![Measuring Our Universe](http://s1.studyres.com/store/data/008814834_1-43f980e980a1abf116744047392075d7-300x300.png)
Measuring Our Universe
... The distance AD is called the baseline. This method is limited by our ability to measure very small angles, and so to determine the distance to very far objects, we must use as long a baseline as possible. Astronomers realized that the longest possible baseline that could be used to measure astronom ...
... The distance AD is called the baseline. This method is limited by our ability to measure very small angles, and so to determine the distance to very far objects, we must use as long a baseline as possible. Astronomers realized that the longest possible baseline that could be used to measure astronom ...
Lab: Heliocentric Parallax
... The computer can simulate a number of different fields (areas on the sky). For this lab, it will randomly select three fields for your use. For each field, you can blink back and forth between 2 virtual photo taken six months apart. As you blink between the photos, you’ll notice several stars shift ...
... The computer can simulate a number of different fields (areas on the sky). For this lab, it will randomly select three fields for your use. For each field, you can blink back and forth between 2 virtual photo taken six months apart. As you blink between the photos, you’ll notice several stars shift ...
Celestial Objects
... 1) the farther away the galaxy, the greater the red shift 2) almost all galaxies show a red shiftshiftproof that the universe is expanding (Edwin Hubble was the first to realize this!) ...
... 1) the farther away the galaxy, the greater the red shift 2) almost all galaxies show a red shiftshiftproof that the universe is expanding (Edwin Hubble was the first to realize this!) ...
ASTR 1120 STUDY GUIDE FOR MIDTERM III This guide is to aid
... 2. How does the Milky Way look at various wavelengths? Which wavelengths are mostly absorbed and which ones are not? 3. The cosmic “distance ladder”: what are the various ways by which astronomers measure cosmic distances beyond what is possible with parallax? Be sure to be familiar with the basic i ...
... 2. How does the Milky Way look at various wavelengths? Which wavelengths are mostly absorbed and which ones are not? 3. The cosmic “distance ladder”: what are the various ways by which astronomers measure cosmic distances beyond what is possible with parallax? Be sure to be familiar with the basic i ...
Skywatch Astro Ed Dec13
... more than four light-years away; a reminder of the vast gulf that separates us from even our closest stellar neighbours. Between Sirius and Aldebaran, another bright star beckons us. This is Rigel, which at 900 light years away, is more than 100 times further away than Sirius. Yet, if we swapped the ...
... more than four light-years away; a reminder of the vast gulf that separates us from even our closest stellar neighbours. Between Sirius and Aldebaran, another bright star beckons us. This is Rigel, which at 900 light years away, is more than 100 times further away than Sirius. Yet, if we swapped the ...
doc - IAC
... same way as planetary masses are measured. The most massive ones are 100 to 150 times heavier than the Sun. The most massive stars evolve more rapidly than those of low mass. Does this in any way affect the galaxies in which they are found? Indeed it does. Massive stars have very short lifetimes, at ...
... same way as planetary masses are measured. The most massive ones are 100 to 150 times heavier than the Sun. The most massive stars evolve more rapidly than those of low mass. Does this in any way affect the galaxies in which they are found? Indeed it does. Massive stars have very short lifetimes, at ...
E3 – Stellar distances
... Cepheid variables • At distances greater than Mpc, neither parallax nor spectroscopic parallax can be relied upon to measure the distance to a star. • When we observe another galaxy, all of the stars in that galaxy are approximately the same distance away from the earth. What we really need is a li ...
... Cepheid variables • At distances greater than Mpc, neither parallax nor spectroscopic parallax can be relied upon to measure the distance to a star. • When we observe another galaxy, all of the stars in that galaxy are approximately the same distance away from the earth. What we really need is a li ...
Comparing Earth, Sun and Jupiter
... ¾ The dust obscures most of the light from these stars. If there were no dust, the centre of the galaxy would be as bright as the full moon ¾ Looking in infrared light, which is less affected by dust, we can see the full structure of our Galaxy. • Young stars and open clusters, in roughly circular o ...
... ¾ The dust obscures most of the light from these stars. If there were no dust, the centre of the galaxy would be as bright as the full moon ¾ Looking in infrared light, which is less affected by dust, we can see the full structure of our Galaxy. • Young stars and open clusters, in roughly circular o ...
Big Bang Balloon
... In the 1920s astronomer Edwin Hubble used the red shift of the spectra of stars to determine that the universe was expanding. By carefully observing the light from galaxies at different distances from Earth, he determined that the farther something was from Earth, the faster it seemed to be moving a ...
... In the 1920s astronomer Edwin Hubble used the red shift of the spectra of stars to determine that the universe was expanding. By carefully observing the light from galaxies at different distances from Earth, he determined that the farther something was from Earth, the faster it seemed to be moving a ...
+(J - cloudfront.net
... spectrum and temperature of a certain star are used to determine its luminosity to be approximately 5.0 x 1031 W. The '!Pparent brightness of the star is 1.4 x 10-9 W m-2. These data can be used to detennine the distance ofihe'staifromEarth~------""----..-.--..---- - - ..(i) ...
... spectrum and temperature of a certain star are used to determine its luminosity to be approximately 5.0 x 1031 W. The '!Pparent brightness of the star is 1.4 x 10-9 W m-2. These data can be used to detennine the distance ofihe'staifromEarth~------""----..-.--..---- - - ..(i) ...
Sky News – March 2015 The Realm of the Galaxies
... we can see deep into the sky without objects being obscured or dimmed by looking through our galaxy. In spring skies we are treated to views of the closest cluster of galaxies in Virgo of which our local group of galaxies are outlying members. Here galaxies are so numerous that they seem to outnumbe ...
... we can see deep into the sky without objects being obscured or dimmed by looking through our galaxy. In spring skies we are treated to views of the closest cluster of galaxies in Virgo of which our local group of galaxies are outlying members. Here galaxies are so numerous that they seem to outnumbe ...
02-02Stars_Part_One
... Concept 2 – Apparent Magnitude - m The idea here is that a ratio of apparent brightness of 100, would lead to a difference in apparent magnitude of 5. Note that the dimmer the star, the bigger m is. ...
... Concept 2 – Apparent Magnitude - m The idea here is that a ratio of apparent brightness of 100, would lead to a difference in apparent magnitude of 5. Note that the dimmer the star, the bigger m is. ...
The Sun and the Stars
... • It can be measured more precisely as a star’s total energy output per second, measured in Joules per second (J/s) • When discussion stars we always compare with the sun, some stars are about 10 000 times less luminous than the Sun or up to 30 000 times more luminous. ...
... • It can be measured more precisely as a star’s total energy output per second, measured in Joules per second (J/s) • When discussion stars we always compare with the sun, some stars are about 10 000 times less luminous than the Sun or up to 30 000 times more luminous. ...
Measuring the Heavens: Parallax
... Parallax angles are very small, much smaller than 1°. Thus, astronomers express angles in terms of arc minutes (abbreviated ') and arc seconds (abbreviated "), where 60 arc minutes = 1 degree (60' = 1°), and 60 arc seconds = 1 arc minute (60" = 1'). ...
... Parallax angles are very small, much smaller than 1°. Thus, astronomers express angles in terms of arc minutes (abbreviated ') and arc seconds (abbreviated "), where 60 arc minutes = 1 degree (60' = 1°), and 60 arc seconds = 1 arc minute (60" = 1'). ...
antarctic and associated exploration book collection
... brightness of 1080 stars, using a simple classification ranging between 1 (for the brightest stars) and 6 (for the dimmest stars, just visible to the naked eye.) In 1856, Norman Pogson noted that the difference in apparent brightness between stars of magnitude 1 and 6 was a factor of about 100, with ...
... brightness of 1080 stars, using a simple classification ranging between 1 (for the brightest stars) and 6 (for the dimmest stars, just visible to the naked eye.) In 1856, Norman Pogson noted that the difference in apparent brightness between stars of magnitude 1 and 6 was a factor of about 100, with ...
Disk Galaxies: Structural Components
... • Collapse of an over-dense region of space (containing more gas and dark matter than average) under gravity • Disks are produced as the cloud of material spins faster and faster as the gravitational collapse progresses • To conserve angular momentum, the spin speed must increase inversely proportio ...
... • Collapse of an over-dense region of space (containing more gas and dark matter than average) under gravity • Disks are produced as the cloud of material spins faster and faster as the gravitational collapse progresses • To conserve angular momentum, the spin speed must increase inversely proportio ...
Problem Set 2
... ring’s radius in parcsec? Recall from class that the ring’s angular radius is the projected ellipse’s semi-major axis. What is the distance d to the supernova? Finally, at its brightest, SN1987A had an apparent magnitude of mV ≈ 3 mag. What was its peak absolute magnitude? Given that the Sun has an ...
... ring’s radius in parcsec? Recall from class that the ring’s angular radius is the projected ellipse’s semi-major axis. What is the distance d to the supernova? Finally, at its brightest, SN1987A had an apparent magnitude of mV ≈ 3 mag. What was its peak absolute magnitude? Given that the Sun has an ...
Where is the Solar System in the Universe?
... Scientists find it hard to work with the measurements we use on earth, like kilometers and miles, because the distances are so great it is hard for us to comprehend such enormous numbers. ...
... Scientists find it hard to work with the measurements we use on earth, like kilometers and miles, because the distances are so great it is hard for us to comprehend such enormous numbers. ...
canopus e.g procyon
... • Proxima Centauri – closest of the triplet of stars loosely known as alpha-Centauri Proxima Centauri is a faint red star that orbits Alpha-Centauri A and B with a period of about one million years. Proxima Centauri is 4.22 light years from the Earth (now) and about 0.24 light years from Alpha-Cent ...
... • Proxima Centauri – closest of the triplet of stars loosely known as alpha-Centauri Proxima Centauri is a faint red star that orbits Alpha-Centauri A and B with a period of about one million years. Proxima Centauri is 4.22 light years from the Earth (now) and about 0.24 light years from Alpha-Cent ...
Römer and the speed of light
... brightest stars are 1st magnitude (m=1) faintest stars are 6th magnitude (m=6) Pogson (1856): A 1st magnitude star is 100 times brighter than a 6th magnitude star! The Eye is a negative logarithmic detector. ...
... brightest stars are 1st magnitude (m=1) faintest stars are 6th magnitude (m=6) Pogson (1856): A 1st magnitude star is 100 times brighter than a 6th magnitude star! The Eye is a negative logarithmic detector. ...
Galaxies and the Big Bang Theory
... A _______________ _________________ is a device used to detect long radio waves from objects in space. A ___________ is a huge group of single stars, star systems, star clusters, dust, and gas bound together by gravity The three different types of galaxies that exist in our universe are: ...
... A _______________ _________________ is a device used to detect long radio waves from objects in space. A ___________ is a huge group of single stars, star systems, star clusters, dust, and gas bound together by gravity The three different types of galaxies that exist in our universe are: ...
Friday, April 25 - Otterbein University
... • Extends the cosmic distance ladder out as far as we can see Cepheids – about 50 million ly • In 1920 Hubble used this technique to measure the distance to Andromeda (about 2 million ly) • Works best for periodic variables ...
... • Extends the cosmic distance ladder out as far as we can see Cepheids – about 50 million ly • In 1920 Hubble used this technique to measure the distance to Andromeda (about 2 million ly) • Works best for periodic variables ...
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.