![Newton`s Law of Universal Gravitation](http://s1.studyres.com/store/data/008084879_2-cd0753a252214bbb67b0d7fedef33b67-300x300.png)
Newton`s Law of Universal Gravitation
... of our galaxy, the Milky Way. The sun, mass 2.0X1030kg, revolves around the center of thee galaxy with a radius of 2.2X1020 m. The period of one rotation is 2.6X108 years. a. Find the approximate mass of the galaxy. b. Assume the average star in the galaxy has the mass of the sun, find the number of ...
... of our galaxy, the Milky Way. The sun, mass 2.0X1030kg, revolves around the center of thee galaxy with a radius of 2.2X1020 m. The period of one rotation is 2.6X108 years. a. Find the approximate mass of the galaxy. b. Assume the average star in the galaxy has the mass of the sun, find the number of ...
Lecture 1
... Size and Time Scales of the Universe Physical scale: What does the solar system look like? How far away are the stars? How big is our Milky Way? How does it compare to other galaxies? How far away are galaxies? Time scale: How much time do we live? how much time do stars live? how old is the univers ...
... Size and Time Scales of the Universe Physical scale: What does the solar system look like? How far away are the stars? How big is our Milky Way? How does it compare to other galaxies? How far away are galaxies? Time scale: How much time do we live? how much time do stars live? how old is the univers ...
Chapter 27.1
... Nearby stars apparent position in relation to more distant stars changes as earth moves in its orbit from one side of the sun to the other. Limited to measuring the distance to stars within 1000 light years of earth. ...
... Nearby stars apparent position in relation to more distant stars changes as earth moves in its orbit from one side of the sun to the other. Limited to measuring the distance to stars within 1000 light years of earth. ...
Final for Astro 322, Prof. Heinke, April 23rd, 2010 Formula sheet
... b) What is the emitting material likely to be? c) What are two possibilities for the original source of the energy we see? (Describe each in a couple of sentences.) They are not necessarily exclusive. d) What do you think this galaxy’s recent history has been, and what will happen to it now? Problem ...
... b) What is the emitting material likely to be? c) What are two possibilities for the original source of the energy we see? (Describe each in a couple of sentences.) They are not necessarily exclusive. d) What do you think this galaxy’s recent history has been, and what will happen to it now? Problem ...
No Slide Title
... globular clusters (left-hand panel) is made of objects on low-inclination, nearly-circular orbits <=> the system has some prograde rotation. Spherical system (right panel) has completely disorganized motions, no rotation on average; some clusters have prograge, some retrograde motion, Orbits are hig ...
... globular clusters (left-hand panel) is made of objects on low-inclination, nearly-circular orbits <=> the system has some prograde rotation. Spherical system (right panel) has completely disorganized motions, no rotation on average; some clusters have prograge, some retrograde motion, Orbits are hig ...
Lecture 6
... any part of the electromagnetic spectrum (X-ray, infrared, radio, etc…). We sense its presence only through its gravitational influence on the orbits of stars and gas clouds. Conclusion: Galaxies are surrounded by massive halos of invisible matter. This is the main evidence for so-called “dark matte ...
... any part of the electromagnetic spectrum (X-ray, infrared, radio, etc…). We sense its presence only through its gravitational influence on the orbits of stars and gas clouds. Conclusion: Galaxies are surrounded by massive halos of invisible matter. This is the main evidence for so-called “dark matte ...
Physics 5 – The Universe
... a. A basic description of how an optical telescope works b. Explain how astronomers know that all stars are moving away from us c. A description of the Earth’s place in the universe, this is to include solar system, galaxy and universe. d. Describe the terms: Solar system, Galaxy, universe e. Explai ...
... a. A basic description of how an optical telescope works b. Explain how astronomers know that all stars are moving away from us c. A description of the Earth’s place in the universe, this is to include solar system, galaxy and universe. d. Describe the terms: Solar system, Galaxy, universe e. Explai ...
Life Cycle of Stars Flipbook Assignment
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
Powerpoint of lecture 1
... E = gravitational energy of star, L = luminosity: tKH = GM2/LR ~ 3107 yr for Sun. But geology requires much longer timescale – only nuclear fuel provides this; nuclear binding energy releases up to ~1% of rest mass energy: EN ~ 0.01Mc2, so tN ~ 0.01Mc2/L ~ 1.5 1011 yr for Sun. Over-estimate, becau ...
... E = gravitational energy of star, L = luminosity: tKH = GM2/LR ~ 3107 yr for Sun. But geology requires much longer timescale – only nuclear fuel provides this; nuclear binding energy releases up to ~1% of rest mass energy: EN ~ 0.01Mc2, so tN ~ 0.01Mc2/L ~ 1.5 1011 yr for Sun. Over-estimate, becau ...
Distance measurement in Astronomy
... You can find the distances of stars that are ‘relatively close’ to the Earth using parallax. A very simple example of parallax is to hold one forefinger upright about 30 cm in front of your nose and close your right eye. Using just your left eye line up your forefinger with an object on the other si ...
... You can find the distances of stars that are ‘relatively close’ to the Earth using parallax. A very simple example of parallax is to hold one forefinger upright about 30 cm in front of your nose and close your right eye. Using just your left eye line up your forefinger with an object on the other si ...
LAB #6 - GEOCITIES.ws
... ANSWER ALL PRE-LAB WARMUPS BEFORE COMING TO LAB. You will begin lab with a short quiz on these questions. This exercise will continue with the techniques used by astronomers to determine the fundamental properties of stars. In this exercise we will use these techniques to study the characteristics o ...
... ANSWER ALL PRE-LAB WARMUPS BEFORE COMING TO LAB. You will begin lab with a short quiz on these questions. This exercise will continue with the techniques used by astronomers to determine the fundamental properties of stars. In this exercise we will use these techniques to study the characteristics o ...
Part 1- The Basics
... Binary star systems: stellar masses • The masses can be computed from measurements of the orbital period and orbital size of the system • The mass ratio of M1 and M2 is inversely proportional to the distance of stars to the center of mass ...
... Binary star systems: stellar masses • The masses can be computed from measurements of the orbital period and orbital size of the system • The mass ratio of M1 and M2 is inversely proportional to the distance of stars to the center of mass ...
For each statement or question, select the word or expression that
... A. Canis Major B. Cassiopeia C. Orion D. Ursa Major ____ 10. An example of a winter constellation is A. Lyra B. Orion C. Cygnus D. Cassiopeia ____ 11. A light-year measures A. time B. distance C. speed D. energy ____ 12. The mass of a star can be measured by A. direct observation B. performing calcu ...
... A. Canis Major B. Cassiopeia C. Orion D. Ursa Major ____ 10. An example of a winter constellation is A. Lyra B. Orion C. Cygnus D. Cassiopeia ____ 11. A light-year measures A. time B. distance C. speed D. energy ____ 12. The mass of a star can be measured by A. direct observation B. performing calcu ...
2.64 3.26156 8.61 pc ly × =
... Thus Polaris is about 49.6 times farther from us than Sirius. From Appendix 5 of the textbook, Sirius is 8.58 ly from Earth so Polaris is 8.58 ly X 49.6 = 425 ly away. 13.49. Proxima Centauri, the star nearest the Earth other than the Sun, has a parallax of 0.772 arcseconds. How long does it take li ...
... Thus Polaris is about 49.6 times farther from us than Sirius. From Appendix 5 of the textbook, Sirius is 8.58 ly from Earth so Polaris is 8.58 ly X 49.6 = 425 ly away. 13.49. Proxima Centauri, the star nearest the Earth other than the Sun, has a parallax of 0.772 arcseconds. How long does it take li ...
Stars and Sun
... Only part of the Milky Way is visible due to our being in the galaxy Galileo saw the Milky Way in 1609 using a telescope Bigger and brighter than most galaxies in the universe ...
... Only part of the Milky Way is visible due to our being in the galaxy Galileo saw the Milky Way in 1609 using a telescope Bigger and brighter than most galaxies in the universe ...
The Earth
... big it is. I mean, you may think it’s a long way down the road to the chemist’s, but that's just peanuts to space. Douglas ...
... big it is. I mean, you may think it’s a long way down the road to the chemist’s, but that's just peanuts to space. Douglas ...
Chapter 1 Vocabulary – The Puzzled of Matter
... flung into space Neutron Star – the dense core left after a high-mass star has exploded as a supernova Pulsar – a spinning neutron star that appears to give off strong pulses of radio waves Black Hole – an object whose surface gravity is so great that no even electromagnetic waves can escape from it ...
... flung into space Neutron Star – the dense core left after a high-mass star has exploded as a supernova Pulsar – a spinning neutron star that appears to give off strong pulses of radio waves Black Hole – an object whose surface gravity is so great that no even electromagnetic waves can escape from it ...
Stellar Parallax
... As a result it is convenient to use logarithmic scales. • Astronomers use relative measures of Intensity. The system is based on the assumption that iVEGA = 1.0 and the apparent intensities of all other stars (i) are measured relative to the intensity of Vega. We define the apparent magnitude (m) of ...
... As a result it is convenient to use logarithmic scales. • Astronomers use relative measures of Intensity. The system is based on the assumption that iVEGA = 1.0 and the apparent intensities of all other stars (i) are measured relative to the intensity of Vega. We define the apparent magnitude (m) of ...
Astro twopages
... the center (net mass located inside a sphere of radius r concentric with the , ρ(r) is the density at distance r and G is the universal gravitational constant. Distances (actually best expressed as light travel time): Moon: When you listen to the communications of the Apollo astronauts there is a co ...
... the center (net mass located inside a sphere of radius r concentric with the , ρ(r) is the density at distance r and G is the universal gravitational constant. Distances (actually best expressed as light travel time): Moon: When you listen to the communications of the Apollo astronauts there is a co ...
Chapter 12 Our Place in the Universe
... She did this by looking at nearby Cepheids of known distance. So if you observed a Cepheid variable and measured the changes in brightness then you could work out the size of the star. This allowed you to work out how far away it was! Luckily, Cepheid variables are very big, very bright stars. This ...
... She did this by looking at nearby Cepheids of known distance. So if you observed a Cepheid variable and measured the changes in brightness then you could work out the size of the star. This allowed you to work out how far away it was! Luckily, Cepheid variables are very big, very bright stars. This ...
Slides from Lecture04
... • The brightest stars were labeled “1st magnitude” stars • Successively fainter stars were catalogued as 2nd magnitude, 3rd magnitude, etc. • Faintest stars (visible to the “naked eye”) were catalogued by Greek astronomers as 6th magnitude stars. • Astronomers continue to use this “magnitude” system ...
... • The brightest stars were labeled “1st magnitude” stars • Successively fainter stars were catalogued as 2nd magnitude, 3rd magnitude, etc. • Faintest stars (visible to the “naked eye”) were catalogued by Greek astronomers as 6th magnitude stars. • Astronomers continue to use this “magnitude” system ...
18.3 NOTES What is magnitude? Objective: Compare apparent
... brighter than others. One way to measure a star’s brightness is by magnitude. The brightness of a star depends on its temperature, size, and distance from Earth. A hot star is usually brighter than a cool star. A large star is usually brighter than a small star. The closer it is to earth, the bright ...
... brighter than others. One way to measure a star’s brightness is by magnitude. The brightness of a star depends on its temperature, size, and distance from Earth. A hot star is usually brighter than a cool star. A large star is usually brighter than a small star. The closer it is to earth, the bright ...
Astr 40 Final Exam Review ()
... 47. A black hole is best defined as any object which is smaller than its event horizon. 48. Isolated black holes slowly evaporate because they slowly leak mass via virtual particles that form near the event horizon. 49. When compared to visual, spectroscopic, or eclipsing binaries, optical doubles a ...
... 47. A black hole is best defined as any object which is smaller than its event horizon. 48. Isolated black holes slowly evaporate because they slowly leak mass via virtual particles that form near the event horizon. 49. When compared to visual, spectroscopic, or eclipsing binaries, optical doubles a ...
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.