Final Revision 1] Complete the following
... 7. A concave mirror its focal length (vertex) is 10 cm, so its radius of curvature is 5 cm. --------------------------------------------------------------------------------------------------------------------8. The contact les is a very thin lens made of glass. -------------------------------------- ...
... 7. A concave mirror its focal length (vertex) is 10 cm, so its radius of curvature is 5 cm. --------------------------------------------------------------------------------------------------------------------8. The contact les is a very thin lens made of glass. -------------------------------------- ...
Galaxies
... distant star to similar close star. Large uncertainty. • Variable Stars, especially Cepheids, give small error during certain stages of star’s evolution it is nonstable. Luminosity varies with time ...
... distant star to similar close star. Large uncertainty. • Variable Stars, especially Cepheids, give small error during certain stages of star’s evolution it is nonstable. Luminosity varies with time ...
Galaxy Classification Much of modern extragalactic astronomy deals
... In this method, supergiant galaxies with well-developed bright spiral arms and bars have the Roman numeral I (like supergiant stars), and small, low-surface-brightness, irregular galaxies have the roman numeral V. Of course, since one doesn’t usually know a galaxy’s distance, it is somewhat difficul ...
... In this method, supergiant galaxies with well-developed bright spiral arms and bars have the Roman numeral I (like supergiant stars), and small, low-surface-brightness, irregular galaxies have the roman numeral V. Of course, since one doesn’t usually know a galaxy’s distance, it is somewhat difficul ...
The kinematics of Galaxies in Compact Groups
... agreement does not tell us much about the DM (outer halo). ...
... agreement does not tell us much about the DM (outer halo). ...
HR diagram
... The Hertzsprung-Russell diagram is an analytical tool for understanding the properties of stars. This diagram is a plot of stellar brightness (luminosity) versus stellar color (temperature). Brightness (luminosity) is plotted along the Y-axis; color (temperature) along the X-axis. The diagram is nam ...
... The Hertzsprung-Russell diagram is an analytical tool for understanding the properties of stars. This diagram is a plot of stellar brightness (luminosity) versus stellar color (temperature). Brightness (luminosity) is plotted along the Y-axis; color (temperature) along the X-axis. The diagram is nam ...
HI in Local Group Dwarf Galaxies
... to our detection limits, and these upper limits are lower than the HI mass of any known dwarf which has HI. • Dwarf galaxies at smaller galactocentric distances have less HI on average than those at larger distances. • The HI -distance trend supports data from simulations which suggest ram-pressure ...
... to our detection limits, and these upper limits are lower than the HI mass of any known dwarf which has HI. • Dwarf galaxies at smaller galactocentric distances have less HI on average than those at larger distances. • The HI -distance trend supports data from simulations which suggest ram-pressure ...
Kinematics of the Solar Neighborhood
... to u(v − va ), indicating that the velocity ellipsoid lies in the plane of the disk, but is not precisely oriented toward the galactic center. The angle between the long axis of the velocity ellipsoid and the R direction is called the longitude of vertex, !v. Results for a wide range of stellar type ...
... to u(v − va ), indicating that the velocity ellipsoid lies in the plane of the disk, but is not precisely oriented toward the galactic center. The angle between the long axis of the velocity ellipsoid and the R direction is called the longitude of vertex, !v. Results for a wide range of stellar type ...
test - Scioly.org
... a. How long is its period in years? b. Consider the points A, B, C, D on the orbit of the object. The arc length from point A to point B is .225 AU. The arc length from point C to D is .556 AU. How much time does it take the object to move from point A to point B compared to the time it takes to get ...
... a. How long is its period in years? b. Consider the points A, B, C, D on the orbit of the object. The arc length from point A to point B is .225 AU. The arc length from point C to D is .556 AU. How much time does it take the object to move from point A to point B compared to the time it takes to get ...
transcript
... million meters. Soon the Earth will show as a solid sphere. We are able to see the whole Earth now, just over a minute along the journey. The Earth diminishes into the distance but those background stars are so much farther away that they do not yet appear to move. A line extends at the true speed o ...
... million meters. Soon the Earth will show as a solid sphere. We are able to see the whole Earth now, just over a minute along the journey. The Earth diminishes into the distance but those background stars are so much farther away that they do not yet appear to move. A line extends at the true speed o ...
Unit 1 - mmRyan
... million meters. Soon the Earth will show as a solid sphere. We are able to see the whole Earth now, just over a minute along the journey. The Earth diminishes into the distance but those background stars are so much farther away that they do not yet appear to move. A line extends at the true speed o ...
... million meters. Soon the Earth will show as a solid sphere. We are able to see the whole Earth now, just over a minute along the journey. The Earth diminishes into the distance but those background stars are so much farther away that they do not yet appear to move. A line extends at the true speed o ...
CHP 15
... a. they did not count the brightest stars. b. they did not study the southern sky. c. they did not have large enough telescopes. d. they only observed stars in the disk of the galaxy and not the halo. e. they did not know about interstellar dust clouds. 2. Which of the following is not a characteris ...
... a. they did not count the brightest stars. b. they did not study the southern sky. c. they did not have large enough telescopes. d. they only observed stars in the disk of the galaxy and not the halo. e. they did not know about interstellar dust clouds. 2. Which of the following is not a characteris ...
ausac_cjs_2008_1
... HI from Black-hole Host Galaxies Ho, Darling and Greene have made a large survey of 154 nearby Type-1 (broad-lined) AGNs whose black-hole masses and accretion rates are known. This enables them to constrain a number of properties of relevance to the relationship between BHs and their hosts. HI was ...
... HI from Black-hole Host Galaxies Ho, Darling and Greene have made a large survey of 154 nearby Type-1 (broad-lined) AGNs whose black-hole masses and accretion rates are known. This enables them to constrain a number of properties of relevance to the relationship between BHs and their hosts. HI was ...
D109-08x
... In Cycle 17 of HST we request a small amount of time to obtain high resolution imaging of this collection of knots in as many filters as practical. Having a better photometric characterization of the knots over a broader color baseline than obtainable from the ground coupled with higher resolution i ...
... In Cycle 17 of HST we request a small amount of time to obtain high resolution imaging of this collection of knots in as many filters as practical. Having a better photometric characterization of the knots over a broader color baseline than obtainable from the ground coupled with higher resolution i ...
Slide 1
... Milky Way But the solution to this is even more confusing. If we make a graph of how fast stars in the arms move compared to distance, we get line “B”. The fact that all the stars go the same speed explains why the spiral arms don’t twist up, but it doesn’t make sense. According to physics, the spe ...
... Milky Way But the solution to this is even more confusing. If we make a graph of how fast stars in the arms move compared to distance, we get line “B”. The fact that all the stars go the same speed explains why the spiral arms don’t twist up, but it doesn’t make sense. According to physics, the spe ...
PH607lec11
... Another question is why, if all galaxies are mergers of smaller ones, many of them don't look it. Beautiful spiral galaxies, for instance, appear neat and symmetrical, not as though they were formed from violent collisions of multiple smaller galaxies. Merging galaxies look like train wrecks. Maybe ...
... Another question is why, if all galaxies are mergers of smaller ones, many of them don't look it. Beautiful spiral galaxies, for instance, appear neat and symmetrical, not as though they were formed from violent collisions of multiple smaller galaxies. Merging galaxies look like train wrecks. Maybe ...
Photometry – I. “All sky”
... years, you might not even be able to get the same glass that was used previously. Detectors are also not really uniform; CCDs are much more red-sensitive than photomultipliers and different types (of either) might have significantly different responses as a function of wavelength. At the same time, ...
... years, you might not even be able to get the same glass that was used previously. Detectors are also not really uniform; CCDs are much more red-sensitive than photomultipliers and different types (of either) might have significantly different responses as a function of wavelength. At the same time, ...
PH607 – Galaxies
... Another question is why, if all galaxies are mergers of smaller ones, many of them don't look it. Beautiful spiral galaxies, for instance, appear neat and symmetrical, not as though they were formed from violent collisions of multiple smaller galaxies. Merging galaxies look like train wrecks. Maybe ...
... Another question is why, if all galaxies are mergers of smaller ones, many of them don't look it. Beautiful spiral galaxies, for instance, appear neat and symmetrical, not as though they were formed from violent collisions of multiple smaller galaxies. Merging galaxies look like train wrecks. Maybe ...
astro-ph/0504597 PDF
... The fundamental aim of cosmology (the science of study of the Universe as a whole) is to test its theoretical models against observations. Today, all most all the cosmological observations come from cosmic microwave background and supernovae. Supernovae are the tools at hand(!) for measuring the uni ...
... The fundamental aim of cosmology (the science of study of the Universe as a whole) is to test its theoretical models against observations. Today, all most all the cosmological observations come from cosmic microwave background and supernovae. Supernovae are the tools at hand(!) for measuring the uni ...
The Milky Way: Spiral galaxies:
... black hole or starburst or nuclear star cluster –! Stellar halo: very low surface brightness (few % of the total light), metal poor stars, GCs, low-density hot gas, little/no rotation –! Dark halo: dominates mass (and gravitational potential) outside ~10kpc, nature unknown? ...
... black hole or starburst or nuclear star cluster –! Stellar halo: very low surface brightness (few % of the total light), metal poor stars, GCs, low-density hot gas, little/no rotation –! Dark halo: dominates mass (and gravitational potential) outside ~10kpc, nature unknown? ...
Black Holes - Troy University
... – 1 Big BH per galaxy (~ million-billion solar masses) – millions of little BHs per galaxy ( ~ solar mass) BHs are responsible for the most dramatic and energetic phenomena in the universe – BHs are “seen” via the light produced by infalling gas & the gravitational pull that they exert on nearby obj ...
... – 1 Big BH per galaxy (~ million-billion solar masses) – millions of little BHs per galaxy ( ~ solar mass) BHs are responsible for the most dramatic and energetic phenomena in the universe – BHs are “seen” via the light produced by infalling gas & the gravitational pull that they exert on nearby obj ...
1 - Università degli Studi dell`Insubria
... >K is typically positive, but the eccentricity evoution of the binary is modest >MBHB-star interactions flatten the stellar distribution >Interacting stars typically corotate with the MBHB >A mass of the order of 0.7M is ejected from the bulge on nearly radial corotating orbits in the MBHB plane >LI ...
... >K is typically positive, but the eccentricity evoution of the binary is modest >MBHB-star interactions flatten the stellar distribution >Interacting stars typically corotate with the MBHB >A mass of the order of 0.7M is ejected from the bulge on nearly radial corotating orbits in the MBHB plane >LI ...
EarthComm_c1s9
... interesting, but they also show scientists what the fate of our solar system will be billions of years from now. What would happen if there were a supernova explosion in our stellar neighborhood some time in the future? Depending on how close it was, you could be bombarded with strong radiation and ...
... interesting, but they also show scientists what the fate of our solar system will be billions of years from now. What would happen if there were a supernova explosion in our stellar neighborhood some time in the future? Depending on how close it was, you could be bombarded with strong radiation and ...
Expected Coalescence Rate of NS/NS Binaries for Laser Beam
... NS : fraction of massive binaries that remain bounded after the second supernova P( ): probability for a newly formed NS/NS to coalesce in a timescale 0 : minimum coalescence time * : mean timescale required for the newly formed massive system to evolve into two NSs ...
... NS : fraction of massive binaries that remain bounded after the second supernova P( ): probability for a newly formed NS/NS to coalesce in a timescale 0 : minimum coalescence time * : mean timescale required for the newly formed massive system to evolve into two NSs ...
astronomy practice test ch 9
... ____ 12. The absolute magnitude of a star is the apparent magnitude it would have if it were 10 pc from Earth. ____ 13. Lines in the spectra of supergiant stars are broader than the same spectral lines in main sequence stars of the same spectral type. ____ 14. Giant stars are members of luminosity c ...
... ____ 12. The absolute magnitude of a star is the apparent magnitude it would have if it were 10 pc from Earth. ____ 13. Lines in the spectra of supergiant stars are broader than the same spectral lines in main sequence stars of the same spectral type. ____ 14. Giant stars are members of luminosity c ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.