Abstracts - Physics of Evolved Stars 2015
... solar masses per year. Evolutionary models suggest that this phase does not last much longer than 10^5 years, implying that these stars are not likely to have lost more than one solar mass before entering the high mass-loss phase. To evolve into a post-AGB star, with a white dwarf cooling at the cen ...
... solar masses per year. Evolutionary models suggest that this phase does not last much longer than 10^5 years, implying that these stars are not likely to have lost more than one solar mass before entering the high mass-loss phase. To evolve into a post-AGB star, with a white dwarf cooling at the cen ...
A search for debris disks in the Herschel
... To identify candidate disks in our sample we apply a photometric distance cut to select the brightest and nearest objects that are least likely to be QSOs or unresolved galaxies and the most likely to be debris disks. We apply an initial photometric distance cut of 200 pc to select the most likely c ...
... To identify candidate disks in our sample we apply a photometric distance cut to select the brightest and nearest objects that are least likely to be QSOs or unresolved galaxies and the most likely to be debris disks. We apply an initial photometric distance cut of 200 pc to select the most likely c ...
Introduction to Galaxies - West Jefferson Local Schools
... • orbits of stars and gas are “circular”, rotating about disk axis • star formation is on-going; it is can be fairly constant over the age of the galaxy • gas and dust mass fraction is roughly 10-50% of full disk • due on-going star formation, ages of stars widely range from age of galaxy to new • s ...
... • orbits of stars and gas are “circular”, rotating about disk axis • star formation is on-going; it is can be fairly constant over the age of the galaxy • gas and dust mass fraction is roughly 10-50% of full disk • due on-going star formation, ages of stars widely range from age of galaxy to new • s ...
Binarity in carbon-enhanced metal-poor stars
... s-process elements (Herwig 2004), or some rotating AGB companions (Herwig, Langer & Lugaro 2003; Siess, Goriely & Langer 2004). However, this result is dependent on the parameters adopted, as shown by Piersanti, Cristallo & Straniero (2013). Komiya et al. (2007) argue that relative high-mass AGB sta ...
... s-process elements (Herwig 2004), or some rotating AGB companions (Herwig, Langer & Lugaro 2003; Siess, Goriely & Langer 2004). However, this result is dependent on the parameters adopted, as shown by Piersanti, Cristallo & Straniero (2013). Komiya et al. (2007) argue that relative high-mass AGB sta ...
Processing of Star Catalog and Star Image
... 6 × 9 × 9 = 486 sub-blocks and then the direction vector of each sub-block’s corresponding central axis can be obtained. 486 boresight pointings (direction vector) evenly distributed in the full sky resulting from this method and the angle between each pair of neighboring boresight pointings is 10°. ...
... 6 × 9 × 9 = 486 sub-blocks and then the direction vector of each sub-block’s corresponding central axis can be obtained. 486 boresight pointings (direction vector) evenly distributed in the full sky resulting from this method and the angle between each pair of neighboring boresight pointings is 10°. ...
Galaxies
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
Slide 1
... their electrons overlap. This happens for stars with cores up to 3 times heavier than the sun. This is the case with neutron stars. When a big core dies, gravity crushes down, but it crushes even harder than electron degeneracy pressure. As the electrons overlap, they merge with the protons to turn ...
... their electrons overlap. This happens for stars with cores up to 3 times heavier than the sun. This is the case with neutron stars. When a big core dies, gravity crushes down, but it crushes even harder than electron degeneracy pressure. As the electrons overlap, they merge with the protons to turn ...
It is now recognized that the vast majority of ellipticals are of
... brightnesses. As , we can substitute the previous correlation and see that and therefore: ...
... brightnesses. As , we can substitute the previous correlation and see that and therefore: ...
Galaxies - University of Iowa Astrophysics
... A) They all have the same distance. B) Their luminosity can be determined from their pulsation period. C) They all have the same luminosity. D) They all have the same radius. ...
... A) They all have the same distance. B) Their luminosity can be determined from their pulsation period. C) They all have the same luminosity. D) They all have the same radius. ...
Starwalk Manual En
... Star Walk™ is a stargazing application for amateurs, professionals, and kids who are eager to learn. The app allows users to identify about 250,000 heavenly bodies and learn about them, watch moon phases, meteor showers, see daily sunset and sunrise times, elevation angle, and daily hours of sunligh ...
... Star Walk™ is a stargazing application for amateurs, professionals, and kids who are eager to learn. The app allows users to identify about 250,000 heavenly bodies and learn about them, watch moon phases, meteor showers, see daily sunset and sunrise times, elevation angle, and daily hours of sunligh ...
The Nature of the Stars
... this is done by comparing how bright different stars appear. Perhaps the star Betelgeuse in the constellation Orion appears bright because it is relatively close, while the dimmer and less conspicuous star Polaris (the North Star, in the constellation Ursa Minor) is farther away. But this line of re ...
... this is done by comparing how bright different stars appear. Perhaps the star Betelgeuse in the constellation Orion appears bright because it is relatively close, while the dimmer and less conspicuous star Polaris (the North Star, in the constellation Ursa Minor) is farther away. But this line of re ...
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.