Astronomy Quiz 12 “Stars
... A. white dwarfs / red giant C. red giants / blue dwarfs B. yellow dwarfs / red supergiant D. red dwarfs / blue supergiant _____3. The actual 3D motion of stars relative to each other in a rotating and swirling galaxy is called __ motion. A. radial B. proper C. real D. transverse _____4. How far away ...
... A. white dwarfs / red giant C. red giants / blue dwarfs B. yellow dwarfs / red supergiant D. red dwarfs / blue supergiant _____3. The actual 3D motion of stars relative to each other in a rotating and swirling galaxy is called __ motion. A. radial B. proper C. real D. transverse _____4. How far away ...
Sample Midterm - IUPUI Physics
... b) A nice neat plot with a clear main sequence but a few red giant branches c) A plot with a clear main sequence but an unclear red giant branch d) A complete scatterplot 14. Why would using a cluster of stars in which all the stars are the same distance to plot on an HR diagram be very useful? a) T ...
... b) A nice neat plot with a clear main sequence but a few red giant branches c) A plot with a clear main sequence but an unclear red giant branch d) A complete scatterplot 14. Why would using a cluster of stars in which all the stars are the same distance to plot on an HR diagram be very useful? a) T ...
Calculate the Mass of the Milky Way Galaxy
... "cosmic scatter" and is probably due to the fact that the gas clouds that formed the galaxies all had some small additional motion of their own. The recessional velocity of a galaxy at a particular distance inferred from Hubble's law is called the "Hubble velocity". ...
... "cosmic scatter" and is probably due to the fact that the gas clouds that formed the galaxies all had some small additional motion of their own. The recessional velocity of a galaxy at a particular distance inferred from Hubble's law is called the "Hubble velocity". ...
STAAR Science Tutorial 28 TEK 8.8A: Stars
... o Spiral galaxies have “arms” of stars that spiral outward from the center. The overall shape is round and flat like a plate, but the dense center of a spiral galaxy is spherical. Younger stars are more likely found in the arms of the spiral, and older stars are most likely found in the center sphe ...
... o Spiral galaxies have “arms” of stars that spiral outward from the center. The overall shape is round and flat like a plate, but the dense center of a spiral galaxy is spherical. Younger stars are more likely found in the arms of the spiral, and older stars are most likely found in the center sphe ...
Constellations and Distances to Stars
... • Stars within the same constellation are not necessarily close. They could appear to be almost touching and actually be one trillion kilometers apart. Very few stars are gravitationally bound to one another. • One way to know when a star is close to our solar system is to measure parallax. • Parall ...
... • Stars within the same constellation are not necessarily close. They could appear to be almost touching and actually be one trillion kilometers apart. Very few stars are gravitationally bound to one another. • One way to know when a star is close to our solar system is to measure parallax. • Parall ...
STAAR Science Tutorial 34 TEK 8.8A: Stars, Galaxies
... o Spiral galaxies have “arms” of stars that spiral outward from the center. The overall shape is round and flat like a plate, but the dense center of a spiral galaxy is spherical. Younger stars are more likely found in the arms of the spiral, and older stars are most likely found in the center sphe ...
... o Spiral galaxies have “arms” of stars that spiral outward from the center. The overall shape is round and flat like a plate, but the dense center of a spiral galaxy is spherical. Younger stars are more likely found in the arms of the spiral, and older stars are most likely found in the center sphe ...
Compact Extragalactic Star Formation
... massive star clusters? How do they evolve to become globular clusters today? What is the luminosity function of SSCs, and the mass function of their star formation? • Is optical/IR modeling of star formation in SSCs consistent with radio observations? • How do supernovae evolve in dense environments ...
... massive star clusters? How do they evolve to become globular clusters today? What is the luminosity function of SSCs, and the mass function of their star formation? • Is optical/IR modeling of star formation in SSCs consistent with radio observations? • How do supernovae evolve in dense environments ...
The Galactic Halo The Galactic Disk Height and Thickness of MW
... Shapley’s Center of the Galaxy " To find the center of the Galaxy, Shapley measured the distance to each cluster using RR Lyrae stars and produced a three dimensional plot of the clusters’ positions. The center of the Galaxy was then identified by the average position of the clusters. " We now know ...
... Shapley’s Center of the Galaxy " To find the center of the Galaxy, Shapley measured the distance to each cluster using RR Lyrae stars and produced a three dimensional plot of the clusters’ positions. The center of the Galaxy was then identified by the average position of the clusters. " We now know ...
Searching for stars in high-velocity clouds
... et al. (2002) have measured a metallicity of ≈0.5 solar for one compact HVC. They say that such a low metallicity is inconsistent with an origin for the gas inside the Milky Way. They suggest that it is associated with the Magellanic Clouds or Stream. If stars are associated with some HVCs then ther ...
... et al. (2002) have measured a metallicity of ≈0.5 solar for one compact HVC. They say that such a low metallicity is inconsistent with an origin for the gas inside the Milky Way. They suggest that it is associated with the Magellanic Clouds or Stream. If stars are associated with some HVCs then ther ...
A105 Stars and Galaxies
... The bright, point-like source at the center of the image was produced by a huge X-ray flare in the vicinity of the supermassive black hole. ...
... The bright, point-like source at the center of the image was produced by a huge X-ray flare in the vicinity of the supermassive black hole. ...
November | Activity of the Month
... What to do Part I: A ‘speed of light’ trip through the Universe 1. It’s a big place out there so to see a lot we need to go fast. The fastest thing in the universe is light – it travels at 299,792 kilometres every second. Light is so fast that it takes only 8 minutes to get from the Sun to us. The ...
... What to do Part I: A ‘speed of light’ trip through the Universe 1. It’s a big place out there so to see a lot we need to go fast. The fastest thing in the universe is light – it travels at 299,792 kilometres every second. Light is so fast that it takes only 8 minutes to get from the Sun to us. The ...
Return both exam and scantron sheet when you
... (b) Yellow. (c) Red. 23. A star that is hot and dim must have (a) a very great distance. (b) a very small mass. (c) a very small radius. (d) a very large radius. 24. Stars with masses in excess of 50 solar masses are not very common. (a) True. (b) False. 25. The spectroscopic binaries are detected ( ...
... (b) Yellow. (c) Red. 23. A star that is hot and dim must have (a) a very great distance. (b) a very small mass. (c) a very small radius. (d) a very large radius. 24. Stars with masses in excess of 50 solar masses are not very common. (a) True. (b) False. 25. The spectroscopic binaries are detected ( ...
Gugus Bintang [Compatibility Mode]
... 2. Identify stellar types (such as blue giant stars and red giant stars), determine luminosity from the type, measure brightness, and then calculate distance. If the giant star is in a cluster, then we can determine the distance to the cluster by using several giant stars in the cluster to get its d ...
... 2. Identify stellar types (such as blue giant stars and red giant stars), determine luminosity from the type, measure brightness, and then calculate distance. If the giant star is in a cluster, then we can determine the distance to the cluster by using several giant stars in the cluster to get its d ...
Galaxies - Mike Brotherton
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
... dwarf in a binary system): Type Ia supernovae have well known standard luminosities Compare to apparent magnitudes Find its distances Both are “Standard-candle” methods: Know absolute magnitude (luminosity) compare to apparent magnitude find distance. ...
lecture 27 nuclar fusion in stars
... The sun became hot enough to glow, and the radiation pressure of the light swept away the dust and gas in the solar system. The core kept collapsing, and the temperature of the center of the cloud kept increasing eventually reaching millions of degrees, hot enough for nuclear fusion of hydrogen to t ...
... The sun became hot enough to glow, and the radiation pressure of the light swept away the dust and gas in the solar system. The core kept collapsing, and the temperature of the center of the cloud kept increasing eventually reaching millions of degrees, hot enough for nuclear fusion of hydrogen to t ...
click here - CAPSTONE 2011
... •Knowing a few stars by absolute magnitude in clusters allows us to use the same distance for all cluster stars and to place millions of stars in the HR diagram. • This then allows one to calibrate spectral signatures of luminosity (the H lines are not so broad in giants as in dwarfs) in any stars. ...
... •Knowing a few stars by absolute magnitude in clusters allows us to use the same distance for all cluster stars and to place millions of stars in the HR diagram. • This then allows one to calibrate spectral signatures of luminosity (the H lines are not so broad in giants as in dwarfs) in any stars. ...
File - Physical Science
... There are billions of solar systems in our galaxy and billions of galaxies in the known universe! ...
... There are billions of solar systems in our galaxy and billions of galaxies in the known universe! ...
Proper Motion
... toward or away from the observer. • Radial velocity is measured through the Doppler effect. • When the velocities measure less than 0.01c, we can use prerelativistic formulae: – Vr = c*(λobserver – λs)/ λsource – z=Δλ/λ=Vr/c • Z>0 red-shifted; radial velocity positive • Z<0 blue-shifted; radial velo ...
... toward or away from the observer. • Radial velocity is measured through the Doppler effect. • When the velocities measure less than 0.01c, we can use prerelativistic formulae: – Vr = c*(λobserver – λs)/ λsource – z=Δλ/λ=Vr/c • Z>0 red-shifted; radial velocity positive • Z<0 blue-shifted; radial velo ...
The Hertzsprung-Russell Diagram
... Most stars lie in the main sequence because if a star is hotter it is brighter. Thus you would expect stars of the same size but different temperatures to form a diagonal line since “hotter means brighter” That Main-Sequence is steeper than a ‘same-size diagonal” shows that larger mass ‘normal’ star ...
... Most stars lie in the main sequence because if a star is hotter it is brighter. Thus you would expect stars of the same size but different temperatures to form a diagonal line since “hotter means brighter” That Main-Sequence is steeper than a ‘same-size diagonal” shows that larger mass ‘normal’ star ...
22 pm - Starmap
... As a starting point, face North, holding the map in your eyesight direction, with its North down. As you change the direction, rotate the map accordingly. The objects listed on the first page can be observed with naked eyes, in clear skies, with moderate light pollution. Close your eyes one minute a ...
... As a starting point, face North, holding the map in your eyesight direction, with its North down. As you change the direction, rotate the map accordingly. The objects listed on the first page can be observed with naked eyes, in clear skies, with moderate light pollution. Close your eyes one minute a ...
Lecture 12: Age, Metalicity, and Observations Abundance
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
... SFR(M " yr #1 ) = 7.9 $10#42 L(H% )(ergs#1 ) = 1.08 $10#53 Q(H o )(s#1 ) Q(H o ) is the ionising photon luminosity constants are derived from evol. synthesis models (e.g., Kennicutt 1982) ...
R. Bender (ESO)
... assembly of galaxies and dust-enshrouded violent star formation processes that may have produced a large fraction of all stars in the universe, especially those in spheroids. ALMA will allow to probe the collapse of the first massive galaxy fragments before they have largely turned into stars. A ...
... assembly of galaxies and dust-enshrouded violent star formation processes that may have produced a large fraction of all stars in the universe, especially those in spheroids. ALMA will allow to probe the collapse of the first massive galaxy fragments before they have largely turned into stars. A ...
3rd EXAM VERSION A key - Department of Physics and Astronomy
... A. a galaxy with streams of stars arching out from one region, as if from an explosion B. *a galaxy with an unusually large number of newborn and young stars C. a galaxy that is still in the process of formation from the intergalactic medium and is undergoing its first episode of star formation D. a ...
... A. a galaxy with streams of stars arching out from one region, as if from an explosion B. *a galaxy with an unusually large number of newborn and young stars C. a galaxy that is still in the process of formation from the intergalactic medium and is undergoing its first episode of star formation D. a ...
colour
... Spectrum . . . yields information about surface chemical composition and gravity Evidence from: • Individual stars • Binary systems • Star clusters....these reveal how stars evolve with time • Nuclear physics...energy source, synthesis of heavy elements No direct information about physical condition ...
... Spectrum . . . yields information about surface chemical composition and gravity Evidence from: • Individual stars • Binary systems • Star clusters....these reveal how stars evolve with time • Nuclear physics...energy source, synthesis of heavy elements No direct information about physical condition ...
STELLAR STRUCTURE AND EVOLUTION
... Spectrum . . . yields information about surface chemical composition and gravity Evidence from: • Individual stars • Binary systems • Star clusters....these reveal how stars evolve with time • Nuclear physics...energy source, synthesis of heavy elements No direct information about physical condition ...
... Spectrum . . . yields information about surface chemical composition and gravity Evidence from: • Individual stars • Binary systems • Star clusters....these reveal how stars evolve with time • Nuclear physics...energy source, synthesis of heavy elements No direct information about physical condition ...
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.