Hot Horizontal Branch Stars in the Galactic Bulge. I
... http://www.cfht.hawaii.edu/∼ bernt/gsc/gscbrowser.html to identify 271 guide stars from Hubble Space Telescope. An astrometric solution was found which included a single frame scale in α, δ, a rotation angle, and quadratic terms in row and column position. The resulting solution had an r.m.s. scatte ...
... http://www.cfht.hawaii.edu/∼ bernt/gsc/gscbrowser.html to identify 271 guide stars from Hubble Space Telescope. An astrometric solution was found which included a single frame scale in α, δ, a rotation angle, and quadratic terms in row and column position. The resulting solution had an r.m.s. scatte ...
An Unbiased Near-infrared Interferometric Survey for Hot
... evolution of extrasolar planetary systems. However, debris discs that are relatively easy to detect are located several astronomical units (au) to a few hundreds of au from their host stars, and thus only trace the outer regions of planetary systems. In order to study the inner regions close to the ...
... evolution of extrasolar planetary systems. However, debris discs that are relatively easy to detect are located several astronomical units (au) to a few hundreds of au from their host stars, and thus only trace the outer regions of planetary systems. In order to study the inner regions close to the ...
Distance determination for RAVE stars using stellar models
... Therefore the isochrones or stellar tracks from a given model can be seen as samples from the theoretical stars defined by F0 (Z, τ, m). Throughout this paper we assume solar-scaled metallicities, which means that [α/Fe] = 0 and [M/H] = [Fe/H], where [M/H] is defined as log(Z/Z ). For our study we ...
... Therefore the isochrones or stellar tracks from a given model can be seen as samples from the theoretical stars defined by F0 (Z, τ, m). Throughout this paper we assume solar-scaled metallicities, which means that [α/Fe] = 0 and [M/H] = [Fe/H], where [M/H] is defined as log(Z/Z ). For our study we ...
A search for debris disks in the Herschel
... QSOs or unresolved galaxies whose optical colours are reddened into the main sequence locus (Ivezić et al. 2002). Indeed, the sample have a median r-band magnitude of 19.8, fainter than the value at which galaxies dominate over stars (Covey et al. 2007). Unsurprisingly due to their optical colours, ...
... QSOs or unresolved galaxies whose optical colours are reddened into the main sequence locus (Ivezić et al. 2002). Indeed, the sample have a median r-band magnitude of 19.8, fainter than the value at which galaxies dominate over stars (Covey et al. 2007). Unsurprisingly due to their optical colours, ...
Galaxies - University of Iowa Astrophysics
... Why are Cepheid variable stars useful in determining distances? 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. ...
... Why are Cepheid variable stars useful in determining distances? 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. ...
Tycho Brahe
... New Star • A supernova was observed in Cassiopeia for 18 months. • Using a sextant he observed that the new star was not moving in relationship to other stars. • This observation challenged the beliefs of the time that the heavens remain ...
... New Star • A supernova was observed in Cassiopeia for 18 months. • Using a sextant he observed that the new star was not moving in relationship to other stars. • This observation challenged the beliefs of the time that the heavens remain ...
PP Chapter 28 Text
... We see the Sun’s luminosity as LSun. If we were on a spaceship twice as far away from the Sun, its apparent brightness would appear A. B. C. D. ...
... We see the Sun’s luminosity as LSun. If we were on a spaceship twice as far away from the Sun, its apparent brightness would appear A. B. C. D. ...
course objectives - Metropolitan Community College
... Describe heat transfer methods that transport solar energy from the center of the sun outward. Outline the solar neutrino problem. Describe the basic characteristics of the solar atmosphere. Graph a typical pattern of sunspot numbers over time ...
... Describe heat transfer methods that transport solar energy from the center of the sun outward. Outline the solar neutrino problem. Describe the basic characteristics of the solar atmosphere. Graph a typical pattern of sunspot numbers over time ...
Starburst Galaxies - Beck-Shop
... by the arms. The reason why the arms stand out so sharply from the rest of the disk is that they contain numerous star-forming regions. In those regions the massive hot young stars are extremely bright and outshine the far more numerous less massive stars. Few starforming regions are to be found in ...
... by the arms. The reason why the arms stand out so sharply from the rest of the disk is that they contain numerous star-forming regions. In those regions the massive hot young stars are extremely bright and outshine the far more numerous less massive stars. Few starforming regions are to be found in ...
Lecture21 - Michigan State University
... sky as a streak of dim white light stretching from horizon to horizon • All the stars we can see in the night sky are in the Milky Way • The Milky Way is a flat, spiral galaxy containing 200 billion stars • The picture on the right is the center of the Milky Way taken with infrared ISP 205 - Astrono ...
... sky as a streak of dim white light stretching from horizon to horizon • All the stars we can see in the night sky are in the Milky Way • The Milky Way is a flat, spiral galaxy containing 200 billion stars • The picture on the right is the center of the Milky Way taken with infrared ISP 205 - Astrono ...
What Are the Faint X-ray Transients Near the Galactic Center?
... Another LMXB (0.1 pc from Sgr A*) with Periodic Eclipses ...
... Another LMXB (0.1 pc from Sgr A*) with Periodic Eclipses ...
ASTRONOMY AND ASTROPHYSICS Barium abundances in cool
... metal-poor stars ([Fe/H] < ; : ) barium is underabundant relative to iron by ; : dex, and [Ba/Fe] grows with increasing metallicity and reaches a solar value at about [Fe/H] ; : . The second feature is the large scatter of the data. It is within 0.5 dex at [Fe/H] > ; : and increases up to 1 dex for ...
... metal-poor stars ([Fe/H] < ; : ) barium is underabundant relative to iron by ; : dex, and [Ba/Fe] grows with increasing metallicity and reaches a solar value at about [Fe/H] ; : . The second feature is the large scatter of the data. It is within 0.5 dex at [Fe/H] > ; : and increases up to 1 dex for ...
Homologous Stars: Simple Scaling Relations
... The case n = 0 corresponds to incompressible fluid, i.e. ρ = ρc = const, P = Pc θ, and it requires rewriting eq. (poly.6) in a different form. In this case pressure vanishes at the surface, but density is the same throughout the ”star”. This solution is a crude approximation to the interior structur ...
... The case n = 0 corresponds to incompressible fluid, i.e. ρ = ρc = const, P = Pc θ, and it requires rewriting eq. (poly.6) in a different form. In this case pressure vanishes at the surface, but density is the same throughout the ”star”. This solution is a crude approximation to the interior structur ...
Chapter18.1
... • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit). © 2010 Pearson Education, Inc. ...
... • As a white dwarf’s mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar limit). © 2010 Pearson Education, Inc. ...
Locating Geographic Coordinates Using Observations over the Sun
... sunrise and sunset the Sun ascends to its highest point relative to horizon. This event defines solar noon. The interval from sunrise to sunset sets the length of the day [1]. As mentioned in the introduction, the objective of my first experiment was to observe the seasonal variations of the noon Su ...
... sunrise and sunset the Sun ascends to its highest point relative to horizon. This event defines solar noon. The interval from sunrise to sunset sets the length of the day [1]. As mentioned in the introduction, the objective of my first experiment was to observe the seasonal variations of the noon Su ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.