Lecture 14 - Center for Astrophysics and Space Astronomy CASA
... That’s as much energy as the Sun emits during its entire lifetime. In a few seconds!!!! This is so titanic we can see it across the universe A billion trillion trillion atomic bombs ...
... That’s as much energy as the Sun emits during its entire lifetime. In a few seconds!!!! This is so titanic we can see it across the universe A billion trillion trillion atomic bombs ...
Round 1
... Before reaching the main sequence, a protostar is doing this. (contracting due to gravity) A star becomes a red giant when this happens. (runs out of hydrogen to fuse in its core → leaves the main sequence) $1600 A Type 1a supernova occurs when a white dwarf’s mass exceeds this. (1.4 M ) $2000 This ...
... Before reaching the main sequence, a protostar is doing this. (contracting due to gravity) A star becomes a red giant when this happens. (runs out of hydrogen to fuse in its core → leaves the main sequence) $1600 A Type 1a supernova occurs when a white dwarf’s mass exceeds this. (1.4 M ) $2000 This ...
17 The Deaths of Stars
... 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 supernova ...
... 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 supernova ...
The Death of Stars - Mounds Park Academy Blogs
... • Stars less than 1.4 times the mass of the sun continue to shrink. • Our Sun will shrink until it becomes the size of the earth. • It becomes very dense (1 tsp. = 5 tons) • Small and faint White Dwarfs are hard to see. • They slowly fizzle out over billions of years. ...
... • Stars less than 1.4 times the mass of the sun continue to shrink. • Our Sun will shrink until it becomes the size of the earth. • It becomes very dense (1 tsp. = 5 tons) • Small and faint White Dwarfs are hard to see. • They slowly fizzle out over billions of years. ...
The Sun - Center for Astrophysics and Space Astronomy CASA
... (On border between fusion and fission) Develops degenerate iron core than cannot flash Just gets hotter and heavier down in the middle of the star ...
... (On border between fusion and fission) Develops degenerate iron core than cannot flash Just gets hotter and heavier down in the middle of the star ...
How the Universe Works: Supernova Video Guide
... 2. Our Sun won’t become a supernova because its too ___________________________. 3. The Sun is a nuclear reactor that fuses hydrogen atoms into helium and energy. Helium fuses into carbon, carbon into oxygen. When small stars begin to make ___________________, they begin to ______________________. 4 ...
... 2. Our Sun won’t become a supernova because its too ___________________________. 3. The Sun is a nuclear reactor that fuses hydrogen atoms into helium and energy. Helium fuses into carbon, carbon into oxygen. When small stars begin to make ___________________, they begin to ______________________. 4 ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... Beyond that, though, consider that most of the energy of a Type II supernova comes out as neutrinos. (A lot of neutrinos will come out in a Type Ia as well, but not as big a fraction.) If the supernova is close enough and you have a good enough neutrino detector, measuring the number of neutrinos yo ...
... Beyond that, though, consider that most of the energy of a Type II supernova comes out as neutrinos. (A lot of neutrinos will come out in a Type Ia as well, but not as big a fraction.) If the supernova is close enough and you have a good enough neutrino detector, measuring the number of neutrinos yo ...
Lecture 15 - Deaths of Stars, Supernovae
... Determining the age of a star cluster • Imagine we have a cluster of stars that were all formed at the same time, but have a variety of different masses • Using what we know about stellar evolution is there a way to determine the age of the star cluster? ...
... Determining the age of a star cluster • Imagine we have a cluster of stars that were all formed at the same time, but have a variety of different masses • Using what we know about stellar evolution is there a way to determine the age of the star cluster? ...
Degeneracy pressure Normal/degeneracy pressure White dwarfs — Oct 10
... from SN, now by blast wave from SN. ...
... from SN, now by blast wave from SN. ...
A Star’s Life
... b. Search the internet for an appropriate real image. If a real life image is not available, please state this is an artist’s rendering. c. Please share the slide show with me when you create in Google slides. ...
... b. Search the internet for an appropriate real image. If a real life image is not available, please state this is an artist’s rendering. c. Please share the slide show with me when you create in Google slides. ...
Life Cycle of Stars: Chapter 21
... • Expands and collapses to facilitate helium burning – Becomes helium burning star ...
... • Expands and collapses to facilitate helium burning – Becomes helium burning star ...
Nuclear Interactions in Supernovae .
... Chandrasekhar Limit • The white dwarf will continue to accrete mass, the pressure and density of the dwarf rises and the temperature increases from this increase in weight bearing down on the dead core. • Eventually (at around 1.38 solar masses) the temperature is increased so much, carbon starts f ...
... Chandrasekhar Limit • The white dwarf will continue to accrete mass, the pressure and density of the dwarf rises and the temperature increases from this increase in weight bearing down on the dead core. • Eventually (at around 1.38 solar masses) the temperature is increased so much, carbon starts f ...
ppt file
... If M>0.4Msun, start to burn HeC through the triplealpha process (occurs explosively if 0.4Msun2-3Msun)
The expels stellar envelope in series of explosive
events (novae)… form a planetary nebula
He or C core remains as a white dwarf… dense
(stellar mass but size of Earth) an ...
... If M>0.4Msun, start to burn HeC through the triplealpha process (occurs explosively if 0.4Msun
The Hidden Lives of Galaxies NSTA 2001
... more material. • Contraction causes Temperature and Pressure to slowly increase. ...
... more material. • Contraction causes Temperature and Pressure to slowly increase. ...
Type I SuperNova
... degeneracy pressure can no longer support the strong gravitational pull, the temperature will rise, and carbon will fuse explosively in the dwarf. The carbon/oxygen fuse explosively, blowing the entire system into space and leaving nothing behind. ...
... degeneracy pressure can no longer support the strong gravitational pull, the temperature will rise, and carbon will fuse explosively in the dwarf. The carbon/oxygen fuse explosively, blowing the entire system into space and leaving nothing behind. ...
Homework #3 10 points Question #1 (2 pts) The brightest star in the
... Thermonuclear supernova is an explosion of a white dwarf, which is less massive than a progenitor of a core-collapse supernova. Which produces a larger fractional abundance of iron? You can think the following way: let’s imagine that in a region of space A we found one massive star that exploded as ...
... Thermonuclear supernova is an explosion of a white dwarf, which is less massive than a progenitor of a core-collapse supernova. Which produces a larger fractional abundance of iron? You can think the following way: let’s imagine that in a region of space A we found one massive star that exploded as ...
Death of Massive Stars
... • Any event that takes place inside the Schwarzchild radius of a black hole can never be seen by the outside universe. The Schwarzchild radius is effectively the boundary of the black hole (its surface), and is called the event horizon. • The only things we can tell about the matter inside the black ...
... • Any event that takes place inside the Schwarzchild radius of a black hole can never be seen by the outside universe. The Schwarzchild radius is effectively the boundary of the black hole (its surface), and is called the event horizon. • The only things we can tell about the matter inside the black ...
ppt
... Consists of stars living out the “normal” part of their lives… Stars on MS produce energy via steady hydrogen burning (i.e., converting hydrogen into helium). Stars of different mass lie at different points on the main sequence. Mass-luminosity relation: L M4. ...
... Consists of stars living out the “normal” part of their lives… Stars on MS produce energy via steady hydrogen burning (i.e., converting hydrogen into helium). Stars of different mass lie at different points on the main sequence. Mass-luminosity relation: L M4. ...
ASTRONOMY 1102 1
... example of what the test will look like and a couple of examples of questions and problems. Review class notes: do not memorize rst, understand rst, and then commit to memory only a few basic de nitions and laws. Review homework. The basic properties of stars and the H{R diagram ARE NECESSARY BACK ...
... example of what the test will look like and a couple of examples of questions and problems. Review class notes: do not memorize rst, understand rst, and then commit to memory only a few basic de nitions and laws. Review homework. The basic properties of stars and the H{R diagram ARE NECESSARY BACK ...
White Dwarfs
... 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 to follow the story you will have to proceed with care, testing theories against evidence and answer four essential ...
... 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 to follow the story you will have to proceed with care, testing theories against evidence and answer four essential ...
19Nov_2014
... predictable curve – Initial brightness increase followed by a slowly decaying “tail” ...
... predictable curve – Initial brightness increase followed by a slowly decaying “tail” ...
Jeopardy Questions
... Q: Name 3 pieces of evidence for dark matter A: X-ray observations of hot gas in galaxy clusters, gravitational lensing from galaxy clusters, flat rotation curves of spiral galaxies ...
... Q: Name 3 pieces of evidence for dark matter A: X-ray observations of hot gas in galaxy clusters, gravitational lensing from galaxy clusters, flat rotation curves of spiral galaxies ...
The Milky Way - Houston Community College System
... learn that stars are born and grow old. Modern astronomers can tell the story of the stars right to the end. In this chapter you will learn how stars die, and as you follow the story you will see how astronomers have tested their hypotheses against evidence to ...
... learn that stars are born and grow old. Modern astronomers can tell the story of the stars right to the end. In this chapter you will learn how stars die, and as you follow the story you will see how astronomers have tested their hypotheses against evidence to ...
White Dwarfs
... 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 to follow the story you will have to proceed with care, testing theories against evidence and answer four essential ...
... 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 to follow the story you will have to proceed with care, testing theories against evidence and answer four essential ...
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.