Astronomy Chapter 13 Name
... L. A star whose luminosity changes in time M. The region in the H-R diagram in which most stars are located N. A dense star whose radius is approximately equal to Earth’s but whose mass is comparable to the Sun’s O. Two stars in orbit around each other, held together by their mutual gravity P. A pai ...
... L. A star whose luminosity changes in time M. The region in the H-R diagram in which most stars are located N. A dense star whose radius is approximately equal to Earth’s but whose mass is comparable to the Sun’s O. Two stars in orbit around each other, held together by their mutual gravity P. A pai ...
Unit XII Study Guide
... ____ 22. What is a pulsar? a. the remains of a low-mass star after it explodes b. a spinning neutron star emitting radio waves c. another name for a protostar d. the stage before a dying star becomes a supernova ...
... ____ 22. What is a pulsar? a. the remains of a low-mass star after it explodes b. a spinning neutron star emitting radio waves c. another name for a protostar d. the stage before a dying star becomes a supernova ...
The Interstellar Medium and Star Formation
... pebbles, then rocks, then boulders, then planetesimals, then planets. Some planets become massive enough to also accumulate Hydrogen and Helium gas. • However, during and after formation, it seems that some planets are able to migrate in their disks, drifting inwards to settle close to the star. We ...
... pebbles, then rocks, then boulders, then planetesimals, then planets. Some planets become massive enough to also accumulate Hydrogen and Helium gas. • However, during and after formation, it seems that some planets are able to migrate in their disks, drifting inwards to settle close to the star. We ...
Stars Notes - Yonkers Public Schools
... • Very luminous • Low Temperature • Late evolution of medium-sized main sequence stars when they greatly expand in size ...
... • Very luminous • Low Temperature • Late evolution of medium-sized main sequence stars when they greatly expand in size ...
Life Cycles of Stars
... Why Black-Body Radiation is so Important • Color is directly related to temperature • Temperature is the only determinant of color • Energy per unit area is the same if temperature is the same – If two stars have the same color and distance, difference in brightness is due to difference in size – D ...
... Why Black-Body Radiation is so Important • Color is directly related to temperature • Temperature is the only determinant of color • Energy per unit area is the same if temperature is the same – If two stars have the same color and distance, difference in brightness is due to difference in size – D ...
HR-Diagram
... This time there is so much energy because of the large mass of the outer star that the collapse causes a Super Nova Explosion. NOW…if the CORE of the star has a mass of 3x or less the size of the sun ( but has a much smaller diameter than the sun) it creates a Neutron Star which spins and emits a st ...
... This time there is so much energy because of the large mass of the outer star that the collapse causes a Super Nova Explosion. NOW…if the CORE of the star has a mass of 3x or less the size of the sun ( but has a much smaller diameter than the sun) it creates a Neutron Star which spins and emits a st ...
Wednesday, November 7, 2007
... Suppose you could represent the age of the solar system, so far, by one calendar year. Then 1 day would represent about 13 million years. ...
... Suppose you could represent the age of the solar system, so far, by one calendar year. Then 1 day would represent about 13 million years. ...
Document
... the star per second) are the basic properties of a star • Magnitude: how bright the star appears; +1 was the brightest star, +2 was the next brightest star, +3 was the third brightest star • Absolute magnitude: takes into account distance and measures how bright a star would appear if they all were ...
... the star per second) are the basic properties of a star • Magnitude: how bright the star appears; +1 was the brightest star, +2 was the next brightest star, +3 was the third brightest star • Absolute magnitude: takes into account distance and measures how bright a star would appear if they all were ...
The night sky in October and November
... Messier. M31 is a Messier object. Time-elapse photos through a large telescope reveal it as a spiral galaxy about four times the width of the full moon. It is the most distant object you can see without optical aids. The stars that make up the constellation of Andromeda are in the Milky Way. That’s ...
... Messier. M31 is a Messier object. Time-elapse photos through a large telescope reveal it as a spiral galaxy about four times the width of the full moon. It is the most distant object you can see without optical aids. The stars that make up the constellation of Andromeda are in the Milky Way. That’s ...
Slide 1 - Beverley High School
... • These high mass stars finish their lives in massive supernova explosions • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
... • These high mass stars finish their lives in massive supernova explosions • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
iClicker Questions
... The shockwave from a nearby supernova b) The shockwave from a newly formed high-mass star that is nearby c) The shockwave experienced by the cloud as it passes through a spiral arm d) All of the above ...
... The shockwave from a nearby supernova b) The shockwave from a newly formed high-mass star that is nearby c) The shockwave experienced by the cloud as it passes through a spiral arm d) All of the above ...
Cosmic Distance Ladder
... Note that beyond the Virgo cluster, even very bright stars like Cepheids become unresolved and we see only the integrated light from galaxies. Further away than this, we must determine distances using the redshift of galaxies. ...
... Note that beyond the Virgo cluster, even very bright stars like Cepheids become unresolved and we see only the integrated light from galaxies. Further away than this, we must determine distances using the redshift of galaxies. ...
Why is there a main sequence?
... become giant stars. Here you will answer four important questions: • Why is there a main sequence? • Why is there a relationship between the masses and luminosities of main-sequence stars? • How does a star change as it exhausts its hydrogen fusion fuel? • What is the evidence that stars really do e ...
... become giant stars. Here you will answer four important questions: • Why is there a main sequence? • Why is there a relationship between the masses and luminosities of main-sequence stars? • How does a star change as it exhausts its hydrogen fusion fuel? • What is the evidence that stars really do e ...
photons.
... random directions. Photons of other wavelengths go through. Get dark absorption line at green part of spectrum. ...
... random directions. Photons of other wavelengths go through. Get dark absorption line at green part of spectrum. ...
HW8 - UCSB Physics
... Taking the square root of both sides shows that v = .6c 21.36)Let us start with the Lorentz length contraction formula which is given as r v2 L = L0 1 − 2 c Setting L = .6m and L0 = 1m, we have r v2 ...
... Taking the square root of both sides shows that v = .6c 21.36)Let us start with the Lorentz length contraction formula which is given as r v2 L = L0 1 − 2 c Setting L = .6m and L0 = 1m, we have r v2 ...
HR Diagram and Life of a star
... from 100-1000 times the size of the sun GIANTS- large bright stars a bit smaller and fainter than Super giants Super giants in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium into Carbon. White Dwarfs- are the small, dense remains of low ...
... from 100-1000 times the size of the sun GIANTS- large bright stars a bit smaller and fainter than Super giants Super giants in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium into Carbon. White Dwarfs- are the small, dense remains of low ...
General Introduction 1. Luminosity, Flux and Magnitude The
... The evolution of the Sun is shown schematically in Fig. 7.3. The red giant phase occurs after the interior of the Sun is exhausted of hydrogen and helium burning initiates. The Sun is not massive enough to burn elements beyond He, so after shedding roughly half its mass in a violent wind leading to ...
... The evolution of the Sun is shown schematically in Fig. 7.3. The red giant phase occurs after the interior of the Sun is exhausted of hydrogen and helium burning initiates. The Sun is not massive enough to burn elements beyond He, so after shedding roughly half its mass in a violent wind leading to ...
File
... 1.They can react to their environment. 2.They can grow by taking in nourishment and processing it into energy. 3.They can reproduce, passing along their characteristics to their offspring. 4.They have the capacity for genetic change & can therefore evolve from generation to generation & adapt to a c ...
... 1.They can react to their environment. 2.They can grow by taking in nourishment and processing it into energy. 3.They can reproduce, passing along their characteristics to their offspring. 4.They have the capacity for genetic change & can therefore evolve from generation to generation & adapt to a c ...
Name: Period : _____ Bulldog Review #9 1. The Milky Wa
... hydrogen into helium, releasing energy. ...
... hydrogen into helium, releasing energy. ...
Foundation 1 - Discovering Astronomy
... – H2 (mostly), CO, H2O, NH3, H2CO – Most is concentrated in giant molecular clouds ...
... – H2 (mostly), CO, H2O, NH3, H2CO – Most is concentrated in giant molecular clouds ...
solution
... statistical mechanics. Combined with this is the rapid pace of development in computational physics and the computing power that can fit in the palm of your hand – we can now simulate much of stellar evolution to make predictions about what we observe. This allows us to more than speculate about the ...
... statistical mechanics. Combined with this is the rapid pace of development in computational physics and the computing power that can fit in the palm of your hand – we can now simulate much of stellar evolution to make predictions about what we observe. This allows us to more than speculate about the ...