Astronomy 730 / Galaxies
... MW to Sculptor to find tff ~ 300 (2/10)3/2 (2 × 107/1011)-1/2 Myr ~ 1.9 Gyr. (c) S&G 7.1: This problem asks you to calculate the crossing time for galaxies in the Coma cluster. The distance is 2R, R = 3 Mpc, and for half the distance galaxies are typically moving at 800 km/s, and for the other half ...
... MW to Sculptor to find tff ~ 300 (2/10)3/2 (2 × 107/1011)-1/2 Myr ~ 1.9 Gyr. (c) S&G 7.1: This problem asks you to calculate the crossing time for galaxies in the Coma cluster. The distance is 2R, R = 3 Mpc, and for half the distance galaxies are typically moving at 800 km/s, and for the other half ...
Section 2
... from the projector through the prism so that the spectrum is visible on a white surface. Use a double thickness of red cellophane to reduce the occurence of light leaks. Ask students to predict what will happen when red cellophane is held between the prism and the spectrum. Students will observe tha ...
... from the projector through the prism so that the spectrum is visible on a white surface. Use a double thickness of red cellophane to reduce the occurence of light leaks. Ask students to predict what will happen when red cellophane is held between the prism and the spectrum. Students will observe tha ...
The star Epsilon UMa, or more commonly known as Alioth
... Alpha-CV type stars are divided into three main groups depending on which spectral lines are most dominant. These three types of spectral lines are silicon, manganese, or as in Alioth’s case, chromium-strontium lines.8 These stars usually lack the more common elements that are found in stars and hav ...
... Alpha-CV type stars are divided into three main groups depending on which spectral lines are most dominant. These three types of spectral lines are silicon, manganese, or as in Alioth’s case, chromium-strontium lines.8 These stars usually lack the more common elements that are found in stars and hav ...
What are Messier Objects? - Bowling Green State University
... Throughout the night as the earth rotates our sky changes, and so does the sky where we stand. The information that continues is the results of a Messier marathon. How many Messier objects can you see in one night? The answer is you never know for sure. If you ask yourself that question everyday, yo ...
... Throughout the night as the earth rotates our sky changes, and so does the sky where we stand. The information that continues is the results of a Messier marathon. How many Messier objects can you see in one night? The answer is you never know for sure. If you ask yourself that question everyday, yo ...
Measurement Systems
... This comparison says “the distance from Selden to Boston is 4.34 times the distance from Selden to NYC.” From there we can use the knowledge that if it’s an hour long trip a trip to Boston would be a little over 4.3 hours (4 hrs 18 min). to NYC by car then Ratios are the means for creating model ...
... This comparison says “the distance from Selden to Boston is 4.34 times the distance from Selden to NYC.” From there we can use the knowledge that if it’s an hour long trip a trip to Boston would be a little over 4.3 hours (4 hrs 18 min). to NYC by car then Ratios are the means for creating model ...
Astronomy (ASTR)
... we cannot see nor properly characterize, the so-called 'dark matter,' and of energy whose source is unknown and may defy knowing, the ubiquitous 'dark energy.' This course will attempt to elucidate what we currently understand about the composition, structure and evolution of the universe based on g ...
... we cannot see nor properly characterize, the so-called 'dark matter,' and of energy whose source is unknown and may defy knowing, the ubiquitous 'dark energy.' This course will attempt to elucidate what we currently understand about the composition, structure and evolution of the universe based on g ...
Chapter 20. Galaxies
... star light from the galaxy. It is further characterized by sometimes extreme variability that reflects variations in the accretion rate. The time scale for the variations can be as short as minutes, hours, days or months. When variable galaxies on these time scales were first discovered it was hard ...
... star light from the galaxy. It is further characterized by sometimes extreme variability that reflects variations in the accretion rate. The time scale for the variations can be as short as minutes, hours, days or months. When variable galaxies on these time scales were first discovered it was hard ...
PDF format
... a) Some stars are larger than others and therefore appear larger. b) Some stars are nearer than others and therefore appear larger. c) Photographs make brighter stars appear larger than fainter stars, although they should all be points of light. d) Sometimes what looks like a single star is actu ...
... a) Some stars are larger than others and therefore appear larger. b) Some stars are nearer than others and therefore appear larger. c) Photographs make brighter stars appear larger than fainter stars, although they should all be points of light. d) Sometimes what looks like a single star is actu ...
Task - Illustrative Mathematics
... when they are placed in increasing order. On the other hand, outliers can have a dramatic impact on the mean, especially if the data set is small or if these outliers are several orders of magnitude larger than most other data points. This is made particularly clear in the case of the distance of th ...
... when they are placed in increasing order. On the other hand, outliers can have a dramatic impact on the mean, especially if the data set is small or if these outliers are several orders of magnitude larger than most other data points. This is made particularly clear in the case of the distance of th ...
PPT
... What have we learned? • How do we measure the distances to galaxies? – The distance-measurement chain begins with parallax measurements that build on radar ranging in our solar system – Using parallax and the relationship between luminosity, distance, and brightness, we can calibrate a series of st ...
... What have we learned? • How do we measure the distances to galaxies? – The distance-measurement chain begins with parallax measurements that build on radar ranging in our solar system – Using parallax and the relationship between luminosity, distance, and brightness, we can calibrate a series of st ...
10 Measuring The Stars
... appears when viewed from Earth; it depends on the absolute brightness but also on the distance of the star: apparent brightness luminosity/distance2 ...
... appears when viewed from Earth; it depends on the absolute brightness but also on the distance of the star: apparent brightness luminosity/distance2 ...
Unit 13―The “Fixed” Stars
... and so jump by whole factors of 100 on the energy or luminosity scale, but we need to know luminosity values for single values of magnitude. That means we are looking for a number which when multiplied by its self five times equals 100. That is called the “fifth-root of 100.” And the ancients stuck ...
... and so jump by whole factors of 100 on the energy or luminosity scale, but we need to know luminosity values for single values of magnitude. That means we are looking for a number which when multiplied by its self five times equals 100. That is called the “fifth-root of 100.” And the ancients stuck ...
Measuring the Stars Section 29.2
... Basic Properties of Stars Magnitude The classification of stars by absolute magnitude allows comparisons that are based on how bright the stars would appear at equal distances from an observer. The disadvantage of absolute magnitude is that it can be calculated only when the actual distance to a sta ...
... Basic Properties of Stars Magnitude The classification of stars by absolute magnitude allows comparisons that are based on how bright the stars would appear at equal distances from an observer. The disadvantage of absolute magnitude is that it can be calculated only when the actual distance to a sta ...
Sample Exam for 3 rd Astro Exam
... A. In the galactic halo. B. In the galactic nuclear bulge C. Beyond the Sun above and below the galactic mid-plane D. Perpendicular to the galactic plane. E. In the galactic mid-plane 16. True or false: The Sun is located within the galactic gas layer of the Milky Way A. True B. False C. I have no @ ...
... A. In the galactic halo. B. In the galactic nuclear bulge C. Beyond the Sun above and below the galactic mid-plane D. Perpendicular to the galactic plane. E. In the galactic mid-plane 16. True or false: The Sun is located within the galactic gas layer of the Milky Way A. True B. False C. I have no @ ...
The Evening Sky Map
... Constellation – A defined area of the sky containing a star pattern. Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to each other in the sky; either linked by gravity so that they orbit each other (binary star) or lying at different distances f ...
... Constellation – A defined area of the sky containing a star pattern. Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to each other in the sky; either linked by gravity so that they orbit each other (binary star) or lying at different distances f ...
Supermassive black holes
... Edwin Hubble used observations of _______ to determine the distance to the ...
... Edwin Hubble used observations of _______ to determine the distance to the ...
ppt
... Why not to use them to search for new sources? How? Just using the fact that all known magnetars show periodicity in a narrow range! Muno et al. used 506 Chandra and 441 XMM-Newton observations of the 1033 for erg/s Galactic plane (|b|<5oL=3 ) to look sources with 5 s < P < 20 s. ...
... Why not to use them to search for new sources? How? Just using the fact that all known magnetars show periodicity in a narrow range! Muno et al. used 506 Chandra and 441 XMM-Newton observations of the 1033 for erg/s Galactic plane (|b|<5oL=3 ) to look sources with 5 s < P < 20 s. ...
FREE Sample Here
... sky. Most people today no longer have an understanding of the basic appearance or motions of the sky. The three Window on Science (WOS) discussions in this chapter present very important concepts in all sciences. WOS 2-1 focuses on the development of scientific arguments. It is important to emphasiz ...
... sky. Most people today no longer have an understanding of the basic appearance or motions of the sky. The three Window on Science (WOS) discussions in this chapter present very important concepts in all sciences. WOS 2-1 focuses on the development of scientific arguments. It is important to emphasiz ...
chapter 2 - Test Bank 1
... sky. Most people today no longer have an understanding of the basic appearance or motions of the sky. The three Window on Science (WOS) discussions in this chapter present very important concepts in all sciences. WOS 2-1 focuses on the development of scientific arguments. It is important to emphasiz ...
... sky. Most people today no longer have an understanding of the basic appearance or motions of the sky. The three Window on Science (WOS) discussions in this chapter present very important concepts in all sciences. WOS 2-1 focuses on the development of scientific arguments. It is important to emphasiz ...
Local group
... • where Mtotal is the sum of the 2 masses Initially, take r=0 at t=0 • solution of the form r=Rmax/2(1-cosq) and t=(R3max/8MtotalGtotal)1/2(q-sinq) • The distance increases from 0 (forq=0 ) to some maximum value Rmax (forq=p ), and then decreases again. The relative velocity is ...
... • where Mtotal is the sum of the 2 masses Initially, take r=0 at t=0 • solution of the form r=Rmax/2(1-cosq) and t=(R3max/8MtotalGtotal)1/2(q-sinq) • The distance increases from 0 (forq=0 ) to some maximum value Rmax (forq=p ), and then decreases again. The relative velocity is ...
Word
... collisions between two circular galaxies, and each of them respectively consists of N and N1 “particles” which appear in the form of a dot in the animation programme. N and N1 can be adjusted. All of them have the same mass. The steps of the program is shown as follows: 1.) The positions of the cent ...
... collisions between two circular galaxies, and each of them respectively consists of N and N1 “particles” which appear in the form of a dot in the animation programme. N and N1 can be adjusted. All of them have the same mass. The steps of the program is shown as follows: 1.) The positions of the cent ...
Age Distributions of Low Mass Stars in the Rho Ophiucus Molecular
... one of the closest star-forming regions available for study. Because of this relatively close distance, low luminosity young stellar objects (YSOs) in the optical range can be viewed and studied that would otherwise would be too faint in more distant star-forming regions[2]. These YSOs can be imaged ...
... one of the closest star-forming regions available for study. Because of this relatively close distance, low luminosity young stellar objects (YSOs) in the optical range can be viewed and studied that would otherwise would be too faint in more distant star-forming regions[2]. These YSOs can be imaged ...
Galaxies
... them from their orbits. In some cases, they will be forced into an orbit closer to the center of the galaxy; in other cases, they will be forced into orbits farther out. There will be a change in speed when a star changes orbit. As a result, as the star continues to move, the overall galaxy will beg ...
... them from their orbits. In some cases, they will be forced into an orbit closer to the center of the galaxy; in other cases, they will be forced into orbits farther out. There will be a change in speed when a star changes orbit. As a result, as the star continues to move, the overall galaxy will beg ...
1 Introduction - High Point University
... (Dwarfs (V)) is known as the main sequence and contains all stars that are fusing hydrogen into helium as their primary energy source. Over 90% of all stars fall in this region on the H-R diagram. Move the active cursor up and down the main sequence and explore the different values of stellar radius ...
... (Dwarfs (V)) is known as the main sequence and contains all stars that are fusing hydrogen into helium as their primary energy source. Over 90% of all stars fall in this region on the H-R diagram. Move the active cursor up and down the main sequence and explore the different values of stellar radius ...
Malmquist bias
The Malmquist bias is an effect in observational astronomy which leads to the preferential detection of intrinsically bright objects. It was first described in 1922 by Swedish astronomer Gunnar Malmquist (1893–1982), who then greatly elaborated upon this work in 1925. In statistics, this bias is referred to as a selection bias and affects the survey results in a brightness limited survey, where stars below a certain apparent brightness are not included. Since observed stars and galaxies appear dimmer when farther away, the brightness that is measured will fall off with distance until their brightness falls below the observational threshold. Objects which are more luminous, or intrinsically brighter, can be observed at a greater distance, creating a false trend of increasing intrinsic brightness, and other related quantities, with distance. This effect has led to many spurious claims in the field of astronomy. Properly correcting for these effects has become an area of great focus.