Chapter 6 Stars
... supergiant stars are very bright. These bright giant and supergiant stars can be found near the top center and right of the diagram. White dwarfs are hot, but not very bright so they appear at the bottom left or bottom center. ...
... supergiant stars are very bright. These bright giant and supergiant stars can be found near the top center and right of the diagram. White dwarfs are hot, but not very bright so they appear at the bottom left or bottom center. ...
The Sun: Example of Radiation Laws
... The production of neutrinos and the nucleosynthesis and ejection of heavy nuclei in Type II supernovae was confirmed by SN 1987a in the Large Magellenic Cloud, a nearby galaxy, on February 23, 1987. Neutrino detectors in Ohio and Japan detected a total of about 20 neutrinos even though this supernov ...
... The production of neutrinos and the nucleosynthesis and ejection of heavy nuclei in Type II supernovae was confirmed by SN 1987a in the Large Magellenic Cloud, a nearby galaxy, on February 23, 1987. Neutrino detectors in Ohio and Japan detected a total of about 20 neutrinos even though this supernov ...
Document
... red giant is increasing due to the great increase in luminosity being provided by the fusion occurring in a shell around the core. ...
... red giant is increasing due to the great increase in luminosity being provided by the fusion occurring in a shell around the core. ...
Lecture 8: The Stars - Department of Physics and Astronomy
... Globular cluster: Up to a million or more stars in a dense ball bound together by gravity ...
... Globular cluster: Up to a million or more stars in a dense ball bound together by gravity ...
Distance to the SMC
... your results to the values in Table I. Your instructor will provide tips on how to best reduce the light curves. Record all of your measurements for this part on your own paper and submit that data page with the rest of your work. For each of the four light curves for Cepheid variables, estimate the ...
... your results to the values in Table I. Your instructor will provide tips on how to best reduce the light curves. Record all of your measurements for this part on your own paper and submit that data page with the rest of your work. For each of the four light curves for Cepheid variables, estimate the ...
Student Exploration Sheet: Growing Plants
... “smeared out.” Giant stars, which have relatively low atmospheric pressures, are characterized by narrow spectral lines. ...
... “smeared out.” Giant stars, which have relatively low atmospheric pressures, are characterized by narrow spectral lines. ...
Virtual HR Diagram Lab
... 3. Drag the active location around on the HR Diagram once again. This time focus on the Size Comparison panel. Check the appropriate region of the HR diagram corresponding to each description below. ...
... 3. Drag the active location around on the HR Diagram once again. This time focus on the Size Comparison panel. Check the appropriate region of the HR diagram corresponding to each description below. ...
PHYS-633: Problem set #0 Solutions
... c. Which result seems more “reasonable”? Briefly discuss what other physics might be important to include to understand the actual surface temperature of Earth. This apparently more realistic model thus seems to give a temperature that is much lower than the typical temperature of the actual Earth. ...
... c. Which result seems more “reasonable”? Briefly discuss what other physics might be important to include to understand the actual surface temperature of Earth. This apparently more realistic model thus seems to give a temperature that is much lower than the typical temperature of the actual Earth. ...
click here
... • Stars of given type of spectrum and the same colors have the same absolute magnitude (99.9%) • Stars have different apparent magnitudes depending on their distance. • Stars behind dust clouds look redder than they are intrinsically, so… m-M=5 log d1 –5+ A(l) (i.e., the star looks fainter) ...
... • Stars of given type of spectrum and the same colors have the same absolute magnitude (99.9%) • Stars have different apparent magnitudes depending on their distance. • Stars behind dust clouds look redder than they are intrinsically, so… m-M=5 log d1 –5+ A(l) (i.e., the star looks fainter) ...
hubble_refurb
... The wispy, glowing, magenta structures in this image are the remains of a star 10 to 15 times the mass of the Sun that we would have seen exploding as a supernova 3,000 years ago. The remnant’s fast-moving gas is plowing into the surrounding gas of the galaxy, creating a supersonic shock wave in th ...
... The wispy, glowing, magenta structures in this image are the remains of a star 10 to 15 times the mass of the Sun that we would have seen exploding as a supernova 3,000 years ago. The remnant’s fast-moving gas is plowing into the surrounding gas of the galaxy, creating a supersonic shock wave in th ...
Magnitude. . . ?
... reads that “the minor planet was of fifteenth brightness class”, i.e., that its faintness was approximately fifteen magnitudes, one understands that it was some one million times fainter than Vega, or than a fixed star of zero-th brightness class (fifteen is three times five, and the third power of ...
... reads that “the minor planet was of fifteenth brightness class”, i.e., that its faintness was approximately fifteen magnitudes, one understands that it was some one million times fainter than Vega, or than a fixed star of zero-th brightness class (fifteen is three times five, and the third power of ...
Lecture6
... • The protostar gets hot and luminous enough to shine when the temperature gets to about 3000 K (so it should look red). • This newborn protostar is surrounded and protected by a dense cocoon of grains and gas which absorbs visible light from the star, and so a protostar is hard to see by visible li ...
... • The protostar gets hot and luminous enough to shine when the temperature gets to about 3000 K (so it should look red). • This newborn protostar is surrounded and protected by a dense cocoon of grains and gas which absorbs visible light from the star, and so a protostar is hard to see by visible li ...
Polaris
... Recent research reported in Science suggests that Polaris is 2.5 times brighter today than when Ptolemy observed it (now 2mag, antiquity 3mag). The astronomer Edward Guinan considers this to be a remarkable rate of change and is on record as saying that "If they are real, these changes are 100 times ...
... Recent research reported in Science suggests that Polaris is 2.5 times brighter today than when Ptolemy observed it (now 2mag, antiquity 3mag). The astronomer Edward Guinan considers this to be a remarkable rate of change and is on record as saying that "If they are real, these changes are 100 times ...
Triangulation Trigonometric Parallax
... • The Stefan-Boltzmann law is a key to understanding the H-R diagram – For stars of a given temperature, the larger the radius, the larger the luminosity – Therefore, as one moves up the H-R diagram, a star’s radius must become bigger – On the other hand, for a given luminosity, the larger the radiu ...
... • The Stefan-Boltzmann law is a key to understanding the H-R diagram – For stars of a given temperature, the larger the radius, the larger the luminosity – Therefore, as one moves up the H-R diagram, a star’s radius must become bigger – On the other hand, for a given luminosity, the larger the radiu ...
Study Guide for the Comprehensive Final Exam
... 9. Draw and label the horizon, meridian, zenith, celestial poles and celestial equator on the celestial sphere for an observer at any latitude. 10. Draw the apparent motion of stars as seen by any observer looking North, East, South or West at any location in the northern hemisphere. 11. Define a co ...
... 9. Draw and label the horizon, meridian, zenith, celestial poles and celestial equator on the celestial sphere for an observer at any latitude. 10. Draw the apparent motion of stars as seen by any observer looking North, East, South or West at any location in the northern hemisphere. 11. Define a co ...
SPECTRAL ANALYSIS OF A NEWLY DISCOVERED HgMn STAR
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.