Star Life Cycle Web Activity
... of a Star. Read the web page and the summary of a typical cycle of stars given here. Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then condensing (shrinking) because of gravity, making the core more dense and hotter…so hot that now a new element c ...
... of a Star. Read the web page and the summary of a typical cycle of stars given here. Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then condensing (shrinking) because of gravity, making the core more dense and hotter…so hot that now a new element c ...
Sunspots - Sage Middle School
... Radiative Diffusion The photons “diffuse” outwards, heating the gas as they go. ...
... Radiative Diffusion The photons “diffuse” outwards, heating the gas as they go. ...
Leaving the Main Sequence
... 3. Red giant – Core begins to run out of hydrogen fuel, begins to contract and heats. Remaining hydrogen burns faster in the shell around core and generates extra energy, disrupting hydrostatic equilibrium and causing outer regions to expand and cool. Star turns red. – Core (helium) becomes a degene ...
... 3. Red giant – Core begins to run out of hydrogen fuel, begins to contract and heats. Remaining hydrogen burns faster in the shell around core and generates extra energy, disrupting hydrostatic equilibrium and causing outer regions to expand and cool. Star turns red. – Core (helium) becomes a degene ...
Luminosity - U of L Class Index
... • Any star that varies significantly in brightness with time is called a variable star • Some stars vary in brightness because they cannot achieve proper balance between power welling up from the core and power radiated from the surface • Such a star alternately expands and contracts, varying in bri ...
... • Any star that varies significantly in brightness with time is called a variable star • Some stars vary in brightness because they cannot achieve proper balance between power welling up from the core and power radiated from the surface • Such a star alternately expands and contracts, varying in bri ...
Chapter 8 – Continuous Absorption
... • Absorption coefficient depends on the speed of the electron (slower electrons are more likely to absorb a photon because their encounters with H atoms take longer) • Adopt a Maxwell-Boltzman distribution for the speed of electrons • Again multiply by the number of neutral hydrogen atoms: log e I ...
... • Absorption coefficient depends on the speed of the electron (slower electrons are more likely to absorb a photon because their encounters with H atoms take longer) • Adopt a Maxwell-Boltzman distribution for the speed of electrons • Again multiply by the number of neutral hydrogen atoms: log e I ...
Variable Stars
... Quasars: give off radio & X-waves. They are the most distant objects in space. Give off tremendous amounts of energy. Quasars give off enormous amounts of energy - they can be a trillion times brighter than the Sun! Quasars are believed to produce their energy from massive black holes in the center ...
... Quasars: give off radio & X-waves. They are the most distant objects in space. Give off tremendous amounts of energy. Quasars give off enormous amounts of energy - they can be a trillion times brighter than the Sun! Quasars are believed to produce their energy from massive black holes in the center ...
Stars and Their Life Cycles
... • all are parts of a binary system (two stars orbit around one another) • possible that brown dwarfs represent a lot of the mass in the universe ...
... • all are parts of a binary system (two stars orbit around one another) • possible that brown dwarfs represent a lot of the mass in the universe ...
After the ZAMS - Lincoln-Sudbury Regional High School
... matter-to-energy conversion in their cores. However the stellar winds are a much more serious source of mass loss. These winds commence as soon as a molecular cloud starts to heat up. But the effect really becomes important when fusion starts in the core. ...
... matter-to-energy conversion in their cores. However the stellar winds are a much more serious source of mass loss. These winds commence as soon as a molecular cloud starts to heat up. But the effect really becomes important when fusion starts in the core. ...
I. Stars - SharpSchool
... Stars The Brightness of Stars -Star: A luminous sphere of gas with enormous mass, that produces energy by fusion. -Fusion: The joining of separate nuclei. Common in nature, but not on Earth. ...
... Stars The Brightness of Stars -Star: A luminous sphere of gas with enormous mass, that produces energy by fusion. -Fusion: The joining of separate nuclei. Common in nature, but not on Earth. ...
How stars form slide show File
... Summary – The birth of stars •Huge amounts of gas and dust from nebulae are slowly drawn together over millions of years by gravity. •As the gas compresses it changes its gravitational potential energy changes into kinetic energy. •The KE changes into heat and the protostar becomes hotter and hotte ...
... Summary – The birth of stars •Huge amounts of gas and dust from nebulae are slowly drawn together over millions of years by gravity. •As the gas compresses it changes its gravitational potential energy changes into kinetic energy. •The KE changes into heat and the protostar becomes hotter and hotte ...
The ISM and Stellar Birth
... start to collapse under their own gravity • As gas molecules fall in, their speed increases • They collide with other molecules and randomize their speeds • Temperature is just a measure of how fast, on average, the random motion of molecules is • So as the cloud collapses, its temperature increases ...
... start to collapse under their own gravity • As gas molecules fall in, their speed increases • They collide with other molecules and randomize their speeds • Temperature is just a measure of how fast, on average, the random motion of molecules is • So as the cloud collapses, its temperature increases ...
Time From the Perspective of a Particle Physicist
... 2. Protostar: hot ball but no fusion 3. Star: nuclear fusion but not final equilibrium 4. Main Sequence Star: final equilibrium with excess gas blown away ...
... 2. Protostar: hot ball but no fusion 3. Star: nuclear fusion but not final equilibrium 4. Main Sequence Star: final equilibrium with excess gas blown away ...
Unit 1
... hydrogen into helium is called its main sequence lifetime – Stars spend most of their lives on the main sequence – Lifetime depends on the star’s mass and luminosity • More luminous stars burn their energy more rapidly than less luminous stars. • High-mass stars are more luminous than low-mass stars ...
... hydrogen into helium is called its main sequence lifetime – Stars spend most of their lives on the main sequence – Lifetime depends on the star’s mass and luminosity • More luminous stars burn their energy more rapidly than less luminous stars. • High-mass stars are more luminous than low-mass stars ...
Star Formation
... As an individual “proto-star’ lump contracts, it slowly heats up. It glows first in the infrared, and only later in visible light (as it gets progressively hotter). On the other hand, such a proto-star is quite big to begin with. So it can emit quite a lot of red and infrared light! But it will grad ...
... As an individual “proto-star’ lump contracts, it slowly heats up. It glows first in the infrared, and only later in visible light (as it gets progressively hotter). On the other hand, such a proto-star is quite big to begin with. So it can emit quite a lot of red and infrared light! But it will grad ...
Chapter 10 powerpoint presentation
... Then the gas law becomes, P(r) = r(r) k T(r) / mH, With the understanding that is the average mass of an atom, in units of the hydrogen mass, so that the average mass of a stellar atom is m, where m = mH ...
... Then the gas law becomes, P(r) = r(r) k T(r) / mH, With the understanding that is the average mass of an atom, in units of the hydrogen mass, so that the average mass of a stellar atom is m, where m = mH ...
Unit 1 The Universe
... • Stars form in nebulae. • Nebula -large cloud of gas and dust. It is composed mainly of hydrogen and helium, with small amounts of heavier elements. ...
... • Stars form in nebulae. • Nebula -large cloud of gas and dust. It is composed mainly of hydrogen and helium, with small amounts of heavier elements. ...
Hydrostatic equilibrium : no large scale acceleration of the same
... Opacity described by Opacity Distribution Function or Opacity Sampling NLTE represents, at its best, the interaction between matter and radiation NLTE is present – at some point – in every stellar atmosphere To have LTE, the net collisional rate in every atomic transition must be larger than the net ...
... Opacity described by Opacity Distribution Function or Opacity Sampling NLTE represents, at its best, the interaction between matter and radiation NLTE is present – at some point – in every stellar atmosphere To have LTE, the net collisional rate in every atomic transition must be larger than the net ...
Name: Astronomy Lab: The Hertzsprung-Russell (H
... Sometimes the student of astronomy starts to become overwhelmed trying to understand the many measurements and observations astronomers make. Data concerning distance, brightness, color, spectral class, mass, temperature, motion, etc. all seem to be gathered in an attempt to impress the student with ...
... Sometimes the student of astronomy starts to become overwhelmed trying to understand the many measurements and observations astronomers make. Data concerning distance, brightness, color, spectral class, mass, temperature, motion, etc. all seem to be gathered in an attempt to impress the student with ...
Homework 1
... can pull in more dust from the surrounding cloud, and this cycle continues. At some point the density and temperature reach a point where hydrogen starts to fuse into helium. From the fusion process many photons are produced and this in turn creates radiation pressure outwards that balances the forc ...
... can pull in more dust from the surrounding cloud, and this cycle continues. At some point the density and temperature reach a point where hydrogen starts to fuse into helium. From the fusion process many photons are produced and this in turn creates radiation pressure outwards that balances the forc ...
7/3 Some stars were found in regions above the main sequence
... Stars are born as a result of the gravitational contraction of the interstellar medium. Today there are four types of interstellar medium: 1. HII Regions — hydrogen, helium, and dust — Hot bright stars in the region ionize the gas — emit light when electrons recombine with ions — hot and low density ...
... Stars are born as a result of the gravitational contraction of the interstellar medium. Today there are four types of interstellar medium: 1. HII Regions — hydrogen, helium, and dust — Hot bright stars in the region ionize the gas — emit light when electrons recombine with ions — hot and low density ...
Compact Extragalactic Star Formation
... Linear Resolution ~ 2-4 pc NLyc 7 1052 s-1 Super star clusters From KJ ...
... Linear Resolution ~ 2-4 pc NLyc 7 1052 s-1 Super star clusters From KJ ...
Chapter 14
... wave that causes particles to move closer together into a growing cluster and as the mass increases the gravitational attraction of the particles for each other increases. • Eventually you end up with a protostar, an accumulation of gases that will form a star. ...
... wave that causes particles to move closer together into a growing cluster and as the mass increases the gravitational attraction of the particles for each other increases. • Eventually you end up with a protostar, an accumulation of gases that will form a star. ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... light-emitting body would exceed the body's gravitational attraction. That is, a body emitting radiation at greater than the Eddington limit would break up from its own photon pressure (see class derivation). ...
... light-emitting body would exceed the body's gravitational attraction. That is, a body emitting radiation at greater than the Eddington limit would break up from its own photon pressure (see class derivation). ...
L11
... light-emitting body would exceed the body's gravitational attraction. That is, a body emitting radiation at greater than the Eddington limit would break up from its own photon pressure (see class derivation). ...
... light-emitting body would exceed the body's gravitational attraction. That is, a body emitting radiation at greater than the Eddington limit would break up from its own photon pressure (see class derivation). ...
Stellar Evolution
... 18. What does the core of a star at the end of being a main sequence star look like ? ...
... 18. What does the core of a star at the end of being a main sequence star look like ? ...