Pretest
... inner solar system, most gases escaped the gravity of planets forming in this region, causing the inner planets to be rocky. The outer solar system, being farther from the sun, was cooler. As a result, planets forming in this region were able to capture gases and so became gas giants. ...
... inner solar system, most gases escaped the gravity of planets forming in this region, causing the inner planets to be rocky. The outer solar system, being farther from the sun, was cooler. As a result, planets forming in this region were able to capture gases and so became gas giants. ...
Blowing Bubbles in Space: The Birth and Death of Practically
... viewed end-on rather than a spherical bubble. • The intriguing result implies that the massive star's explosion has produced a shape similar to what is seen in some planetary nebulae associated with lower mass stars. • SMC=190 kly away, so this field of view spans about 150 light-years. ...
... viewed end-on rather than a spherical bubble. • The intriguing result implies that the massive star's explosion has produced a shape similar to what is seen in some planetary nebulae associated with lower mass stars. • SMC=190 kly away, so this field of view spans about 150 light-years. ...
Aging nearby spiral galaxies using H
... loss, spectral output, plasma/gas dynamics &c. » Different options to cover most types of conditions: ...
... loss, spectral output, plasma/gas dynamics &c. » Different options to cover most types of conditions: ...
Groups of Stars
... What makes a quasar so bright? The most likely explanation involves matter spiraling into a super-massive black hole with the mass of a billion suns. ...
... What makes a quasar so bright? The most likely explanation involves matter spiraling into a super-massive black hole with the mass of a billion suns. ...
Chapter 9 / Adobe Acrobat Document
... it. Students would likely use the library a lot more; they would not be able to communicate using e-mail or on-line communication websites, so they might have more face-to-face communication. 978Learning Check Answers (Student textbook page 379) 1. Dark matter is the most abundant form of matter in ...
... it. Students would likely use the library a lot more; they would not be able to communicate using e-mail or on-line communication websites, so they might have more face-to-face communication. 978Learning Check Answers (Student textbook page 379) 1. Dark matter is the most abundant form of matter in ...
Globular Cluster in Canes Venatici
... Distance: 35,000 light years Diameter: 214 light years Magnitude: 6.4 Angular Size: 21 minutes ...
... Distance: 35,000 light years Diameter: 214 light years Magnitude: 6.4 Angular Size: 21 minutes ...
Introduction to Galaxies and Cosmology Exercises 2
... c) What is the Schwarzschild radius of the black hole? 9. (Challenging) A quasar emits two radiating clouds in our general direction at 13/14 the speed of light. They are first observed when they appear to have been first produced at the central powerhouse, and are subsequently observed to move appa ...
... c) What is the Schwarzschild radius of the black hole? 9. (Challenging) A quasar emits two radiating clouds in our general direction at 13/14 the speed of light. They are first observed when they appear to have been first produced at the central powerhouse, and are subsequently observed to move appa ...
Outline 8: History of the Universe and Solar System
... • No, gravitational forces have slowed down the galaxies since the Big Bang. • (Note: Recent observations suggest this was the case for the first 2/3 of the Universe’s history. The expansion rate now seems to have increased for the last 1/3 of the Universe’s history. This is explained by “dark phant ...
... • No, gravitational forces have slowed down the galaxies since the Big Bang. • (Note: Recent observations suggest this was the case for the first 2/3 of the Universe’s history. The expansion rate now seems to have increased for the last 1/3 of the Universe’s history. This is explained by “dark phant ...
Presentazione di PowerPoint
... and gas is predominantly Keplerian (relativistic effects are minimal), with a component due to the combined gravitational potential of stars, dust, gas, dark matter, and anything else contributing mass to within that region. Beyond the sphere of influence, the gravitational dominance of the SMBH qui ...
... and gas is predominantly Keplerian (relativistic effects are minimal), with a component due to the combined gravitational potential of stars, dust, gas, dark matter, and anything else contributing mass to within that region. Beyond the sphere of influence, the gravitational dominance of the SMBH qui ...
Galaxy clusters - University of Iowa Astrophysics
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
guide to orion 3-d flythrough
... The central area of the nebula is called the Trapezium cluster. It is dominated by four young, massive stars in a kite-like arrangement. The brightest of these stars, which has a luminosity 100,000 times that of the Sun, provides the energy that creates the nebula as we see it. It produces a flood o ...
... The central area of the nebula is called the Trapezium cluster. It is dominated by four young, massive stars in a kite-like arrangement. The brightest of these stars, which has a luminosity 100,000 times that of the Sun, provides the energy that creates the nebula as we see it. It produces a flood o ...
Chapter 30 Review
... pulsation, astronomers can determine its luminosity and calculate how far away a variable star must be to appear as dim or as bright as it does. ...
... pulsation, astronomers can determine its luminosity and calculate how far away a variable star must be to appear as dim or as bright as it does. ...
Galaxy clusters - University of Iowa Astrophysics
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
... • From this, the amount of X-ray emitting gas can be calculated to be 2×1014 M • The mass of X-ray emitting gas is greater than the mass in all the stars in all the galaxies in the cluster and about 10% of the total mass. ...
Astro 10 Practice Test 3
... its core, what would we observe if we could look at the star from the outside? a. The intense energy from the `shell hydrogen burning’ would cause it to contract and cool off, moving down and to the left on the H-R diagram. b. This transition doesn’t actually have any visible effect on the surface o ...
... its core, what would we observe if we could look at the star from the outside? a. The intense energy from the `shell hydrogen burning’ would cause it to contract and cool off, moving down and to the left on the H-R diagram. b. This transition doesn’t actually have any visible effect on the surface o ...
Gas and dust evolution in distant AGN
... Chemical version of the cosmic downsizing (anti-hierarchical growth) Evolution of the Mass-Metallicity relation: massive galaxies chemically evolve rapidly at high-z QSOs ...
... Chemical version of the cosmic downsizing (anti-hierarchical growth) Evolution of the Mass-Metallicity relation: massive galaxies chemically evolve rapidly at high-z QSOs ...
ON THE TEMPERATURE STRUCTURE OF THE
... underestimated the extent of G0.253-0.016 along the observed line-of-sight, and so the true effective column of the cloud is much smaller than we are assuming in the fiducial models. However we find that similar environmental conditions are also required when we consider our lower-density version of ...
... underestimated the extent of G0.253-0.016 along the observed line-of-sight, and so the true effective column of the cloud is much smaller than we are assuming in the fiducial models. However we find that similar environmental conditions are also required when we consider our lower-density version of ...
Guide to Deep Space Poster PDF
... back in time. The light we can see left the stars and galaxies hundreds or even thousands of years ago. In fact, some of the stars we can see may not even be there any more. We live in a galaxy called the Milky Way, a vast flat spiral of hundreds of billions of stars. Our Sun and its family of plane ...
... back in time. The light we can see left the stars and galaxies hundreds or even thousands of years ago. In fact, some of the stars we can see may not even be there any more. We live in a galaxy called the Milky Way, a vast flat spiral of hundreds of billions of stars. Our Sun and its family of plane ...
Star Formation and Feedback II: The IMF and the SFR
... HCN 1–0 correlation for Galactic and extragalactic sources. Top: Linear least-squares fit for (with to LIR 1 104.5 L,; As mentioned earlier, the fact that we Galactic find star cores formation symbols above the associated dashed line) andthe forhigh galaxies, separately. Bottom: Overall be most inti ...
... HCN 1–0 correlation for Galactic and extragalactic sources. Top: Linear least-squares fit for (with to LIR 1 104.5 L,; As mentioned earlier, the fact that we Galactic find star cores formation symbols above the associated dashed line) andthe forhigh galaxies, separately. Bottom: Overall be most inti ...
Probing the first stars through the abundance of metal poor stars
... Five signatures of CMB-regulated star formation are: 1) Higher supernova rate than predicted at high redshift 2) Systematic discrepancy between direct and indirect measurements of the high redshift star formation rate 3)Lack of surviving globular clusters that formed at high metallicity and high red ...
... Five signatures of CMB-regulated star formation are: 1) Higher supernova rate than predicted at high redshift 2) Systematic discrepancy between direct and indirect measurements of the high redshift star formation rate 3)Lack of surviving globular clusters that formed at high metallicity and high red ...
Section 7.3 - CPO Science
... Figuring out the distance between galaxies is one of the more difficult tasks in astronomy. A faint object in the night sky could be a dim object that is relatively nearby or a bright object that is far, far away. ...
... Figuring out the distance between galaxies is one of the more difficult tasks in astronomy. A faint object in the night sky could be a dim object that is relatively nearby or a bright object that is far, far away. ...
HERE
... Since gas is more compact in a colder climate, it is easier for gravity to collapse it to form new stars. ...
... Since gas is more compact in a colder climate, it is easier for gravity to collapse it to form new stars. ...
The Origin of Stars
... gas is blown away, but its thermal energy comes from gravitational contraction, not fusion 4) The collapsing gas becomes a young stellar object with an accretion disk and jets 4) When the young stellar object begins fusing hydrogen into helium it becomes a true star ...
... gas is blown away, but its thermal energy comes from gravitational contraction, not fusion 4) The collapsing gas becomes a young stellar object with an accretion disk and jets 4) When the young stellar object begins fusing hydrogen into helium it becomes a true star ...
eneb_form
... • Here is a visual example of how it works. • We know the properties of the H-R diagram for the near by stars. ...
... • Here is a visual example of how it works. • We know the properties of the H-R diagram for the near by stars. ...
Infinity Express
... The information and activities presented in the Infinity Express Teacher’s Guide have been adapted for use and distribution by OMSI from the following: Smithsonian National Air and Space Museum GLOSSARY ...
... The information and activities presented in the Infinity Express Teacher’s Guide have been adapted for use and distribution by OMSI from the following: Smithsonian National Air and Space Museum GLOSSARY ...
origins of the Universe
... in the early 1900’s astronomers started to find evidence that pointed to a Big Bang. • In 1922, astronomer Edwin Hubble observed that the universe was expanding. The most distant galaxies he could see through his telescope were moving away at about 40 000 km per second. • This observation led to wha ...
... in the early 1900’s astronomers started to find evidence that pointed to a Big Bang. • In 1922, astronomer Edwin Hubble observed that the universe was expanding. The most distant galaxies he could see through his telescope were moving away at about 40 000 km per second. • This observation led to wha ...