Interstellar clouds
... countless nova outbursts, the mass of the white dwarf increases. • There comes a point when the pressure can no longer balance gravity and the temperature of 6 X 108 K fuse carbon nuclei up to element ...
... countless nova outbursts, the mass of the white dwarf increases. • There comes a point when the pressure can no longer balance gravity and the temperature of 6 X 108 K fuse carbon nuclei up to element ...
Plotting Supernova Light Curves
... this explosion, the star increases drastically in luminosity, which is the visible supernova. The matter which was blown out from the star heats up as it travels through the gas and dust in space, causing it to glow. This is known as a supernova remnant. Depending on the mass of the star, it either ...
... this explosion, the star increases drastically in luminosity, which is the visible supernova. The matter which was blown out from the star heats up as it travels through the gas and dust in space, causing it to glow. This is known as a supernova remnant. Depending on the mass of the star, it either ...
PowerPoint - Chandra X
... IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio data from the Very Large A ...
... IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio data from the Very Large A ...
mass per nucleon
... shell Hydrogen burning (red giant) core Helium burning (Helium Flash) shell Helium burning (double-shell burning red giant) planetary nebula white dwarf ...
... shell Hydrogen burning (red giant) core Helium burning (Helium Flash) shell Helium burning (double-shell burning red giant) planetary nebula white dwarf ...
Neutron Stars and Black Holes
... •! But most likely, the white dwarf will not become a supernova •! Anyway, it is 10-100 million years away from becoming a red giant. ...
... •! But most likely, the white dwarf will not become a supernova •! Anyway, it is 10-100 million years away from becoming a red giant. ...
key - Scioly.org
... a) Sirius A releases 26 times as much energy as our Sun. b) The existence of Sirius B was predicted by Bessel in 1844. It was first observed in 1862 by Alvan Clark (4 points: 1 point for each answer) c) Oxygen and carbon (2 points) 33) HM Cancri or RX J0806.3+152 (7 points) a) 321.5 seconds (5.4 m ...
... a) Sirius A releases 26 times as much energy as our Sun. b) The existence of Sirius B was predicted by Bessel in 1844. It was first observed in 1862 by Alvan Clark (4 points: 1 point for each answer) c) Oxygen and carbon (2 points) 33) HM Cancri or RX J0806.3+152 (7 points) a) 321.5 seconds (5.4 m ...
What is a Star
... If brightness and surface temperature are considered, stars can be plotted on a graph called the Hertzsprung-Russell Diagram, a graph of great utility for the understanding of the life cycle of the stars. Birth of a star Stellar evolution begins with the gravitational collapse of part of a nebula cl ...
... If brightness and surface temperature are considered, stars can be plotted on a graph called the Hertzsprung-Russell Diagram, a graph of great utility for the understanding of the life cycle of the stars. Birth of a star Stellar evolution begins with the gravitational collapse of part of a nebula cl ...
Stellar Evolution (Powerpoint) 17
... • Then, star collapses under the weight and because it is electron degenerate, energy created will not expand the star and shut off the fusion. • So, entire star (carbon, mostly) undergoes fusion at once. What a star normally takes billions of years to burn, this star burns all at once. BIG explosio ...
... • Then, star collapses under the weight and because it is electron degenerate, energy created will not expand the star and shut off the fusion. • So, entire star (carbon, mostly) undergoes fusion at once. What a star normally takes billions of years to burn, this star burns all at once. BIG explosio ...
2.5.2 development of a star
... During this time it is stable as the gravitational forces that enable hydrogen burning balance and pull the star in, balance with the gas pressure pushing out. This is much like the gas pressure inside a balloon balancing with the tension in the plastic of the balloon. In the star it is known ...
... During this time it is stable as the gravitational forces that enable hydrogen burning balance and pull the star in, balance with the gas pressure pushing out. This is much like the gas pressure inside a balloon balancing with the tension in the plastic of the balloon. In the star it is known ...
Lecture 10a Neutron Star and Black Holes (Test 2 overview)
... • Massive stars have fusion to heavier nuclei (Neon, Silicon, Sulpher, etc) • End up with core of Iron nuclei plus 26 unbound “free” electrons for every Fe • Electrons are “degenerate” as so close together. This causes them to provide most of the pressure resisting gravity • Enormous stress. If ...
... • Massive stars have fusion to heavier nuclei (Neon, Silicon, Sulpher, etc) • End up with core of Iron nuclei plus 26 unbound “free” electrons for every Fe • Electrons are “degenerate” as so close together. This causes them to provide most of the pressure resisting gravity • Enormous stress. If ...
29.3 – Stellar Evolution
... gases = planetary nebula •Gravity causes star to collapse inward •Hot, dense core of matter = white dwarf ...
... gases = planetary nebula •Gravity causes star to collapse inward •Hot, dense core of matter = white dwarf ...
Is space created and destroyed? 9 Feb 16 Feb 2012
... gravity. The hydrogen is from the outermost part of the star. è A Type I supernova is a white dwarf that explodes. A WD and giant orbit each other. Mass moves from the giant to the WD. WD explodes when it gets so much mass from the giant that degeneracy pressure can no longer oppose gravity. è Type ...
... gravity. The hydrogen is from the outermost part of the star. è A Type I supernova is a white dwarf that explodes. A WD and giant orbit each other. Mass moves from the giant to the WD. WD explodes when it gets so much mass from the giant that degeneracy pressure can no longer oppose gravity. è Type ...
Constellation, Star, and Deep Sky Object
... Black Hole – supernova remnant where ≥ 3-4 solar masses are compressed into infinitely small space, gravity around it is so intense that not even light can escape the gravitational field Supernovae Type Ia – If a carbon-oxygen white dwarf star goes over the Chandrasekhar Limit of about 1.38 solar ma ...
... Black Hole – supernova remnant where ≥ 3-4 solar masses are compressed into infinitely small space, gravity around it is so intense that not even light can escape the gravitational field Supernovae Type Ia – If a carbon-oxygen white dwarf star goes over the Chandrasekhar Limit of about 1.38 solar ma ...
Exploding Massive Stars:
... ascertain the core collapse supernova mechanism(s) understand supernova phenomenology e.g.: (1) element synthesis, (2) neutrino, gravitational wave, and gamma ray signatures provide theoretical foundation in support of OS experimental facilities (RHIC, SNO, RIA, NUSL) develop enabling technolo ...
... ascertain the core collapse supernova mechanism(s) understand supernova phenomenology e.g.: (1) element synthesis, (2) neutrino, gravitational wave, and gamma ray signatures provide theoretical foundation in support of OS experimental facilities (RHIC, SNO, RIA, NUSL) develop enabling technolo ...
Another Old Final
... (b) Estimate the distance to this supernova and the lookback time (how long ago we are observing it). (c) Type-Ia supernovae reach peak luminosities of 109 L . Estimate the peak apparent brightness of this supernova. Would it have been visible to the naked eye on a clear night? ...
... (b) Estimate the distance to this supernova and the lookback time (how long ago we are observing it). (c) Type-Ia supernovae reach peak luminosities of 109 L . Estimate the peak apparent brightness of this supernova. Would it have been visible to the naked eye on a clear night? ...
PHY 150
... The mass determines the gravitational pressure at the core of the star. The greater the mass the greater the pressure, the greater the temperature, the greater the luminosity, the faster the burning of the star’s fuel, the heavier the elements that can ultimately be burned in the core, and the ultim ...
... The mass determines the gravitational pressure at the core of the star. The greater the mass the greater the pressure, the greater the temperature, the greater the luminosity, the faster the burning of the star’s fuel, the heavier the elements that can ultimately be burned in the core, and the ultim ...
E5 stellar processes and stellar evolution (HL only)
... • Neutron stars with masses substantially more than the Oppenheimer-Volkoff limit continue to collapse as the neutron pressure is insufficient. They become Black holes • At the centre of the black hole is a singularity • The boundary around the singularity where even light does not have sufficient e ...
... • Neutron stars with masses substantially more than the Oppenheimer-Volkoff limit continue to collapse as the neutron pressure is insufficient. They become Black holes • At the centre of the black hole is a singularity • The boundary around the singularity where even light does not have sufficient e ...
File
... systems can end their lives in a different manner.) Since the Sun is a typical star in this mass range, we focus our attention on stars of one solar mass when describing the various evolutionary stages of stars. ...
... systems can end their lives in a different manner.) Since the Sun is a typical star in this mass range, we focus our attention on stars of one solar mass when describing the various evolutionary stages of stars. ...
An absence of ex-companion stars in the type Ia supernova remnant
... white dwarf) will survive the explosion, and shine at near its preexplosion brightness from the middle of the expanding supernova remnant. (During the explosion, portions of the outer envelope of the companion star will be stripped off22,23, but its location on the colour–magnitude diagram will not ...
... white dwarf) will survive the explosion, and shine at near its preexplosion brightness from the middle of the expanding supernova remnant. (During the explosion, portions of the outer envelope of the companion star will be stripped off22,23, but its location on the colour–magnitude diagram will not ...
SupernovaExplosionPhysics_8pages
... GeV/fm2 ) which are compressed by the collapse, but then spring back to equilibrium, thus the bounce. 7. The bounce sends a shock wave outward at high velocity, blowing off the remaining stellar atmosphere in the process. One the shock reaches the outer atmosphere, the photons emitted by recombinati ...
... GeV/fm2 ) which are compressed by the collapse, but then spring back to equilibrium, thus the bounce. 7. The bounce sends a shock wave outward at high velocity, blowing off the remaining stellar atmosphere in the process. One the shock reaches the outer atmosphere, the photons emitted by recombinati ...
Life Cycle of Stars - Lab Science Schedule
... Medium-sized stars pass through a red-giant stage before they become white dwarfs and die. The core of the star left behind after the supernova may become a neutron star or a black hole, depending on the star’s starting mass. The Life and Death of Stars Changes in stars may take place over a few mil ...
... Medium-sized stars pass through a red-giant stage before they become white dwarfs and die. The core of the star left behind after the supernova may become a neutron star or a black hole, depending on the star’s starting mass. The Life and Death of Stars Changes in stars may take place over a few mil ...
Stellar Evolution II
... main-sequence star becomes a giant • When hydrogen fusion ceases in the core, the star will collapse inward – this causes the layer just outside the core to become so hot and dense so that hydrogen fusion will begin in this outer layer. • The energy produced by hydrogen fusion in this layer just out ...
... main-sequence star becomes a giant • When hydrogen fusion ceases in the core, the star will collapse inward – this causes the layer just outside the core to become so hot and dense so that hydrogen fusion will begin in this outer layer. • The energy produced by hydrogen fusion in this layer just out ...
Information (Word Doc)
... Gravity pulls the materials together. Compressing the gas and dust into a giant ball that, at it’s centre temperatures are 15 million degrees or so (created by all gas and dust bumping into each other under the great pressure of the surrounding material). The pressure at the centre of the ball becom ...
... Gravity pulls the materials together. Compressing the gas and dust into a giant ball that, at it’s centre temperatures are 15 million degrees or so (created by all gas and dust bumping into each other under the great pressure of the surrounding material). The pressure at the centre of the ball becom ...
Stages in the Life of a Star
... • Core Fusion -- core has shrunk enough to create high enough temperatures to start Helium (or heavier element) fusion (100 million K). • In low mass stars the onset of Helium fusion can be very rapid, producing a burst of energy helium flash. • Eventually it settles down. • Core Fusion is releasing ...
... • Core Fusion -- core has shrunk enough to create high enough temperatures to start Helium (or heavier element) fusion (100 million K). • In low mass stars the onset of Helium fusion can be very rapid, producing a burst of energy helium flash. • Eventually it settles down. • Core Fusion is releasing ...
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.