point-like
... • Spectral Energy Distribution (SED): spectrum over a broad energy range, usually radio through gamma-rays ...
... • Spectral Energy Distribution (SED): spectrum over a broad energy range, usually radio through gamma-rays ...
Extreme Physics Explorer - High Energy Astrophysics
... Black Holes, Magnetars & Neutron Stars are cosmic laboratories for Extreme Physics: • Gravity at the event horizon -- Black Holes Frame dragging, metric in strong gravity -- AGNs, BH binaries ...
... Black Holes, Magnetars & Neutron Stars are cosmic laboratories for Extreme Physics: • Gravity at the event horizon -- Black Holes Frame dragging, metric in strong gravity -- AGNs, BH binaries ...
Black Holes - Wayne State University Physics and Astronomy
... X-Ray Emission A visible star in a binary system loses some of its gas to its black-hole companion The gas material forms an accretion disk as it spirals onto the black hole Gas particles in the disk rub against each other and heat up from friction As the particles whirl closer to the event horizon ...
... X-Ray Emission A visible star in a binary system loses some of its gas to its black-hole companion The gas material forms an accretion disk as it spirals onto the black hole Gas particles in the disk rub against each other and heat up from friction As the particles whirl closer to the event horizon ...
A CHANDRA X-RAY STUDY OF THE DENSE GLOBULAR CLUSTER TERZAN... C. O. Heinke, P. D. Edmonds, J. E. Grindlay, and...
... transient low-mass X-ray binary (LMXB) EXO 1745248 in the cluster entered a rare high state during our 2000 August observation, complicating the analysis. Nevertheless, nine additional sources clearly associated with the cluster are also detected, ranging from LX ð0:5 2:5 keVÞ ¼ 5:6 1032 down to ...
... transient low-mass X-ray binary (LMXB) EXO 1745248 in the cluster entered a rare high state during our 2000 August observation, complicating the analysis. Nevertheless, nine additional sources clearly associated with the cluster are also detected, ranging from LX ð0:5 2:5 keVÞ ¼ 5:6 1032 down to ...
5. Star Formation and the Interstellar Medium in the Milky Way
... interstellar chemistry. Nonetheless, the great bulk of the relevant data come from heterodyne observations of rotational spectra at mm and sub-mm wavelengths. The high sensitivity, angular resolution, and mapping speed of the LMT will enable detailed investigations of the chemistry of interstellar m ...
... interstellar chemistry. Nonetheless, the great bulk of the relevant data come from heterodyne observations of rotational spectra at mm and sub-mm wavelengths. The high sensitivity, angular resolution, and mapping speed of the LMT will enable detailed investigations of the chemistry of interstellar m ...
PDF only - at www.arxiv.org.
... of the feedback process by which energy is transferred from the central massive black hole to the surrounding gas. The mechanism by which the filaments are stabilized against tidal shear and dissipation into the surrounding 4×107K gas has been unclear. Here we report new observations that resolve th ...
... of the feedback process by which energy is transferred from the central massive black hole to the surrounding gas. The mechanism by which the filaments are stabilized against tidal shear and dissipation into the surrounding 4×107K gas has been unclear. Here we report new observations that resolve th ...
GRB 130603B: No Compelling Evidence for Neutron Star Merger
... Several explanations of the rebrightening of the NIR afterglow of SHB 130603B around 9.41 days after burst have been proposed. These include a macronova/kilonova produced by a neutron star merger in a close binary [15, 16], a millisecond magnetar produced in neutron star merger in close binaries [30 ...
... Several explanations of the rebrightening of the NIR afterglow of SHB 130603B around 9.41 days after burst have been proposed. These include a macronova/kilonova produced by a neutron star merger in a close binary [15, 16], a millisecond magnetar produced in neutron star merger in close binaries [30 ...
42 SCIENTIFIC AMERICAN OCTOBER 2006 TEN
... problem is that deflagration should eject a large fraction of the white dwarf essentially unchanged, whereas observations suggest that at most a small part of the star remains unaltered. So the explosion cannot be a pure deflagration; some detonation must be involved. Theorists have yet to explain w ...
... problem is that deflagration should eject a large fraction of the white dwarf essentially unchanged, whereas observations suggest that at most a small part of the star remains unaltered. So the explosion cannot be a pure deflagration; some detonation must be involved. Theorists have yet to explain w ...
1 - Stars: Introduction
... • Is a spiral galaxy, about 50 kpc across and about 1 kpc thick • 1 parsec is 3.1 × 1016 m, or 3.26 light years (ly). • Distance between the Earth and the Sun is called the Astronomical Unit, 1 AU = ...
... • Is a spiral galaxy, about 50 kpc across and about 1 kpc thick • 1 parsec is 3.1 × 1016 m, or 3.26 light years (ly). • Distance between the Earth and the Sun is called the Astronomical Unit, 1 AU = ...
Studies on post-flare loop prominence of 1981 April 27
... be located behind the limb. From the rising of the X-ray count-rate in the lower energy channels, recorded by SMM GRS and SMM HXRBS, the onset of the limb flare of 198l April 27 probably occurred between 07:41-07 : 55 UT. At 07 : 59 UT, optically, a bright patch of a flare-like area was observed, on ...
... be located behind the limb. From the rising of the X-ray count-rate in the lower energy channels, recorded by SMM GRS and SMM HXRBS, the onset of the limb flare of 198l April 27 probably occurred between 07:41-07 : 55 UT. At 07 : 59 UT, optically, a bright patch of a flare-like area was observed, on ...
MHD seismology as a tool to diagnose the coronae of X
... which may generate the X-ray QPOs emitted from the stellar coronae (e.g., Antolin & Van Doorsselaere 2013). While, the kink oscillations in the tangled stellar loops w.r.t. L.O.S. can also cause the variation in the plasma column depth, and thus can generate the weak density perturbations as well as ...
... which may generate the X-ray QPOs emitted from the stellar coronae (e.g., Antolin & Van Doorsselaere 2013). While, the kink oscillations in the tangled stellar loops w.r.t. L.O.S. can also cause the variation in the plasma column depth, and thus can generate the weak density perturbations as well as ...
Interstellar Astrophysics Summary notes: Part 5
... when the object becomes a proper main sequence star. At this point it is simply the result of the release of gravitational energy due to collapse). Computer simulations of the star formation process allow us to follow how the temperature and luminosity of the protostar changes with time as the colla ...
... when the object becomes a proper main sequence star. At this point it is simply the result of the release of gravitational energy due to collapse). Computer simulations of the star formation process allow us to follow how the temperature and luminosity of the protostar changes with time as the colla ...
Document
... Create the integrated spectrum (due to target RGB star + stellar background) in a spaxel of 50mas x 50 mas a) decide characteristics of the target RGB star (magnitude, color, [Fe/H], [alpha/Fe], velocity) b) create the stellar background using a stellar population code developed by Joe Liske & E.Tol ...
... Create the integrated spectrum (due to target RGB star + stellar background) in a spaxel of 50mas x 50 mas a) decide characteristics of the target RGB star (magnitude, color, [Fe/H], [alpha/Fe], velocity) b) create the stellar background using a stellar population code developed by Joe Liske & E.Tol ...
saintonge_malaysia09.. - Galaxy Evolution and Environment
... - L* of the IR luminosity function at z=0.4 consistent for field and cluster, but group in excess ...
... - L* of the IR luminosity function at z=0.4 consistent for field and cluster, but group in excess ...
M sun
... Pistol star: initial mass ~ 200 Msun (but too metal rich to collapse into a BH) R145 in 30 Dor: M sin3i = (140 +/- 37) Msun ...
... Pistol star: initial mass ~ 200 Msun (but too metal rich to collapse into a BH) R145 in 30 Dor: M sin3i = (140 +/- 37) Msun ...
File - Adriana Romo
... Interviewer: How did the white dwarf get its name? Scientist: They got their name because of the white color of the first few white dwarfs discovered. Interviewer: How are white dwarfs characterized? Scientist: They are characterized by a low luminosity, a mass close to that of our sun,and radius o ...
... Interviewer: How did the white dwarf get its name? Scientist: They got their name because of the white color of the first few white dwarfs discovered. Interviewer: How are white dwarfs characterized? Scientist: They are characterized by a low luminosity, a mass close to that of our sun,and radius o ...
X-Ray and Extreme Ultraviolet Emission from Comets
... other sources of X-ray emission in the solar system, the structure of the solar wind in the heliosphere, and the source of the local soft X-ray background. ...
... other sources of X-ray emission in the solar system, the structure of the solar wind in the heliosphere, and the source of the local soft X-ray background. ...
Observational Data
... It is likely that the disk of the Milky Way has been formed by continuous accretion of gas from the reservoir, such as the Galactic halo and the IGM, but our simulation already takes into account cosmological gas infall. Our simulation does not take into account the effect of ionizing radiation fiel ...
... It is likely that the disk of the Milky Way has been formed by continuous accretion of gas from the reservoir, such as the Galactic halo and the IGM, but our simulation already takes into account cosmological gas infall. Our simulation does not take into account the effect of ionizing radiation fiel ...
poster_IAU244 - ANU - Australian National University
... The figure to right shows the Hα emission line luminosity plotted against the restframe 1.4 GHz radio continuum luminosity for all 348 'Fujita galaxies' at z = 0.24. The plotted line is the observed relationship found at z 0 (Sullivan et al. 2001, ApJ, 558, 72). The black triangle is a interacting ...
... The figure to right shows the Hα emission line luminosity plotted against the restframe 1.4 GHz radio continuum luminosity for all 348 'Fujita galaxies' at z = 0.24. The plotted line is the observed relationship found at z 0 (Sullivan et al. 2001, ApJ, 558, 72). The black triangle is a interacting ...
CoRoT Observations of O Stars: Diverse Origins of Variability
... curves of Miras and red supergiants, as well as X-ray light curves of active galaxies, dwarf novae and high-mass X-ray binaries. It is not very frequent that a quantitative model is presented for such red noise, however. Usually only a qualitative explanation in terms of something stochastic or quas ...
... curves of Miras and red supergiants, as well as X-ray light curves of active galaxies, dwarf novae and high-mass X-ray binaries. It is not very frequent that a quantitative model is presented for such red noise, however. Usually only a qualitative explanation in terms of something stochastic or quas ...
Quasars- The Brightest Black Holes
... unidentified sources, 3C273, when it would be eclipsed by the Moon three times - in May, August and October. The advantage of such an event is that we always know the position of the Moon exactly. If one then compares the precise location of the edge of its disc against the sky at the moments when t ...
... unidentified sources, 3C273, when it would be eclipsed by the Moon three times - in May, August and October. The advantage of such an event is that we always know the position of the Moon exactly. If one then compares the precise location of the edge of its disc against the sky at the moments when t ...
astronomy - Scioly.org
... variability. Because of their large radii, they are more luminous than main-sequence stars of similar mass. Because of their youth, they are typically found near molecular clouds. -S Doradus variables are extremely rare, extremely massive, and extremely luminous stars. They are also known as Luminou ...
... variability. Because of their large radii, they are more luminous than main-sequence stars of similar mass. Because of their youth, they are typically found near molecular clouds. -S Doradus variables are extremely rare, extremely massive, and extremely luminous stars. They are also known as Luminou ...
Measurements of Dark Energy Lecture 2: Expansion Kinematics
... the combination – most assume “Planck prior” This implicitly assumes that systematics are re-parameterised into nuisance parameters and marginalised over... Analysis can then be done using simple approximation to the joint likelihood – with all parameter degeneracies are broken, high S/N ...
... the combination – most assume “Planck prior” This implicitly assumes that systematics are re-parameterised into nuisance parameters and marginalised over... Analysis can then be done using simple approximation to the joint likelihood – with all parameter degeneracies are broken, high S/N ...
From galaxies to stars
... The core can no longer support itself. Electrons are forced to combine with protons to form neutrons, and the whole core compacts down to a ball of neutrons only 20 km across: a neutron star. Meanwhile, the outer layers of the star fall inwards until they hit the newborn neutron star. When they me ...
... The core can no longer support itself. Electrons are forced to combine with protons to form neutrons, and the whole core compacts down to a ball of neutrons only 20 km across: a neutron star. Meanwhile, the outer layers of the star fall inwards until they hit the newborn neutron star. When they me ...
PDF format
... c) False. Such a black hole would measurably affect the orbits of the planets. d) False. X-ray observations would reveal its presence as it sucked in material around it. e) False. It would be readily apparent as a pulsating radio source in the outer solar system. © 2014 Pearson Education, Inc. ...
... c) False. Such a black hole would measurably affect the orbits of the planets. d) False. X-ray observations would reveal its presence as it sucked in material around it. e) False. It would be readily apparent as a pulsating radio source in the outer solar system. © 2014 Pearson Education, Inc. ...
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.