PowerPoint - Chandra X
... colors in this image show low energy X-rays (red), intermediate energy X-rays (green) and high energy X-rays (blue). ...
... colors in this image show low energy X-rays (red), intermediate energy X-rays (green) and high energy X-rays (blue). ...
The Milky Way
... learn that stars are born and grow old. Modern astronomers can tell the story of the stars right to the end. Here you will learn how stars die, but as you follow the story you will see how astronomers have tested their theories against evidence to answer four ...
... learn that stars are born and grow old. Modern astronomers can tell the story of the stars right to the end. Here you will learn how stars die, but as you follow the story you will see how astronomers have tested their theories against evidence to answer four ...
Stellar Evolution
... • If the core’s mass is even greater/denser than a neutron star, it collapses. • Surface gravity is so great that no matter can escape it…not even electromagnetic ...
... • If the core’s mass is even greater/denser than a neutron star, it collapses. • Surface gravity is so great that no matter can escape it…not even electromagnetic ...
Future Supernova Projects
... • small dispersion • single objects (simpler than galaxies) • can be observed over wide z range Challenges: • dust (grey dust) • chemical composition • evolution • photometric calibration (e.g., Vega) • environmental differences Systematics • lensing Step 2 ...
... • small dispersion • single objects (simpler than galaxies) • can be observed over wide z range Challenges: • dust (grey dust) • chemical composition • evolution • photometric calibration (e.g., Vega) • environmental differences Systematics • lensing Step 2 ...
Chapter 13: The Death of Stars
... learn that stars are born and grow old. Modern astronomers can tell the story of the stars right to the end. Here you will learn how stars die, but as you follow the story you will see how astronomers have tested their theories against evidence to answer four ...
... learn that stars are born and grow old. Modern astronomers can tell the story of the stars right to the end. Here you will learn how stars die, but as you follow the story you will see how astronomers have tested their theories against evidence to answer four ...
A-105 Homework 1
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
poster
... the templates defined by Kinney and al. • A Principal Component Analysis (PCA). This method decreases the number of variables and makes possible a spectral classification of the galaxies. Host Galaxy ...
... the templates defined by Kinney and al. • A Principal Component Analysis (PCA). This method decreases the number of variables and makes possible a spectral classification of the galaxies. Host Galaxy ...
Endpoints of stellar evolution
... Whole star explodes – no remnant b) collapsing Fe core in massive star Fe cannot ignite, but collapse halted by degenerate NUCLEON gas at a radius of ~10 km ...
... Whole star explodes – no remnant b) collapsing Fe core in massive star Fe cannot ignite, but collapse halted by degenerate NUCLEON gas at a radius of ~10 km ...
How the Universe Works Extreme Stars Name 1. When a star dies
... How the Universe Works Extreme Stars Name _______________ 1. When a star dies (gravity) (fusion) wins out. 2. The sun will run out of fuel in about (3) (7) (10) billion years. 3. When the sun runs out of hydrogen fuel, it will become a (red giant) (neutron star) (black hole). 4. Eventually, the heli ...
... How the Universe Works Extreme Stars Name _______________ 1. When a star dies (gravity) (fusion) wins out. 2. The sun will run out of fuel in about (3) (7) (10) billion years. 3. When the sun runs out of hydrogen fuel, it will become a (red giant) (neutron star) (black hole). 4. Eventually, the heli ...
Prep Homework Solutions for HW due 10/04/10
... Sequence before its companion, but then it lost significant mass through mass transfer to the companion, so the more massive star is the less massive star now. Note: a couple of you suggested that the paradox could be resolved by supposing that stars in binaries change each other rate of aging or “l ...
... Sequence before its companion, but then it lost significant mass through mass transfer to the companion, so the more massive star is the less massive star now. Note: a couple of you suggested that the paradox could be resolved by supposing that stars in binaries change each other rate of aging or “l ...
Lecture 19 Review
... heavy elements. There are no more fusion processes. Beyond this point it takes energy to make a heavier element. At this point gravitational collapse occurs followed by a catastrophic rebound. A fast neutron process produces heavy elements all the way up to Plutonium. There is a strong neutron burst ...
... heavy elements. There are no more fusion processes. Beyond this point it takes energy to make a heavier element. At this point gravitational collapse occurs followed by a catastrophic rebound. A fast neutron process produces heavy elements all the way up to Plutonium. There is a strong neutron burst ...
PowerPoint
... Q: Does anything survive the Type II SN Explosion? The inward pressure is enormous, due to the high mass of the star. There is nothing stopping the star from collapsing further; it does so very rapidly, in a giant implosion. As it continues to become more and more dense, the protons and electrons re ...
... Q: Does anything survive the Type II SN Explosion? The inward pressure is enormous, due to the high mass of the star. There is nothing stopping the star from collapsing further; it does so very rapidly, in a giant implosion. As it continues to become more and more dense, the protons and electrons re ...
molecular clouds
... The Interstellar Medium • Today stars form in a complex environment • Hydrogen and helium are the predominant components of the ISM, but it is enriched with heavier elements from earlier stars (created in stellar fusion and supernova explosions). ...
... The Interstellar Medium • Today stars form in a complex environment • Hydrogen and helium are the predominant components of the ISM, but it is enriched with heavier elements from earlier stars (created in stellar fusion and supernova explosions). ...
Our Worlds, Other Worlds
... If we are too close to a radioactive source, like a chunk of uranium, we cannot see the radiation, but it is still harmful to us! So how far should Earth be from cosmic radiation sources to be safe? ...
... If we are too close to a radioactive source, like a chunk of uranium, we cannot see the radiation, but it is still harmful to us! So how far should Earth be from cosmic radiation sources to be safe? ...
ASTRONOMY 157 – Stars and Galaxies - Syllabus
... Core collapse, H shell burning, expansion to red giant, helium flash, heavy element production ...
... Core collapse, H shell burning, expansion to red giant, helium flash, heavy element production ...
doc
... square root of 10,000 (=100) times further away... more than twice the distance of the orbit of Pluto. (Note: No such stars actually exist - even the hottest (non-whitedwarf) stars are only about 6-7 times the Sun's temperature, and these are all somewhat larger than the Sun. This is just an exercis ...
... square root of 10,000 (=100) times further away... more than twice the distance of the orbit of Pluto. (Note: No such stars actually exist - even the hottest (non-whitedwarf) stars are only about 6-7 times the Sun's temperature, and these are all somewhat larger than the Sun. This is just an exercis ...
The Danger of Deadly Cosmic Explosions
... A Nearby Supernova Can Ruin Your Existence • Deadly from neutrinos within 30 light years. • Atmosphere, weather, ruined. • Major extinction. • Not much harm if further. • SN material in sediments. • 1 SN/100 years in our galaxy • Close 1 per 100million years. • Good news: our neighbor stars peacefu ...
... A Nearby Supernova Can Ruin Your Existence • Deadly from neutrinos within 30 light years. • Atmosphere, weather, ruined. • Major extinction. • Not much harm if further. • SN material in sediments. • 1 SN/100 years in our galaxy • Close 1 per 100million years. • Good news: our neighbor stars peacefu ...
Supernovae March 23 − Supernova 1987A
... period Chih-ho, …, a guest star appeared several degrees SE of Thien-kuan. After more than a year it gradually became invisible.−p564. ...
... period Chih-ho, …, a guest star appeared several degrees SE of Thien-kuan. After more than a year it gradually became invisible.−p564. ...
12.4 Evolution of Stars More Massive than the Sun
... 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. ...
NUCLEAR FISSION- a Tunneling Process NUCLEAR FUSION
... different nuclei must be at high T. A simple fusion process- a proton fuses with C-12 The radiation emitted during the to make N-13, with emission of a photon. fusion keeps T high. Slowly the heavier elements up to Fe (whose nucleus has 26 protons and 30 neutrons) are synthesized- depending on the m ...
... different nuclei must be at high T. A simple fusion process- a proton fuses with C-12 The radiation emitted during the to make N-13, with emission of a photon. fusion keeps T high. Slowly the heavier elements up to Fe (whose nucleus has 26 protons and 30 neutrons) are synthesized- depending on the m ...
Nuclear Physics - fission, fusion, and the stars
... different nuclei must be at high T. A simple fusion process- a proton fuses with C-12 The radiation emitted during the to make N-13, with emission of a photon. fusion keeps T high. Slowly the heavier elements up to Fe (whose nucleus has 26 protons and 30 neutrons) are synthesized- depending on the m ...
... different nuclei must be at high T. A simple fusion process- a proton fuses with C-12 The radiation emitted during the to make N-13, with emission of a photon. fusion keeps T high. Slowly the heavier elements up to Fe (whose nucleus has 26 protons and 30 neutrons) are synthesized- depending on the m ...
Lesson Plan: Supernova`s
... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
Stellar Evolution
... layers are driven away • Core becomes hot enough to produce Carbon (C) • Star contracts to normal size when helium is used up • Carbon core left over, White dwarf remains ...
... layers are driven away • Core becomes hot enough to produce Carbon (C) • Star contracts to normal size when helium is used up • Carbon core left over, White dwarf remains ...
Slide 1
... hot gas which looks like planetary disk, and called Planetary Nebulae (PNe) (nothing to do with planets per se) • PNe cores continue to cool and become White Dwarfs (94% stars end up as WDs) ...
... hot gas which looks like planetary disk, and called Planetary Nebulae (PNe) (nothing to do with planets per se) • PNe cores continue to cool and become White Dwarfs (94% stars end up as WDs) ...
3. Stellar Formation and Evolution
... abundance of heavy elements in the Solar System, such as uranium, relative to the abundances of these elements in Population II stars. • These elements could most plausibly have been produced by endergonic nuclear reactions during a supernova, or by transmutation through neutron absorption inside a ...
... abundance of heavy elements in the Solar System, such as uranium, relative to the abundances of these elements in Population II stars. • These elements could most plausibly have been produced by endergonic nuclear reactions during a supernova, or by transmutation through neutron absorption inside a ...
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.