The Sizes of Stars
... z Lower temperature means lower gas pressure z The lower gas pressure cannot hold up against gravity – the Sun shrinks z The added compression puts the Sun’s center under greater pressure, so the central temperature increases z The higher temperature produces higher pressure, which fights off gravit ...
... z Lower temperature means lower gas pressure z The lower gas pressure cannot hold up against gravity – the Sun shrinks z The added compression puts the Sun’s center under greater pressure, so the central temperature increases z The higher temperature produces higher pressure, which fights off gravit ...
Stellar Evolution
... Planetary nebula get their name because some looked like round, green planets in early telescopes. We now know that they are entirely different than the planets and are about one or more light years across (much larger than our solar system!). Many planetary nebulae will look like rings (for example ...
... Planetary nebula get their name because some looked like round, green planets in early telescopes. We now know that they are entirely different than the planets and are about one or more light years across (much larger than our solar system!). Many planetary nebulae will look like rings (for example ...
Biography of a Star - Max-Planck
... By the turn of the 20th century, astrophysicists had already gathered extensive data. For example, they had determined the masses of many stars; they knew their apparent and absolute (actual, independent of distance) brightnesses, their colors and surface temperatures, and their spectral types. In 1 ...
... By the turn of the 20th century, astrophysicists had already gathered extensive data. For example, they had determined the masses of many stars; they knew their apparent and absolute (actual, independent of distance) brightnesses, their colors and surface temperatures, and their spectral types. In 1 ...
Messing Up a Galaxy
... stars themselves are very rare indeed. This is because the spaces between the stars in a galaxy are typically very large compared with the stars' sizes. In our region of space, the distance from the Sun to its nearest stellar neighbour is about 29 million times the Sun's diameter! Our Milky Way Gala ...
... stars themselves are very rare indeed. This is because the spaces between the stars in a galaxy are typically very large compared with the stars' sizes. In our region of space, the distance from the Sun to its nearest stellar neighbour is about 29 million times the Sun's diameter! Our Milky Way Gala ...
Goal: To understand the lifetime of a star and how the
... the sun that we saw that the sun held itself up with a combination of gas pressure and radiation pressure (light has energy) • This was called “Hydrostatic Equilibrium” ...
... the sun that we saw that the sun held itself up with a combination of gas pressure and radiation pressure (light has energy) • This was called “Hydrostatic Equilibrium” ...
1. What is the HR diagram? 1a. The HR diagram is a plot of a star`s
... The explosive start to Helium burning in the core for low mass stars. On the horizontal branch, how is the star powered? What burns where? Helium burning in the core. No real shell burning at this stage. On the asymptotic giant branch (AGB), can you ever get a helium burning shell outside a hydrogen ...
... The explosive start to Helium burning in the core for low mass stars. On the horizontal branch, how is the star powered? What burns where? Helium burning in the core. No real shell burning at this stage. On the asymptotic giant branch (AGB), can you ever get a helium burning shell outside a hydrogen ...
lecture24
... If, after the nova, it does not shed all the mass it gained, it will continue to accrete mass until it novas again. If this process continues (accretion, nova, accretion, nova, etc.) such that the WD continues to gain mass, once it has a mass of 1.4Msun, the core will collapse, ...
... If, after the nova, it does not shed all the mass it gained, it will continue to accrete mass until it novas again. If this process continues (accretion, nova, accretion, nova, etc.) such that the WD continues to gain mass, once it has a mass of 1.4Msun, the core will collapse, ...
Stars and The Universe
... 18. When a massive star runs out of fuel and collapses on itself, its mass collides at its core and bounces back in an explosion called a ____________. As a result of this explosion, the outside layers of the massive star fly away into space, where they can form _____________. If the mass remaining ...
... 18. When a massive star runs out of fuel and collapses on itself, its mass collides at its core and bounces back in an explosion called a ____________. As a result of this explosion, the outside layers of the massive star fly away into space, where they can form _____________. If the mass remaining ...
Lecture 33
... • It probably took a billion or so years before galaxies to scale of the Milky Way could form ...
... • It probably took a billion or so years before galaxies to scale of the Milky Way could form ...
ppt - Wladimir Lyra
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
powerpoint
... What happens to white dwarfs? • Eventually the cool down and become black dwarfs. • And this is the ultimate fate of our sun and all stars more massive than a red dwarf but less than 4 times the mass of our sun. • Now for some pretty pictures (have you forgotten about all the ejected gas already?)! ...
... What happens to white dwarfs? • Eventually the cool down and become black dwarfs. • And this is the ultimate fate of our sun and all stars more massive than a red dwarf but less than 4 times the mass of our sun. • Now for some pretty pictures (have you forgotten about all the ejected gas already?)! ...
Birth, Lives, and Death of Stars
... left over from when the star was still producing energy from nuclear reactions. There are no more nuclear reactions occurring so the white dwarf cools off from an initial temperature of about 100,000 K. The white dwarf loses heat quickly at first cooling off to 20,000 K in only about 100 million yea ...
... left over from when the star was still producing energy from nuclear reactions. There are no more nuclear reactions occurring so the white dwarf cools off from an initial temperature of about 100,000 K. The white dwarf loses heat quickly at first cooling off to 20,000 K in only about 100 million yea ...
Stars and Galaxies
... Planetary Nebulae You read that lower-mass stars, such as the Sun, become white dwarfs. When a star becomes a white dwarf, it casts off hydrogen and helium gases in its outer layers. The expanding, cast-off matter of a white dwarf is a planetary nebula. Most of the star’s carbon remains locked in t ...
... Planetary Nebulae You read that lower-mass stars, such as the Sun, become white dwarfs. When a star becomes a white dwarf, it casts off hydrogen and helium gases in its outer layers. The expanding, cast-off matter of a white dwarf is a planetary nebula. Most of the star’s carbon remains locked in t ...
Faintest Star Cluster Yet Found on Outskirts of Milky Way | Globular
... that would far outshine this entire globular cluster." Muñoz spotted the minute object in observations of a mini galaxy orbiting the Milky Way called Ursa Minor. The photos were taken by the Canada-France-Hawaii Telescope on Hawaii's Mauna Kea peak. "I was looking at an old friend so to speak, the U ...
... that would far outshine this entire globular cluster." Muñoz spotted the minute object in observations of a mini galaxy orbiting the Milky Way called Ursa Minor. The photos were taken by the Canada-France-Hawaii Telescope on Hawaii's Mauna Kea peak. "I was looking at an old friend so to speak, the U ...
Integrative Studies 410 Our Place in the Universe
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
Neutron Stars
... B: They can only be found in star forming regions C: The total mass of the two pulsars must be more than 10 solar masses. D: Each of the pulsars was produced by a massive star that exploded in a Supernova event. ...
... B: They can only be found in star forming regions C: The total mass of the two pulsars must be more than 10 solar masses. D: Each of the pulsars was produced by a massive star that exploded in a Supernova event. ...
black hole - Purdue Physics
... • Far from the event horizon, a black hole exerts gravitational force according to Newton’s Law, just like any star of the same mass • Only at a distance of 3 Rs from the black hole will the gravity increase from what Newton’s Law predicts. – then one could eventually fall into the black hole, if yo ...
... • Far from the event horizon, a black hole exerts gravitational force according to Newton’s Law, just like any star of the same mass • Only at a distance of 3 Rs from the black hole will the gravity increase from what Newton’s Law predicts. – then one could eventually fall into the black hole, if yo ...
How the quasars (lower right) are different than brown dwarfs
... and V-I) for normal stars is indicated by the line marked "ZAMS Relation." Normal stars are clumped along this line. Stars significantly above this line are brighter than expected in U-V given their observed color in V-I. ...
... and V-I) for normal stars is indicated by the line marked "ZAMS Relation." Normal stars are clumped along this line. Stars significantly above this line are brighter than expected in U-V given their observed color in V-I. ...
M-Dwarf Planet Occurrence in the Era of K2
... This means only short-‐period planets (P < 30 days) with large transit depths can be detected. Nonetheless, new interes?ng targets are up for community proposal. i Fields 4 and 5 observa4ons run ...
... This means only short-‐period planets (P < 30 days) with large transit depths can be detected. Nonetheless, new interes?ng targets are up for community proposal. i Fields 4 and 5 observa4ons run ...
When will a neutron star collapse to a black hole?
... Neutron stars are the most extreme and fascinating objects known to exist in our universe: Such a star has a mass that is up to twice that of the sun but a radius of only a dozen kilometres: hence it has an enormous density, thousands of billions of times that of the densest element on Earth. An imp ...
... Neutron stars are the most extreme and fascinating objects known to exist in our universe: Such a star has a mass that is up to twice that of the sun but a radius of only a dozen kilometres: hence it has an enormous density, thousands of billions of times that of the densest element on Earth. An imp ...
Announcements
... • Pressure of “degenerate” electrons can only support so much mass before electron speed would = speed of light. Electrons get squeezed onto protons. ...
... • Pressure of “degenerate” electrons can only support so much mass before electron speed would = speed of light. Electrons get squeezed onto protons. ...