Universe Now - Course Pages of Physics Department
... – Stars that irregularly increase in brightness by a large factor. – Nova or dwarf nova: occurs in semidetached binaries where a white dwarf star is accreting matter from an ordinary companion star. When the accreted layer is about half a meter thick, the temperature at the bottom of the layer incre ...
... – Stars that irregularly increase in brightness by a large factor. – Nova or dwarf nova: occurs in semidetached binaries where a white dwarf star is accreting matter from an ordinary companion star. When the accreted layer is about half a meter thick, the temperature at the bottom of the layer incre ...
Living alongside Monsters: Matter around Central Massive Black Holes Q. Daniel Wang
... 1.87 and 1.90 μm narrow bands: on and off Pα line; Wang et al. 2009 ...
... 1.87 and 1.90 μm narrow bands: on and off Pα line; Wang et al. 2009 ...
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu
... ultraluminous X-ray sources • ULXs are non-nuclear X-ray point sources with Lx > 2 X 1039 erg/s, i.e., more luminous than the Eddington luminosity for stellar mass black holes, and could be intermediate mass black holes of 30 - 105 Ms ...
... ultraluminous X-ray sources • ULXs are non-nuclear X-ray point sources with Lx > 2 X 1039 erg/s, i.e., more luminous than the Eddington luminosity for stellar mass black holes, and could be intermediate mass black holes of 30 - 105 Ms ...
Research Powerpoint - Department of Astronomy
... coming from asteroid 596 Scheila after it was hit by another asteroid. On the right, comet Lulin, seen with Swift’s Xray (red) and UV (blue) telescopes. Comets glow in X-ray when the solar wind flows through the neutral gas (as seen here in UV). ...
... coming from asteroid 596 Scheila after it was hit by another asteroid. On the right, comet Lulin, seen with Swift’s Xray (red) and UV (blue) telescopes. Comets glow in X-ray when the solar wind flows through the neutral gas (as seen here in UV). ...
Stellar Remnants White Dwarfs, Neutron Stars & Black Holes
... • For Main Sequence stars of mass greater than about 20 Solar masses the remnant of the star left behind after a supernova explosion is too large (more than 3 Solar masses) to be a white dwarf or even a neutron star. • These remnants collapse to form Black Holes. • No light can escape from a Black H ...
... • For Main Sequence stars of mass greater than about 20 Solar masses the remnant of the star left behind after a supernova explosion is too large (more than 3 Solar masses) to be a white dwarf or even a neutron star. • These remnants collapse to form Black Holes. • No light can escape from a Black H ...
in the milky way - Chandra X
... Could a black hole in our Galaxy ever be strong enough to pull our solar system into it? It would have to be so close that its gravity could overcome the orbital acceleration of our solar system around the center of the Galaxy. That would be well within a light year, even for a million solar mass bl ...
... Could a black hole in our Galaxy ever be strong enough to pull our solar system into it? It would have to be so close that its gravity could overcome the orbital acceleration of our solar system around the center of the Galaxy. That would be well within a light year, even for a million solar mass bl ...
Blowing Bubbles in Space: The Birth and Death of Practically
... implies that the massive star's explosion has produced a shape similar to what is seen in some planetary nebulae associated with lower mass stars. • SMC=190 kly away, so this field of view spans about 150 light-years. ...
... implies that the massive star's explosion has produced a shape similar to what is seen in some planetary nebulae associated with lower mass stars. • SMC=190 kly away, so this field of view spans about 150 light-years. ...
Galaxy clusters - University of Iowa Astrophysics
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
Neutron Stars and Pulsars
... X-Ray Bursters • Powerful bursts of energy at irregular intervals. • The longer the period between bursts, the stronger the burst. • Explanation: Neutron star with a normal star companion. • Close enough for normal star material to pass through the inner Lagrangian point, form a disk around the neu ...
... X-Ray Bursters • Powerful bursts of energy at irregular intervals. • The longer the period between bursts, the stronger the burst. • Explanation: Neutron star with a normal star companion. • Close enough for normal star material to pass through the inner Lagrangian point, form a disk around the neu ...
Galaxy clusters - University of Iowa Astrophysics
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
... source, we can figure out the total mass in the lens. This provides an independent confirmation of dark matter. • A lense can act as a huge telescope. The deepest images of the most distant galaxies are obtained with clusters acting as gravitational lenses. ...
Stellar life after the Main Sequence (cont.)
... Another planetary nebula: M27 (we saw it during the field trip) ...
... Another planetary nebula: M27 (we saw it during the field trip) ...
Stars after the Main Sequence. Example: Betelgeuse (Alpha Orionis
... Another planetary nebula: M27 (we saw it during the field trip) ...
... Another planetary nebula: M27 (we saw it during the field trip) ...
Final for Astro 322, Prof. Heinke, April 23rd, 2010 Formula sheet
... d) Which of these features in elliptical galaxies indicate a recent merger? Explain for each feature, why it does or does not. i) Strong absorption lines of H. ii) Strong rotation. iii) “Disky” isophotes. iv) Spherical shells of stars. Problem 5: AGN & Clusters a) A distant quasar is observed to be ...
... d) Which of these features in elliptical galaxies indicate a recent merger? Explain for each feature, why it does or does not. i) Strong absorption lines of H. ii) Strong rotation. iii) “Disky” isophotes. iv) Spherical shells of stars. Problem 5: AGN & Clusters a) A distant quasar is observed to be ...
Document
... We have developed a physically meaningful line-profile model, yet one that is simple and not tied to any one proposed mechanism of hot-star X-ray production. Described in Owocki & Cohen (2001, ApJ, 559, 1108), the model assumes a smoothly and spherically symmetrically distributed accelerating X-ray ...
... We have developed a physically meaningful line-profile model, yet one that is simple and not tied to any one proposed mechanism of hot-star X-ray production. Described in Owocki & Cohen (2001, ApJ, 559, 1108), the model assumes a smoothly and spherically symmetrically distributed accelerating X-ray ...
PPT file
... in PRAO. It’s the most long set observations. 125 sources are in the modern list for observation once in the month. Here two type sources: super compact (~1au) gaze clouds in star formation regions and envelopes of variable late spectra classes stars. In star formation regions was found periodicity ...
... in PRAO. It’s the most long set observations. 125 sources are in the modern list for observation once in the month. Here two type sources: super compact (~1au) gaze clouds in star formation regions and envelopes of variable late spectra classes stars. In star formation regions was found periodicity ...
The Life and Times of a Neutron Star
... Z Magnetic stress builds in the crust until it fractures and the field rearranges itself locally leading to hard X-ray burst. Z ...
... Z Magnetic stress builds in the crust until it fractures and the field rearranges itself locally leading to hard X-ray burst. Z ...
Galaxies and Stars Questions KEY
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
First generation stars
... • 1) n_h~10^4 cc where LTE level population are achieved. Fragmentation mass scale ~100 solar masses. • 2) n_h>10^12 cc where gas become optical to H2 lines. Fragmentation mass scale <= 1-2 solar masses. ...
... • 1) n_h~10^4 cc where LTE level population are achieved. Fragmentation mass scale ~100 solar masses. • 2) n_h>10^12 cc where gas become optical to H2 lines. Fragmentation mass scale <= 1-2 solar masses. ...
Sharp Images of Galaxy Groups: Chandra and XMM Uncover New
... Bubbles, shocks, … Comparison with features observed at other wavelengths Extended radio features ...
... Bubbles, shocks, … Comparison with features observed at other wavelengths Extended radio features ...
Puzzling X-rays from the new colliding wind binary Wolf–Rayet 65
... swings behind the LBV star with its dense wind. It is hard to see how a similar model can be used to explain the X-ray variability of WR 65. Strong variations in the absorbing column indicate that the orbit of WR 65 has a high inclination too. Considering the light curve (Fig. 3), we can rule out th ...
... swings behind the LBV star with its dense wind. It is hard to see how a similar model can be used to explain the X-ray variability of WR 65. Strong variations in the absorbing column indicate that the orbit of WR 65 has a high inclination too. Considering the light curve (Fig. 3), we can rule out th ...
ppt - SLAC
... peak of the synchrotron spectral component of ~ 103 – 106, depending on the particular source • Degeneracy between B and gel is “broken” by spectral variability + spectral curvature (Perlman et al. 2005) • The high energy (Compton) component is produced by the same electrons as the synchrotron peak ...
... peak of the synchrotron spectral component of ~ 103 – 106, depending on the particular source • Degeneracy between B and gel is “broken” by spectral variability + spectral curvature (Perlman et al. 2005) • The high energy (Compton) component is produced by the same electrons as the synchrotron peak ...
Honors Question – Black Holes and Neutron Stars In Friday`s lecture
... In Friday's lecture, we learned that physicists think that black holes are mass singularities – an enormous mass concentrated in essentially a point. Since gravitational force increases as the distance decreases, it's natural to conclude that within some radius the gravitational force is so large th ...
... In Friday's lecture, we learned that physicists think that black holes are mass singularities – an enormous mass concentrated in essentially a point. Since gravitational force increases as the distance decreases, it's natural to conclude that within some radius the gravitational force is so large th ...
Geochemistry & Lab
... cool X-ray image of the nebula, from the Chandra X-ray Observatory). The stars that eventually become neutron stars are thought to start out with about 8 to 20-30 times the mass of our sun. These numbers are probably going to change as supernova simulations become more precise, but it appears that f ...
... cool X-ray image of the nebula, from the Chandra X-ray Observatory). The stars that eventually become neutron stars are thought to start out with about 8 to 20-30 times the mass of our sun. These numbers are probably going to change as supernova simulations become more precise, but it appears that f ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.