars have already explode ...
... robustness of our results by running various simulations to account for the uncertainties in our standard assumptions. We find that a significant fraction, 15+98 %, of core-collapse supernovae are ‘late’, that is, they occur 50-200 Myrs after birth, when all massive single stars have already explode ...
X-ray Binaries
... stars and stellar–mass black holes which are the end points of massive star evolution. Studying these remnants thus provides clues to understanding the evolutionary processes that lead to their formation. We focus here on the distributions of dynamical masses, space velocities and chemical anomalies ...
... stars and stellar–mass black holes which are the end points of massive star evolution. Studying these remnants thus provides clues to understanding the evolutionary processes that lead to their formation. We focus here on the distributions of dynamical masses, space velocities and chemical anomalies ...
arXiv:astro-ph/0612072v1 4 Dec 2006 Theory of core
... the outer burning shells of the star, one speaks about the ‘prompt mechanism’. However, it appears as if the energy available to the shock is not sufficient, and the shock uses up its energy in the outer core mostly by the dissociation of heavy nuclei into nucleons. This change in composition result ...
... the outer burning shells of the star, one speaks about the ‘prompt mechanism’. However, it appears as if the energy available to the shock is not sufficient, and the shock uses up its energy in the outer core mostly by the dissociation of heavy nuclei into nucleons. This change in composition result ...
PowerPoint
... • In-Class Q and A: On Wed., Nov. 5th, some time will be allotted in class to ask questions about material on the exam. For example, if there are homework answers you do not understand, this would be an excellent time to ask. To get the most out of this time, you are strongly encouraged to begin stu ...
... • In-Class Q and A: On Wed., Nov. 5th, some time will be allotted in class to ask questions about material on the exam. For example, if there are homework answers you do not understand, this would be an excellent time to ask. To get the most out of this time, you are strongly encouraged to begin stu ...
The Korean 1592--1593 Record of a Guest Star: Animpostor`of the
... about 3 degrees in the traditional angle-measuring system. If the north polar distance is used as recorded, the total angular separation between the comet and ι Cet is 3.1 degrees. In either case, the separation intended by the expression “inside a star” was much larger than one degree, as large as ...
... about 3 degrees in the traditional angle-measuring system. If the north polar distance is used as recorded, the total angular separation between the comet and ι Cet is 3.1 degrees. In either case, the separation intended by the expression “inside a star” was much larger than one degree, as large as ...
15.1 Introduction
... We saw in Lecture 13 that low- and intermediate-mass stars (with M ≤ 8M ) develop carbon-oxygen cores that become degenerate after central He burning. The electron degenerate pressure supports the core against further collapse; as a consequence, the maximum core temperature reached in these stars i ...
... We saw in Lecture 13 that low- and intermediate-mass stars (with M ≤ 8M ) develop carbon-oxygen cores that become degenerate after central He burning. The electron degenerate pressure supports the core against further collapse; as a consequence, the maximum core temperature reached in these stars i ...
TOWARD A MODEL FOR THE Be BINARY SYSTEM PER 1
... with the Paschen emissions and which were made from considerably lower dispersion plates than the rest of my data seem to indicate that these lines follow the primary and their emission edges do not reveal the influence of any emission from the secondary. Clearly, the conditions under which they are ...
... with the Paschen emissions and which were made from considerably lower dispersion plates than the rest of my data seem to indicate that these lines follow the primary and their emission edges do not reveal the influence of any emission from the secondary. Clearly, the conditions under which they are ...
Dr. Amanda Karakas and Prof. John Lattanzio
... 3. Binary evolution channels: mass loss, envelope ejection, Type Ia supernova and nova explosions ...
... 3. Binary evolution channels: mass loss, envelope ejection, Type Ia supernova and nova explosions ...
opportunities nuclear astrophysics
... Our understanding of these processes has developed greatly in the last 75 years. It was known early on that nuclear reactions must provide the energy for the sun. No other processes, chemical or gravitational, could yield the sun’s luminosity over its 4.6 billion-year life. More direct evidence for ...
... Our understanding of these processes has developed greatly in the last 75 years. It was known early on that nuclear reactions must provide the energy for the sun. No other processes, chemical or gravitational, could yield the sun’s luminosity over its 4.6 billion-year life. More direct evidence for ...
Institute for Structure and Nuclear Astrophysics
... Our understanding of these processes has developed greatly in the last 75 years. It was known early on that nuclear reactions must provide the energy for the sun. No other processes, chemical or gravitational, could yield the sun’s luminosity over its 4.6 billion-year life. More direct evidence for ...
... Our understanding of these processes has developed greatly in the last 75 years. It was known early on that nuclear reactions must provide the energy for the sun. No other processes, chemical or gravitational, could yield the sun’s luminosity over its 4.6 billion-year life. More direct evidence for ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... peak magnitude we use Hubble Space Telescope archival data to subtract off the nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear ...
... peak magnitude we use Hubble Space Telescope archival data to subtract off the nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear ...
Galaxies
... Population I stars in the disk and spiral arms. Neutral hydrogen gas, invisible in the optical, but visible in the 21 cm radio line. Dark matter. ...
... Population I stars in the disk and spiral arms. Neutral hydrogen gas, invisible in the optical, but visible in the 21 cm radio line. Dark matter. ...
1 - Piscataway High School
... enough, helium fusion begins to make energy, and the temperature rises, but pressure does not increase because the gas is degenerate. The higher temperature increases the helium fusion even further, and the result is a runaway explosion called the helium flash in which, for a few minutes, the core o ...
... enough, helium fusion begins to make energy, and the temperature rises, but pressure does not increase because the gas is degenerate. The higher temperature increases the helium fusion even further, and the result is a runaway explosion called the helium flash in which, for a few minutes, the core o ...
D ASTROPHYSICS
... A galaxy is a creation of stars, gas, and dust held together by gravity and containing billions of stars. The Milky Way contains about 3 × 10 11 stars and, probably, at least this number of planets. Some galaxies exist in isolation but the majority of them occur in groups known as clusters that have ...
... A galaxy is a creation of stars, gas, and dust held together by gravity and containing billions of stars. The Milky Way contains about 3 × 10 11 stars and, probably, at least this number of planets. Some galaxies exist in isolation but the majority of them occur in groups known as clusters that have ...
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.