Slide 1
... power of supernovae. And light elements used in our technology were formed via cosmic rays. The solar nebula, from which our solar system was formed, was seeded with these elements, and they were present at the Earth's formation. Our very existence is connected to these elements, and to their cosmic ...
... power of supernovae. And light elements used in our technology were formed via cosmic rays. The solar nebula, from which our solar system was formed, was seeded with these elements, and they were present at the Earth's formation. Our very existence is connected to these elements, and to their cosmic ...
ms
... currently constrains at a significant level the neutron star equation of state, collectively, they point to neutron star radii that are in the 8-11 km range, which is consistent only with a subset of the proposed equations of state (see Özel, Baym, & Güver 2010). The two techniques mentioned above ...
... currently constrains at a significant level the neutron star equation of state, collectively, they point to neutron star radii that are in the 8-11 km range, which is consistent only with a subset of the proposed equations of state (see Özel, Baym, & Güver 2010). The two techniques mentioned above ...
MAGIC-II - (CTA) Japan
... MAGIC result: Published in Science in 2008 By measuring the spectrum around cutoff or at high energies is important to distinguish the emission model Polar cap: double exponent Outer gap: simple exponent ...
... MAGIC result: Published in Science in 2008 By measuring the spectrum around cutoff or at high energies is important to distinguish the emission model Polar cap: double exponent Outer gap: simple exponent ...
The X-ray Bursters Problem and its Implications to the Equation of
... We review the understating on X-ray bursting neutron stars, particularly the thermonuclear instabilities on accretion stars that produce thermonuclear (TypeI) X-ray bursts. These bursts are caused by unstable burning in the outer layers of the neutron star due to accreted material from a companion i ...
... We review the understating on X-ray bursting neutron stars, particularly the thermonuclear instabilities on accretion stars that produce thermonuclear (TypeI) X-ray bursts. These bursts are caused by unstable burning in the outer layers of the neutron star due to accreted material from a companion i ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... Stars earlier than about F5 (Teff ~ 8000 K) don’t have convective envelopes and don’t have any X-ray emission… Except that O and early B stars do have X-ray emission they are strong sources of soft X-rays. And they have strong stellar winds. ...
... Stars earlier than about F5 (Teff ~ 8000 K) don’t have convective envelopes and don’t have any X-ray emission… Except that O and early B stars do have X-ray emission they are strong sources of soft X-rays. And they have strong stellar winds. ...
Into the darkness peering
... Patrick Henry – U. Hawaii Abraham Loeb – Harvard U. Takamitsu Miyaji - CMU BALL Steven Jordan William Purcell ...
... Patrick Henry – U. Hawaii Abraham Loeb – Harvard U. Takamitsu Miyaji - CMU BALL Steven Jordan William Purcell ...
Radio Bubbles, Cooling X-ray Gas, Galaxy Interactions, and Star
... redshift systems may therefore give us insight into how AGN heating (and feedback) might have worked in the distant past. Semi-analytic studies currently make general assumptions about the efficiency of AGN feedback, tuned to suppress the formation of over-luminous, blue galaxies at the centers of c ...
... redshift systems may therefore give us insight into how AGN heating (and feedback) might have worked in the distant past. Semi-analytic studies currently make general assumptions about the efficiency of AGN feedback, tuned to suppress the formation of over-luminous, blue galaxies at the centers of c ...
poster
... objects (YSOs) in this region, which lacks high UV flux, and compare evolutionary trends with other young star forming clusters. We present results of our multiwavelength study of IRAS 20050+2720 which includes observations by Chandra, Spitzer, and 2MASS and UBVRI photometry. In total, about 300 YSO ...
... objects (YSOs) in this region, which lacks high UV flux, and compare evolutionary trends with other young star forming clusters. We present results of our multiwavelength study of IRAS 20050+2720 which includes observations by Chandra, Spitzer, and 2MASS and UBVRI photometry. In total, about 300 YSO ...
ly Searching the Sky: The Swift Mission and High Energy Physics Connections
... • IceCube reconstructs the position of each neutrino event (mostly atmospheric ν’s) • If a neutrino pair is observed, use their angular separation to test if they could both be from an astrophysical source (rather than pileup of background) • Search for an X-ray counterpart with Swift in a region ar ...
... • IceCube reconstructs the position of each neutrino event (mostly atmospheric ν’s) • If a neutrino pair is observed, use their angular separation to test if they could both be from an astrophysical source (rather than pileup of background) • Search for an X-ray counterpart with Swift in a region ar ...
No Slide Title - Harvard-Smithsonian Center for Astrophysics
... • Cranmer (2009) modeled equatorial zones of T Tauri stars as a collection of closed loops, energized by “footpoint shaking” (via blob-impact surface turbulence). ...
... • Cranmer (2009) modeled equatorial zones of T Tauri stars as a collection of closed loops, energized by “footpoint shaking” (via blob-impact surface turbulence). ...
Instruments and Methods of Astrophysical X-ray
... Einstein satellite that first introduced the X-ray Optics. The dramatic increase in sensitivity for the detection of faint sources and the capability to resolve extended source with imaging detectors in the focus of grazing incidence telescopes, that do not require rotation, made the mismatching in ...
... Einstein satellite that first introduced the X-ray Optics. The dramatic increase in sensitivity for the detection of faint sources and the capability to resolve extended source with imaging detectors in the focus of grazing incidence telescopes, that do not require rotation, made the mismatching in ...
ISOLATED, MASSIVE SUPERGIANTS NEAR THE GALACTIC
... emission there. The VLA observations identified 30 unresolved sources and 55 extended sources. The positions of the unresolved sources were accurate to 0B1. We searched for X-ray counterparts using the catalog in Muno et al. (2003). The positions of the X-ray sources in the Chandra catalog are accur ...
... emission there. The VLA observations identified 30 unresolved sources and 55 extended sources. The positions of the unresolved sources were accurate to 0B1. We searched for X-ray counterparts using the catalog in Muno et al. (2003). The positions of the X-ray sources in the Chandra catalog are accur ...
ATNF Steering Committee – Astrophysics highlights
... narrow ultra-relativistic jet (5o opening angle) responsible for the gamma ray and early optical emission; and a wide, mildly relativistic, component responsible for the radio emission and optical afterglow at later times. The ubiquity of jet phenomena was also shown in an unrelated paper by Fender ...
... narrow ultra-relativistic jet (5o opening angle) responsible for the gamma ray and early optical emission; and a wide, mildly relativistic, component responsible for the radio emission and optical afterglow at later times. The ubiquity of jet phenomena was also shown in an unrelated paper by Fender ...
A Dozen Colliding-Wind X-Ray Binaries in the Star - UvA-DARE
... We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 X-ray point sources with luminosities between 5 1032 and 2 1035 ergs s1 (0.2–3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type ...
... We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 X-ray point sources with luminosities between 5 1032 and 2 1035 ergs s1 (0.2–3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type ...
Nature paper - University of Southampton
... collapse of a lower-mass oxygen–neon–magnesium core as it loses pressure support owing to the sudden capture of electrons by neon and/or magnesium nuclei3,4. It has hitherto been impossible to identify the two distinct families of neutron stars produced in these formation channels. Here we report th ...
... collapse of a lower-mass oxygen–neon–magnesium core as it loses pressure support owing to the sudden capture of electrons by neon and/or magnesium nuclei3,4. It has hitherto been impossible to identify the two distinct families of neutron stars produced in these formation channels. Here we report th ...
the obscuration in liners - Instituto de Astronomía
... luminosity extending to low luminosity AGNs, independently of their accretion rates. These results clearly disfavour star formation as the dominant nuclear source in LLAGNs. Similar data for a sample of LINERs have been reported by Mason et al. (2011, in preparation). They found that indeed a simila ...
... luminosity extending to low luminosity AGNs, independently of their accretion rates. These results clearly disfavour star formation as the dominant nuclear source in LLAGNs. Similar data for a sample of LINERs have been reported by Mason et al. (2011, in preparation). They found that indeed a simila ...
X-ray binaries
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
Quiescent and flaring X-ray emission from the nearby M/T dwarf
... a 25 circular region around the source position and restricted the analysis to the 0.2–2.0 keV band, where most of the source photons were detected. Only during a large flare occurring in our observation, photons of higher energies were present and a harder band (0.2–3.0 keV) was used to study the ...
... a 25 circular region around the source position and restricted the analysis to the 0.2–2.0 keV band, where most of the source photons were detected. Only during a large flare occurring in our observation, photons of higher energies were present and a harder band (0.2–3.0 keV) was used to study the ...
Summary - X-ray Astronomy Group at ISAS
... number of very faint sourcesby 1980 it was clear that the number of objects required to make up the XRB exceeded (in surface density) that of known AGN by >10 However the x-ray spectra of the objects detected (clusters of galaxies, active galaxies, blazars etc) showed that none had the spectrum of t ...
... number of very faint sourcesby 1980 it was clear that the number of objects required to make up the XRB exceeded (in surface density) that of known AGN by >10 However the x-ray spectra of the objects detected (clusters of galaxies, active galaxies, blazars etc) showed that none had the spectrum of t ...
SOFT X-RAY EMISSIONS FROM PLANETS, MOONS, AND COMETS
... But to observe most of the soft x-ray band one has to be above ~100 km from Earth's surface. 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 - Ein ...
... But to observe most of the soft x-ray band one has to be above ~100 km from Earth's surface. 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 - Ein ...
Read the article
... by a black hole, in explaining the observed structure at the galactic center mediated by the presence of a hierarchically embedded spiral formation. We have also shown that there exists an enigmatic structure at the SgrA*, where magnetic braiding of plasma loops may have formed, whose tightening and ...
... by a black hole, in explaining the observed structure at the galactic center mediated by the presence of a hierarchically embedded spiral formation. We have also shown that there exists an enigmatic structure at the SgrA*, where magnetic braiding of plasma loops may have formed, whose tightening and ...
X-ray binaries
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
... and Magellanic Clouds LMXBs with NSs and BHs as accreting components. Donors can be WDs, or normal low-mass stars (main sequence or sub-giants). Many sources are found in globular clusters. Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an a ...
poster
... Figure 3: FUV emission lines observed with FUSE in CTTS and best fit Gaussian profiles ordered by the shift in the O vi 1032 Å line. For RU Lup an additional absorption component is used. ...
... Figure 3: FUV emission lines observed with FUSE in CTTS and best fit Gaussian profiles ordered by the shift in the O vi 1032 Å line. For RU Lup an additional absorption component is used. ...
The Milky Way at Different Wavelengths
... variations indicate variations of absorption or of the temperatures of emitting regions. The black regions indicate gaps in the ROSAT survey. Gamma Ray (100 MeV which corresponds to 1.2 x 10-14 m or 0.00012 Å ) (Angular resolution: ~120'; Intensity of high-energy gamma-ray emission observed by the E ...
... variations indicate variations of absorption or of the temperatures of emitting regions. The black regions indicate gaps in the ROSAT survey. Gamma Ray (100 MeV which corresponds to 1.2 x 10-14 m or 0.00012 Å ) (Angular resolution: ~120'; Intensity of high-energy gamma-ray emission observed by the E ...
Disks around low-mass stars in extreme environments
... only from core-collapse supernovae Must have been injected into the proto-solar nebula at most a few Myr after the formation of our Sun. Our solar system formed in an environment containing high-mass stars (M✶ > 30 M⊙) ...
... only from core-collapse supernovae Must have been injected into the proto-solar nebula at most a few Myr after the formation of our Sun. Our solar system formed in an environment containing high-mass stars (M✶ > 30 M⊙) ...
History of X-ray astronomy
The history of X-ray astronomy begins in the 1920s, with interest in short wave communications for the U.S. Navy. This was soon followed by extensive study of the earth's ionosphere. By 1927, interest in the detection of X-ray and ultraviolet (UV) radiation at high altitudes inspired researchers to launch Goddard's rockets into the upper atmosphere to support theoretical studies and data gathering. The first successful rocket flight equipped with instrumentation able to detect solar ultraviolet radiation occurred in 1946. X-ray solar studies began in 1949. By 1973 a solar instrument package orbited on Skylab providing significant solar data.In 1965 the Goddard Space Flight Center program in X-ray astronomy was initiated with a series of balloon-borne experiments. In the 1970s this was followed by high altitude sounding rocket experiments, and that was followed by orbiting (satellite) observatories.The first rocket flight to successfully detect a cosmic source of X-ray emission was launched in 1962 by a group at American Science and Engineering (AS&E).X-ray wavelengths reveal information about the bodies (sources) that emit them.