Stellar Evolution
... fuse helium into carbon and oxygen. The core cannot get hot enough to fuse carbon and oxygen, so when the helium runs out, fusion stops. The outer layers of the star are blown off, and you are left with a “white dwarf” which slowly cools off and grows dim, becoming a brown dwarf. ...
... fuse helium into carbon and oxygen. The core cannot get hot enough to fuse carbon and oxygen, so when the helium runs out, fusion stops. The outer layers of the star are blown off, and you are left with a “white dwarf” which slowly cools off and grows dim, becoming a brown dwarf. ...
Section 25.2 Stellar Evolution
... collapses into a red dwarf and forms a planetary nebula 8. blows up in a supernova explosion 9. does not form a red giant; collapses directly into a white dwarf ...
... collapses into a red dwarf and forms a planetary nebula 8. blows up in a supernova explosion 9. does not form a red giant; collapses directly into a white dwarf ...
ppt
... • How are heavy elements distributed through galaxies? • What are the progenitors of Type Ia SNe? • What is the effect of a low-metallicity environment on star formation and gas tracers? ...
... • How are heavy elements distributed through galaxies? • What are the progenitors of Type Ia SNe? • What is the effect of a low-metallicity environment on star formation and gas tracers? ...
Life Cycle of the Stars
... • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the dust and gas. ...
... • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the dust and gas. ...
PHYS 2410 General Astronomy Homework 7
... The energy emitted from the surface of a main sequence star is _____the energy generated in the core. a. ...
... The energy emitted from the surface of a main sequence star is _____the energy generated in the core. a. ...
Linking Asteroids and Meteorites through Reflectance Spectroscopy
... • White Dwarfs is the core left over when a star can no longer undergo fusion • Most white dwarfs are composed of carbon and oxygen • Very dense – Some have densities of 3 million grams per cubic centimeter – A teaspoon of a white dwarf would weigh as much as an elephant ...
... • White Dwarfs is the core left over when a star can no longer undergo fusion • Most white dwarfs are composed of carbon and oxygen • Very dense – Some have densities of 3 million grams per cubic centimeter – A teaspoon of a white dwarf would weigh as much as an elephant ...
Stellar Evolution after the Main Sequence
... White dwarfs grow smaller as their mass increases. (More gravity, but same pressure) ...
... White dwarfs grow smaller as their mass increases. (More gravity, but same pressure) ...
Ch 20-21 Review
... A) hypernova B) nova C) gamma ray burstar D) type I supernova E) type II supernova ...
... A) hypernova B) nova C) gamma ray burstar D) type I supernova E) type II supernova ...
Atypical thermonuclear supernovae from tidally crushed white dwarfs
... of 103 M . This fiducial capture rate may need to be modified for a number of reasons. The actual rate could be lower than that given by equation (4), even if the initial distribution were isotropic, if the loss cone orbits were depleted faster than they could be replenished (Frank & Rees 1976). If t ...
... of 103 M . This fiducial capture rate may need to be modified for a number of reasons. The actual rate could be lower than that given by equation (4), even if the initial distribution were isotropic, if the loss cone orbits were depleted faster than they could be replenished (Frank & Rees 1976). If t ...
Death of Stars with the Mass of 0.3
... collapsing continues until it is hot enough for heavier elements to fuse. If the red giant has only a mass of less than about 1.4 sun masses, the fusion stops after the helium in the core has been burned up. Due to gravitational pressure, the star gets compressed and becomes a white dwarf. The outer ...
... collapsing continues until it is hot enough for heavier elements to fuse. If the red giant has only a mass of less than about 1.4 sun masses, the fusion stops after the helium in the core has been burned up. Due to gravitational pressure, the star gets compressed and becomes a white dwarf. The outer ...
Science Olympiad - Department of Physics and Astronomy
... hydrogen in the core, they cool and begin to collapse Collapsing causes temperature to rise, igniting a shell of hydrogen around the core Star expands over 100 times its original size, core collapses further igniting helium fusion The surface of our sun might swallow the Earth when it becomes a red ...
... hydrogen in the core, they cool and begin to collapse Collapsing causes temperature to rise, igniting a shell of hydrogen around the core Star expands over 100 times its original size, core collapses further igniting helium fusion The surface of our sun might swallow the Earth when it becomes a red ...
Today Only, A New Exhibit: M,L, and T Dwarfs!
... filters can be used to measure band strength and tus give spectral types I-J is a good bet! ...
... filters can be used to measure band strength and tus give spectral types I-J is a good bet! ...
TYPES OF PLANETS AND STARS
... of rocks and/or other metals and they have a solid surface that makes them different from other planets that don’t have a solid surface. Terrestrial planets also have topological features such as valleys, volcanoes and craters. In our solar system there are four terrestrial planets and they are Merc ...
... of rocks and/or other metals and they have a solid surface that makes them different from other planets that don’t have a solid surface. Terrestrial planets also have topological features such as valleys, volcanoes and craters. In our solar system there are four terrestrial planets and they are Merc ...
Requiem for a Star
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
The Hertzsprung – Russell Diagram
... Very bright, red in color, very large, cool in temperature Brightness of stars are due to their enormous size ...
... Very bright, red in color, very large, cool in temperature Brightness of stars are due to their enormous size ...
The Life Cycles of Stars
... collapse inward and compact. This is the white dwarf stage. At this stage, the star’s matter is extremely dense. White dwarfs shine with a white-hot light. Once all of their energy is gone, they no longer emit light. The star has now reached the black dwarf phase in which it will forever remain. ...
... collapse inward and compact. This is the white dwarf stage. At this stage, the star’s matter is extremely dense. White dwarfs shine with a white-hot light. Once all of their energy is gone, they no longer emit light. The star has now reached the black dwarf phase in which it will forever remain. ...
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 ...
powerpoint - Physics @ IUPUI
... • This is done by radiation pressure and gas pressure (they counteract gravity). • But to keep this up requires the constant generation of energy in the core. ...
... • This is done by radiation pressure and gas pressure (they counteract gravity). • But to keep this up requires the constant generation of energy in the core. ...
Document
... What two things does the apparent (or perceived) brightness of an object depend on? How can this relationship be used to determine ...
... What two things does the apparent (or perceived) brightness of an object depend on? How can this relationship be used to determine ...
Handout 30
... outer hydrogen shell will emit more energy causing the star to expand to be a giant. ...
... outer hydrogen shell will emit more energy causing the star to expand to be a giant. ...
Rachel Henning
... Sun will start to run out. The helium will get squeezed. This will speed up the hydrogen burning. Our star will slowly puff into a red giant, which is a star that has exhausted it hydrogen and is burning helium fuel. It will eat all of the inner planets, even the Earth. Then the sun would burn into ...
... Sun will start to run out. The helium will get squeezed. This will speed up the hydrogen burning. Our star will slowly puff into a red giant, which is a star that has exhausted it hydrogen and is burning helium fuel. It will eat all of the inner planets, even the Earth. Then the sun would burn into ...
Starending jeopardy
... Once hydrogen is depleted it can no longer fuse hydrogen into helium. With no energy source to cause outware pressure the gravity is able to collapse the core and change the star’s structure. ...
... Once hydrogen is depleted it can no longer fuse hydrogen into helium. With no energy source to cause outware pressure the gravity is able to collapse the core and change the star’s structure. ...
Lecture 15 - Deaths of Stars, Supernovae
... • Core grows until it is too heavy to support itself • Core collapses, density increases, normal iron nuclei are converted into neutrons with the emission of neutrinos • Core collapse stops, neutron star is formed • Rest of the star collapses in on the core, but bounces off the new neutron star (als ...
... • Core grows until it is too heavy to support itself • Core collapses, density increases, normal iron nuclei are converted into neutrons with the emission of neutrinos • Core collapse stops, neutron star is formed • Rest of the star collapses in on the core, but bounces off the new neutron star (als ...