The Life and Times of a Neutron Star
... Exotic neutron stars may not be so rare. • Highly magnetized neutron stars may be as common as standard radio pulsars, but they don’t radio out their locations so they are harder to find. ...
... Exotic neutron stars may not be so rare. • Highly magnetized neutron stars may be as common as standard radio pulsars, but they don’t radio out their locations so they are harder to find. ...
Document
... Blazars are powerful gamma-ray sources. The most powerful of them have equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been de ...
... Blazars are powerful gamma-ray sources. The most powerful of them have equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been de ...
RSP Plans
... form of small anisotropies in its temperature These anisotropies contain information about basic cosmological parameters (e.g. total energy density and curvature of the universe) ...
... form of small anisotropies in its temperature These anisotropies contain information about basic cosmological parameters (e.g. total energy density and curvature of the universe) ...
- IRSF: Past and Future
... Gamma-ray binaries are a subclass of X-ray binaries that emit the majority of the energy in the gamma-ray band. They are comprised of a compact object and a massive (>10 Msun) star with a circumstellar disk or strong stellar wind. Their emission, ranging from radio to TeV gamma-rays, show variations ...
... Gamma-ray binaries are a subclass of X-ray binaries that emit the majority of the energy in the gamma-ray band. They are comprised of a compact object and a massive (>10 Msun) star with a circumstellar disk or strong stellar wind. Their emission, ranging from radio to TeV gamma-rays, show variations ...
pasta Jos´e A. Pons , Daniele Vigan`o and Nanda Rea
... In the absence of a more detailed microscopical calculation, we can use the impurity parameter formalism as a first simplified approximation to the complex calculation of the resistivity. The impurity parameter, Qimp , is a measure of the distribution of the nuclide charge numbers in the crust mate ...
... In the absence of a more detailed microscopical calculation, we can use the impurity parameter formalism as a first simplified approximation to the complex calculation of the resistivity. The impurity parameter, Qimp , is a measure of the distribution of the nuclide charge numbers in the crust mate ...
Radio Bubbles, Cooling X-ray Gas, Galaxy Interactions, and Star
... solution to the header of the combined narrow-band image using tools available in WCSTools (v. 3.6.3, available from the Smithsonian Astrophysical Observatories). We matched the positions of 13 objects in the field to a catalog of USNO-A2 stars and galaxies. These measurements provided the central a ...
... solution to the header of the combined narrow-band image using tools available in WCSTools (v. 3.6.3, available from the Smithsonian Astrophysical Observatories). We matched the positions of 13 objects in the field to a catalog of USNO-A2 stars and galaxies. These measurements provided the central a ...
PPT
... Nebula into Eridanus Superbubble X-ray outflow carries – Hot gas – Fresh nucleosynthetic products from O stars (26Al??) ...
... Nebula into Eridanus Superbubble X-ray outflow carries – Hot gas – Fresh nucleosynthetic products from O stars (26Al??) ...
CV - iucaa
... • “Astrosat – A Multi-wavelength satellite”, Explosive transients in the universe, Greece, September 2013 • “Time domain science with Indian telescopes”, Caltech, August 2013 • “Building X-ray Telescopes”, IISc, April 2013 Publications • Singer, L. P., Kasliwal, M. M., Cenko, S. B., et al. The Needl ...
... • “Astrosat – A Multi-wavelength satellite”, Explosive transients in the universe, Greece, September 2013 • “Time domain science with Indian telescopes”, Caltech, August 2013 • “Building X-ray Telescopes”, IISc, April 2013 Publications • Singer, L. P., Kasliwal, M. M., Cenko, S. B., et al. The Needl ...
Like a boiling teakettle atop a COLD stove, the sun`s HOT outer
... themselves to neutralize it. And if a plasma cannot sustain an electric field, it cannot move relative to the magnetic field (or vice versa), because to do so would induce an electric field. This is why astronomers talk about magnetic fields being “frozen” into plasmas. This principle can be quantif ...
... themselves to neutralize it. And if a plasma cannot sustain an electric field, it cannot move relative to the magnetic field (or vice versa), because to do so would induce an electric field. This is why astronomers talk about magnetic fields being “frozen” into plasmas. This principle can be quantif ...
Copyright 2004 Society of Photo-Optical Instrumentation Engineers. This
... NASA’s Chandra X-ray Observatory (CXO) is the most powerful X-ray telescope ever built to-date. Its launch in 1999 was a major milestone in the field of high energy astrophysics and the world of science. In the past four years, it has brought many new discoveries to the general public as well as the ...
... NASA’s Chandra X-ray Observatory (CXO) is the most powerful X-ray telescope ever built to-date. Its launch in 1999 was a major milestone in the field of high energy astrophysics and the world of science. In the past four years, it has brought many new discoveries to the general public as well as the ...
main characteristics of the emission from elliptical galaxies
... In order to unveil their properties, such as their structure or chemical composition, one must study their spectral emission. In fact they seem to behave rather dierently when observed with dierent eyes. This is because their light is mainly brought by two dierent components: optical radiation ar ...
... In order to unveil their properties, such as their structure or chemical composition, one must study their spectral emission. In fact they seem to behave rather dierently when observed with dierent eyes. This is because their light is mainly brought by two dierent components: optical radiation ar ...
The nature of the ultraluminous X-ray sources inside galaxies and
... O stars. However, the detected QSOs associated with Arp 220, using its redshift z = 0.018 and H 0 = 60 km s−1 Mpc−1 lie at a distance of ∼90 Mpc. Thus they are much more luminous with M = −16. In the cases in which QSOs have been found to be clustered about active galaxies the scale of the clusterin ...
... O stars. However, the detected QSOs associated with Arp 220, using its redshift z = 0.018 and H 0 = 60 km s−1 Mpc−1 lie at a distance of ∼90 Mpc. Thus they are much more luminous with M = −16. In the cases in which QSOs have been found to be clustered about active galaxies the scale of the clusterin ...
in the milky way - Chandra X
... Galaxy is a teeming and tumultuous place. There are supernova remnants: SNR 0.9-0.1, Sagittarius A East, and probably the X-ray Thread. There are many bright X-ray sources, which astronomers believe are binary systems—or pairs of orbiting objects—that contain a black hole or a neutron star (the 1E s ...
... Galaxy is a teeming and tumultuous place. There are supernova remnants: SNR 0.9-0.1, Sagittarius A East, and probably the X-ray Thread. There are many bright X-ray sources, which astronomers believe are binary systems—or pairs of orbiting objects—that contain a black hole or a neutron star (the 1E s ...
SOFT X-RAY EMISSIONS FROM PLANETS, MOONS, AND COMETS
... Terrestrial x-rays were discovered in the 1950s. The launch of the first x-ray satellite UHURU in 1970 marked the beginning of satellite-based x-ray astronomy. Subsequently launched x-ray observatories - Einstein, and particularly Rontgensatellit (ROSAT), made important contributions to planetary x- ...
... Terrestrial x-rays were discovered in the 1950s. The launch of the first x-ray satellite UHURU in 1970 marked the beginning of satellite-based x-ray astronomy. Subsequently launched x-ray observatories - Einstein, and particularly Rontgensatellit (ROSAT), made important contributions to planetary x- ...
Some Examples of Virtual Observatory Enabled Science What Are the Some Distinguishing
... Radio Galaxies: Typical Examples Radio overlayed on optical images ...
... Radio Galaxies: Typical Examples Radio overlayed on optical images ...
Neutron Star Crustal Emission: a basic, unanswered question.
... 2) Other options : NS models based on a two-T surface distribution (Pons et al, 2002; Walter & Lattimer, ...
... 2) Other options : NS models based on a two-T surface distribution (Pons et al, 2002; Walter & Lattimer, ...
Indications for an influence of Hot Jupiters
... Methods. We have developed a novel approach to test for systematic activity enhancements in planet-hosting stars. We use wide (several 100 AU) binary systems in which one of the stellar components is known to have an exoplanet, while the second stellar component does not have a detected planet and t ...
... Methods. We have developed a novel approach to test for systematic activity enhancements in planet-hosting stars. We use wide (several 100 AU) binary systems in which one of the stellar components is known to have an exoplanet, while the second stellar component does not have a detected planet and t ...
samba2002v2
... reconstruction of the photoemission angle is possible by evaluating the absorption point (or impact point) identified, in the first pass algorithm, with the barycentre. In asymmetric charge distributions, the third momentum (M3) lies along the major axis on the side, with respect to the barycentre, ...
... reconstruction of the photoemission angle is possible by evaluating the absorption point (or impact point) identified, in the first pass algorithm, with the barycentre. In asymmetric charge distributions, the third momentum (M3) lies along the major axis on the side, with respect to the barycentre, ...
DISCOVERY OF HOT SUPERGIANT STARS NEAR THE GALACTIC
... star counterparts (Lbol 105 Y106 L ) to X-ray sources within a projected distance of 30 pc from Sgr A (Muno et al. 2006b; Mikles et al. 2006). The objects found may be either massive Wolf-Rayet (WR)/O stars in colliding-wind binaries (CWBs), accreting neutron stars and black holes in high-mass X ...
... star counterparts (Lbol 105 Y106 L ) to X-ray sources within a projected distance of 30 pc from Sgr A (Muno et al. 2006b; Mikles et al. 2006). The objects found may be either massive Wolf-Rayet (WR)/O stars in colliding-wind binaries (CWBs), accreting neutron stars and black holes in high-mass X ...
X-Ray Scattering from Warm Dense Matter at Vulcan
... materials may be investigated through X-ray diffraction, the structure and dynamics of WDM may be investigated by angularly resolving the scatter of Xrays through this matter. Creating uniform WDM samples in the laboratory is not a trivial task and diagnosis of the plasma conditions requires a brigh ...
... materials may be investigated through X-ray diffraction, the structure and dynamics of WDM may be investigated by angularly resolving the scatter of Xrays through this matter. Creating uniform WDM samples in the laboratory is not a trivial task and diagnosis of the plasma conditions requires a brigh ...
ppt - IASF Milano
... •There are very few constraints on groups scale (1013 ≤ M ≤ 1014 Msun) , where numerical predictions are more accurate because a large number of halo can be simulated. ...
... •There are very few constraints on groups scale (1013 ≤ M ≤ 1014 Msun) , where numerical predictions are more accurate because a large number of halo can be simulated. ...
Advanced information on the Nobel Prize in Physics 2002, 8 October
... developed X-ray spectroscopy of atoms and got the Prize for this in 1924. This intensive development took place more than half a century before X-ray astronomy could be developed. The basic reason for the slow start of X-ray astronomy was the fact that X-rays from the universe are effectively absorb ...
... developed X-ray spectroscopy of atoms and got the Prize for this in 1924. This intensive development took place more than half a century before X-ray astronomy could be developed. The basic reason for the slow start of X-ray astronomy was the fact that X-rays from the universe are effectively absorb ...
Document
... long P, high amplitude High density short P, low amplitude Density profile decides how deep the pulsations penetrate in the star. ...
... long P, high amplitude High density short P, low amplitude Density profile decides how deep the pulsations penetrate in the star. ...
Deep Chandra Observations of the Arches and Quintuplet Clusters at... Hui Dong Q. Daniel Wang ( &
... contamination of faint undetected point-like sources could be upto ∼ 65%, but mostly at energies ≤ 4 keV. The remaining diffuse emission can be characterized by a plasma with a temperature of ∼ 5 × 107 K. The 0.3-8 keV luminosity of the emission is 1.6×1033 ergs s−1 for Quintuplet and 7.7×1033 ergs ...
... contamination of faint undetected point-like sources could be upto ∼ 65%, but mostly at energies ≤ 4 keV. The remaining diffuse emission can be characterized by a plasma with a temperature of ∼ 5 × 107 K. The 0.3-8 keV luminosity of the emission is 1.6×1033 ergs s−1 for Quintuplet and 7.7×1033 ergs ...
Barium Stars Observed with the Coude Echelle Spectrometer
... extensive mixing earlier than in the double-shell phase. Virtually all Ba stars have low-mass companions (McClure, 1983, Astrophysical Journal 268, 384). Although separations appear too large for any close interaction to have occurred, their binary nature must be related somehow to the abundance pec ...
... extensive mixing earlier than in the double-shell phase. Virtually all Ba stars have low-mass companions (McClure, 1983, Astrophysical Journal 268, 384). Although separations appear too large for any close interaction to have occurred, their binary nature must be related somehow to the abundance pec ...
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation.X-ray emission is expected from astronomical objects that contain extremely hot gasses at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). Although X-rays have been observed emanating from the Sun since the 1940s, the discovery in 1962 of the first cosmic X-ray source was a surprise. This source is called Scorpius X-1 (Sco X-1), the first X-ray source found in the constellation Scorpius. The X-ray emission of Scorpius X-1 is 10,000 times greater than its visual emission, whereas that of the Sun is about a million times less. In addition, the energy output in X-rays is 100,000 times greater than the total emission of the Sun in all wavelengths. Based on discoveries in this new field of X-ray astronomy, starting with Scorpius X-1, Riccardo Giacconi received the Nobel Prize in Physics in 2002. It is now known that such X-ray sources as Sco X-1 are compact stars, such as neutron stars or black holes. Material falling into a black hole may emit X-rays, but the black hole itself does not. The energy source for the X-ray emission is gravity. Infalling gas and dust is heated by the strong gravitational fields of these and other celestial objects.Many thousands of X-ray sources are known. In addition, the space between galaxies in galaxy clusters is filled with a very hot, but very dilute gas at a temperature between 10 and 100 megakelvins (MK). The total amount of hot gas is five to ten times the total mass in the visible galaxies.