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Astronomy 350 Fall 2011 Homework #1
... of an ordinary baseball (r = 1.5 inches = 4 cm). In this “shrunken” solar system, find the radius of the proportionally shrink-rayed Earth (ordinary radius REarth = 6400 km). Draw to scale a sketch of this shrunken Earth (you may also sketch Dr. Evil if you so choose). Include the Sun on your drawin ...
... of an ordinary baseball (r = 1.5 inches = 4 cm). In this “shrunken” solar system, find the radius of the proportionally shrink-rayed Earth (ordinary radius REarth = 6400 km). Draw to scale a sketch of this shrunken Earth (you may also sketch Dr. Evil if you so choose). Include the Sun on your drawin ...
Things to know: This meant as a guide to what you should know. I
... The speed of light is the same for all inertial reference frames. What unusual distortions in time and space are experienced when one moves at speeds near the speed of light? What is gravity in Einstein’s general theory of relativity? What is all matter made of (what are leptons, baryons, quarks)? W ...
... The speed of light is the same for all inertial reference frames. What unusual distortions in time and space are experienced when one moves at speeds near the speed of light? What is gravity in Einstein’s general theory of relativity? What is all matter made of (what are leptons, baryons, quarks)? W ...
Linking Asteroids and Meteorites through Reflectance
... • At the dawn of the 20th century, most astronomers thought that the Milky Way Galaxy was the universe, and it measured only a few thousand light-years across. ...
... • At the dawn of the 20th century, most astronomers thought that the Milky Way Galaxy was the universe, and it measured only a few thousand light-years across. ...
Type Ia supernovae and the ESSENCE supernova survey
... (red), ESSENCE objects (black) and 1st year of Legacy SN search (blue). ...
... (red), ESSENCE objects (black) and 1st year of Legacy SN search (blue). ...
COMING EVENTS The Pluto Files Volume 37 Number 03 March
... There are finder charts for each of the challenges but they have different fields-of-view for different objects. Challenge 14, a naked eye challenge, asks you to find Barnard’s Loop and the chart associated with this challenge shows the entire Orion constellation, so the chart in the book is probabl ...
... There are finder charts for each of the challenges but they have different fields-of-view for different objects. Challenge 14, a naked eye challenge, asks you to find Barnard’s Loop and the chart associated with this challenge shows the entire Orion constellation, so the chart in the book is probabl ...
ASTRONOMY WEBQUEST…… EXPLORE THE UNIVERSE
... Date February 23, 2012 Answer all of the questions by typing them on this document. Save your work and then attach this document to an e-mail to me. I am Mr. Aguilar, your 8th grade science teacher. 1. If your home is your universe, how would you like your home to be? Would you like your home to be ...
... Date February 23, 2012 Answer all of the questions by typing them on this document. Save your work and then attach this document to an e-mail to me. I am Mr. Aguilar, your 8th grade science teacher. 1. If your home is your universe, how would you like your home to be? Would you like your home to be ...
Astronomy and Space Science
... http://www2.enel.ucalgary.ca/People/ciubotar/public_html/Starsevol/specbin-anim.gif ...
... http://www2.enel.ucalgary.ca/People/ciubotar/public_html/Starsevol/specbin-anim.gif ...
update : Feb.27,2014
... There are more than 20 and may be as many as 30 physical or cosmological parameters that require very precise calibration in order to produce a life sustaining universe. Probably the most precise of all is the cosmological constant (energy density of empty space) has to be set to 1 part in 1053 or ...
... There are more than 20 and may be as many as 30 physical or cosmological parameters that require very precise calibration in order to produce a life sustaining universe. Probably the most precise of all is the cosmological constant (energy density of empty space) has to be set to 1 part in 1053 or ...
PC2491 Examples 2
... An H1 cloud in the galactic plane at l=30o is observed to have a velocity relative to the local standard of rest of +80 km s-1. Assume the galactic rotation curve is flat with an amplitude of 220 km s-1 , and that Ro = 8.2 kpc and estimate the two possible distances to this cloud. (4) Estimate the m ...
... An H1 cloud in the galactic plane at l=30o is observed to have a velocity relative to the local standard of rest of +80 km s-1. Assume the galactic rotation curve is flat with an amplitude of 220 km s-1 , and that Ro = 8.2 kpc and estimate the two possible distances to this cloud. (4) Estimate the m ...
Slide 1
... wavelength of light from most distant galaxies. The further away the galaxies are, the faster they are moving, and the bigger the observed increase in wavelength. This effect is called red-shift. c) How the observed red-shift provides evidence that the universe is expanding and supports the ‘Big Ban ...
... wavelength of light from most distant galaxies. The further away the galaxies are, the faster they are moving, and the bigger the observed increase in wavelength. This effect is called red-shift. c) How the observed red-shift provides evidence that the universe is expanding and supports the ‘Big Ban ...
Standard EPS Shell Presentation
... Identify the conditions necessary for fusion to occur inside a star. Describe the information that spectroscopy provides about stars. Relate the color of a star to its temperature. Explain the factors that determine the brightness of a star in the sky. Discuss the importance of the H-R diagram to as ...
... Identify the conditions necessary for fusion to occur inside a star. Describe the information that spectroscopy provides about stars. Relate the color of a star to its temperature. Explain the factors that determine the brightness of a star in the sky. Discuss the importance of the H-R diagram to as ...
Scales This is a 16 meter by 16 meter scene. A meter is close in size
... Moving outward, we would be able to see the Milky Way galaxy. Since we are inside the Milky Way, we can’t take a picture from the outside, but our galaxy is a grand design spiral somewhat like the whirlpool ...
... Moving outward, we would be able to see the Milky Way galaxy. Since we are inside the Milky Way, we can’t take a picture from the outside, but our galaxy is a grand design spiral somewhat like the whirlpool ...
Phys 214. Planets and Life
... Hubble Space Telescope-Image of Supernova 1994D (SN1994D) in galaxy NGC 4526 (SN 1994D is the bright spot on the lower left) ...
... Hubble Space Telescope-Image of Supernova 1994D (SN1994D) in galaxy NGC 4526 (SN 1994D is the bright spot on the lower left) ...
Astrophysics - Florence
... • Then move through space towards the Earth in successive orders of magnitude until you reach a tall oak tree just outside the buildings of the National High Magnetic Field Laboratory in Tallahassee, Florida. • After that, begin to move from the actual size of a leaf into a microscopic world that re ...
... • Then move through space towards the Earth in successive orders of magnitude until you reach a tall oak tree just outside the buildings of the National High Magnetic Field Laboratory in Tallahassee, Florida. • After that, begin to move from the actual size of a leaf into a microscopic world that re ...
The galaxies that host powerful radio sources
... physically distinct region to optical emission in this interacting galaxy. Dust obscuration. ...
... physically distinct region to optical emission in this interacting galaxy. Dust obscuration. ...
The universe is faster, colder, and wackier than anything we can
... zero, but to reach these unbelievably frigid depths requires complicated and expensive equipment. The natural universe has no such equipment at its disposal, so how cold can it get? The usual answer is the cosmic microwave background (CMB), the afterglow radiation from the Big Bang. The CMB has a te ...
... zero, but to reach these unbelievably frigid depths requires complicated and expensive equipment. The natural universe has no such equipment at its disposal, so how cold can it get? The usual answer is the cosmic microwave background (CMB), the afterglow radiation from the Big Bang. The CMB has a te ...
SWFAS Apr 16 Newsletter - Southwest Florida Astronomical Society
... farthest stretches of the universe before. And we are indeed approaching the limit to what the Hubble Space Telescope can see of the cosmic dawn — yet the fortune-favored satellite still has some surprises in store for us. Astronomers had already used Hubble to find hundreds of galaxies that existed ...
... farthest stretches of the universe before. And we are indeed approaching the limit to what the Hubble Space Telescope can see of the cosmic dawn — yet the fortune-favored satellite still has some surprises in store for us. Astronomers had already used Hubble to find hundreds of galaxies that existed ...
Astronomy 114 Problem Set # 7 Due: 30 Apr 2007 SOLUTIONS 1
... a fraction of an arc second at best. Especially for ground-based telescopes, the main goal is collecting photons! 2 How big would a radio telescope observing at 20 cm wavelength have to be in order to resolve the same angle as the Keck telescope in the last problem? Since 20 cm is in radio wavelengt ...
... a fraction of an arc second at best. Especially for ground-based telescopes, the main goal is collecting photons! 2 How big would a radio telescope observing at 20 cm wavelength have to be in order to resolve the same angle as the Keck telescope in the last problem? Since 20 cm is in radio wavelengt ...
Getting to Know: Structure of the Universe
... How is a solar system different from a galaxy? A solar system is a star and the objects that orbit that star. Scientists have found several solar systems in our galaxy, many of which have planets surrounding them. If the Milky Way galaxy were the size of a quarter, the Sun would be the size of a sin ...
... How is a solar system different from a galaxy? A solar system is a star and the objects that orbit that star. Scientists have found several solar systems in our galaxy, many of which have planets surrounding them. If the Milky Way galaxy were the size of a quarter, the Sun would be the size of a sin ...
PDF Version
... The final step in calculating the size of the universe is using the red shift of galaxies. The red shift is a result of the Doppler effect, in which waves emitted by a source that is moving away from you have a longer apparent wavelength. (You can illustrate the Doppler effect using sound by noticin ...
... The final step in calculating the size of the universe is using the red shift of galaxies. The red shift is a result of the Doppler effect, in which waves emitted by a source that is moving away from you have a longer apparent wavelength. (You can illustrate the Doppler effect using sound by noticin ...
School Supplies - Rowan County Schools
... According to Hubble’s Law, galaxies are moving _____ from one another. ...
... According to Hubble’s Law, galaxies are moving _____ from one another. ...
TT_and_the_Universe
... measuring distance to remote galaxies. They use color spectrum analysis to check temperature. ...
... measuring distance to remote galaxies. They use color spectrum analysis to check temperature. ...
astronomy webquest…… explore the universe
... http://www.enchantedlearning.com/subjects/astronomy/stars/lifecycle/ http://btc.montana.edu/ceres/html/LifeCycle/starsbackground.htm http://www.windows.ucar.edu/tour/link=/the_universe/Nebula.html http://www.windows.ucar.edu/tour/link=/the_universe/Strange.html http://www.windows.ucar.edu/tour/link= ...
... http://www.enchantedlearning.com/subjects/astronomy/stars/lifecycle/ http://btc.montana.edu/ceres/html/LifeCycle/starsbackground.htm http://www.windows.ucar.edu/tour/link=/the_universe/Nebula.html http://www.windows.ucar.edu/tour/link=/the_universe/Strange.html http://www.windows.ucar.edu/tour/link= ...
Observable universe
![](https://commons.wikimedia.org/wiki/Special:FilePath/Observable_Universe_with_Measurements_01.png?width=300)
The observable universe consists of the galaxies and other matter that can, in principle, be observed from Earth at the present time because light and other signals from these objects has had time to reach the Earth since the beginning of the cosmological expansion. Assuming the universe is isotropic, the distance to the edge of the observable universe is roughly the same in every direction. That is, the observable universe is a spherical volume (a ball) centered on the observer. Every location in the Universe has its own observable universe, which may or may not overlap with the one centered on Earth.The word observable used in this sense does not depend on whether modern technology actually permits detection of radiation from an object in this region (or indeed on whether there is any radiation to detect). It simply indicates that it is possible in principle for light or other signals from the object to reach an observer on Earth. In practice, we can see light only from as far back as the time of photon decoupling in the recombination epoch. That is when particles were first able to emit photons that were not quickly re-absorbed by other particles. Before then, the Universe was filled with a plasma that was opaque to photons.The surface of last scattering is the collection of points in space at the exact distance that photons from the time of photon decoupling just reach us today. These are the photons we detect today as cosmic microwave background radiation (CMBR). However, with future technology, it may be possible to observe the still older relic neutrino background, or even more distant events via gravitational waves (which also should move at the speed of light). Sometimes astrophysicists distinguish between the visible universe, which includes only signals emitted since recombination—and the observable universe, which includes signals since the beginning of the cosmological expansion (the Big Bang in traditional cosmology, the end of the inflationary epoch in modern cosmology). According to calculations, the comoving distance (current proper distance) to particles from the CMBR, which represent the radius of the visible universe, is about 14.0 billion parsecs (about 45.7 billion light years), while the comoving distance to the edge of the observable universe is about 14.3 billion parsecs (about 46.6 billion light years), about 2% larger.The best estimate of the age of the universe as of 2015 is 7010137990000000000♠13.799±0.021 billion years but due to the expansion of space humans are observing objects that were originally much closer but are now considerably farther away (as defined in terms of cosmological proper distance, which is equal to the comoving distance at the present time) than a static 13.8 billion light-years distance. It is estimated that the diameter of the observable universe is about 28 gigaparsecs (91 billion light-years, 8.8×1026 metres or 5.5×1023 miles), putting the edge of the observable universe at about 46–47 billion light-years away.