Pulsars
... • Probably not – brightness temperature of Xrays is about 1011 K, equivalent to electron energies 10MeV, so consistent with incoherent emission. radio coherent ...
... • Probably not – brightness temperature of Xrays is about 1011 K, equivalent to electron energies 10MeV, so consistent with incoherent emission. radio coherent ...
For silicon
... Intensity image is generated by collecting photoelectrons generated in 3-D volume into 2-D array of pixels. Optical and IR focal plane arrays both collect charges via electric fields. In the z-direction, optical and IR use a p-n junction to “sweep” charge toward pixel collection nodes. ...
... Intensity image is generated by collecting photoelectrons generated in 3-D volume into 2-D array of pixels. Optical and IR focal plane arrays both collect charges via electric fields. In the z-direction, optical and IR use a p-n junction to “sweep” charge toward pixel collection nodes. ...
Slide 1
... Interferometry can also be done with visible light but is much more difficult due to shorter wavelengths ...
... Interferometry can also be done with visible light but is much more difficult due to shorter wavelengths ...
Noise mechanisms superconducting tunnel-junction detectors
... Superconducting tunnel-junction detectors 共STJs兲 have demonstrated significant promise as nondispersive, photoncounting spectrometers for a broad range of energies, 1–10 eV.1–4 Applications in astrophysics and materials analysis will benefit from the improved energy resolution, predicted to be 2.8 e ...
... Superconducting tunnel-junction detectors 共STJs兲 have demonstrated significant promise as nondispersive, photoncounting spectrometers for a broad range of energies, 1–10 eV.1–4 Applications in astrophysics and materials analysis will benefit from the improved energy resolution, predicted to be 2.8 e ...
HEA_Pulsars_2002
... Emission processes in pulsars • Important processes in magnetic fields : - cyclotron Optical & X-ray emission in pulsars - synchrotron • Curvature radiation => radio emission B ...
... Emission processes in pulsars • Important processes in magnetic fields : - cyclotron Optical & X-ray emission in pulsars - synchrotron • Curvature radiation => radio emission B ...
poster
... (Wassell et al. 2006). Thus, while the number of counts is small, this feature is compatible with what we expect from a real knot, which was 3 times brighter in 2011. ...
... (Wassell et al. 2006). Thus, while the number of counts is small, this feature is compatible with what we expect from a real knot, which was 3 times brighter in 2011. ...
Measuring the surface temperature of stars by analysing their spectra
... atmosphere interacts with stellar light. This causes a so-called extinction that is much larger for the blue than for the red components of stellar light (also knwn as atmospheric reddening). Moreover, our sensor is more sensitive to red than to blue light: below about 5000 Å and moving towards 4000 ...
... atmosphere interacts with stellar light. This causes a so-called extinction that is much larger for the blue than for the red components of stellar light (also knwn as atmospheric reddening). Moreover, our sensor is more sensitive to red than to blue light: below about 5000 Å and moving towards 4000 ...
PDF only - at www.arxiv.org.
... advantageous to find out a proper methodology to infer the HEW from a direct calculation on the characteristic parameters of the surface roughness. In this work we attempt to provide with quantitative predictions of the HEW for the SIMBOL-X optical module, as a function of the photon energy, startin ...
... advantageous to find out a proper methodology to infer the HEW from a direct calculation on the characteristic parameters of the surface roughness. In this work we attempt to provide with quantitative predictions of the HEW for the SIMBOL-X optical module, as a function of the photon energy, startin ...
Physics of Particle Detection
... elements can be distinguished. The basic principle of particle detection is that every physics effect can be used as an idea to build a detector. In the following we distinguish between the interaction of charged and neutral particles. In most cases the observed signature of a particle is its ioniza ...
... elements can be distinguished. The basic principle of particle detection is that every physics effect can be used as an idea to build a detector. In the following we distinguish between the interaction of charged and neutral particles. In most cases the observed signature of a particle is its ioniza ...
Most-likely Black Holes
... • X-ray emission region is very small • No stable star exists with given mass & size ...
... • X-ray emission region is very small • No stable star exists with given mass & size ...
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 ...
Slide 1
... XRT can pinpoint GRBs to 5arcsec accuracy within 10 seconds of target acquisition for a typical GRB and can study the X-ray counterparts of GRBs beginning 20-70 seconds from burst discovery and continuing for days to weeks. ...
... XRT can pinpoint GRBs to 5arcsec accuracy within 10 seconds of target acquisition for a typical GRB and can study the X-ray counterparts of GRBs beginning 20-70 seconds from burst discovery and continuing for days to weeks. ...
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. ...
ppt
... Measurements of - or upper limits on - the stellar continuum constrains the IMF Sources expected to cover a range of metallicity from Z ~ 0 to 10-3 ...
... Measurements of - or upper limits on - the stellar continuum constrains the IMF Sources expected to cover a range of metallicity from Z ~ 0 to 10-3 ...
Monte Carlo simulations of X-ray absorption in the interstellar medium
... for visible light and of the absence of other detectors, it took a long time until one noticed that astronomical objects emit also light in other wavelengths. Karl Jansky was the first who observed a none optical signal from outside the solar syst ...
... for visible light and of the absence of other detectors, it took a long time until one noticed that astronomical objects emit also light in other wavelengths. Karl Jansky was the first who observed a none optical signal from outside the solar syst ...
SOLAR HARD X-RAY AND GAMMA-RAY OBSERVATIONS FROM
... accelerated during solar flares. Since the beginning of 1990 the PHEBUS instrument and the SIGMA anticoincidence shield aboard GRANAT have provided hard X-ray and gamma-ray observations of solar bursts in the energy range 0.075-124 and 0.200-15 MeV, respectively. After a brief description of the exp ...
... accelerated during solar flares. Since the beginning of 1990 the PHEBUS instrument and the SIGMA anticoincidence shield aboard GRANAT have provided hard X-ray and gamma-ray observations of solar bursts in the energy range 0.075-124 and 0.200-15 MeV, respectively. After a brief description of the exp ...
PowerPoint-Präsentation - Max-Planck
... telescopes at this source for many hours; in extreme cases, data for one celestial object may be accumulated for several hundred hours. The H.E.S.S. telescopes are operated at night when the moon is not visible (otherwise the sky is too bright to see the Cherenkov flashes), and will accumulate about ...
... telescopes at this source for many hours; in extreme cases, data for one celestial object may be accumulated for several hundred hours. The H.E.S.S. telescopes are operated at night when the moon is not visible (otherwise the sky is too bright to see the Cherenkov flashes), and will accumulate about ...
The Big Bang Is Bunk - 21stcenturysciencetech.com
... for observing will be where the band is at the-lowest geo graphic latitude, giving access to the sky as close as possible to the celestial equator and then up to the celestial pole. These places are (in the north) Georgian Bay in south eastern Ontario, Canada, and (in the south) southern Tas mani ...
... for observing will be where the band is at the-lowest geo graphic latitude, giving access to the sky as close as possible to the celestial equator and then up to the celestial pole. These places are (in the north) Georgian Bay in south eastern Ontario, Canada, and (in the south) southern Tas mani ...
Lecture 14: Non-Optical Telescopes )( )( 25.0)(" mD m a
... •The angle of bending limits the resolution of the telescope •This depends on the aperture of the telescope, D=2 x R •The bending angle is given by ...
... •The angle of bending limits the resolution of the telescope •This depends on the aperture of the telescope, D=2 x R •The bending angle is given by ...
PHY418 Particle Astrophysics
... following several years of observations by Vela defence satellites • these were designed to ...
... following several years of observations by Vela defence satellites • these were designed to ...
The Quadrupole Cusp: A Universal Accelerator, or From Radiation
... • Now that we know there are trapping regions of the cusp, e.g. periodic orbits, we can display those orbits with a Poincaré section. Then we can potentially demonstrate the invariant tori and chaotic orbits. • Unfortunately, I only realized the advantage of this approach after plotting 4000 traject ...
... • Now that we know there are trapping regions of the cusp, e.g. periodic orbits, we can display those orbits with a Poincaré section. Then we can potentially demonstrate the invariant tori and chaotic orbits. • Unfortunately, I only realized the advantage of this approach after plotting 4000 traject ...
Student copy of notes - User Web Areas at the University of York
... Eventually a neutron star is formed if the core is less than three solar masses. Neutron stars are incredibly dense - similar to the density of an atomic nucleus. They are typically 20 km across but more massive than the Sun. Because they contain so much mass within such a small volume, the gravitat ...
... Eventually a neutron star is formed if the core is less than three solar masses. Neutron stars are incredibly dense - similar to the density of an atomic nucleus. They are typically 20 km across but more massive than the Sun. Because they contain so much mass within such a small volume, the gravitat ...
Introductory Presentation on Cosmic Rays
... The sun is one of the sources of Cosmic Rays. Nuclei and electrons are accelerated by shock waves traveling through the Corona and by magnetic energy released in Solar flares. The Solar Wind contains roughly equal numbers of electrons and protons along with heavier ions and blows continuously from t ...
... The sun is one of the sources of Cosmic Rays. Nuclei and electrons are accelerated by shock waves traveling through the Corona and by magnetic energy released in Solar flares. The Solar Wind contains roughly equal numbers of electrons and protons along with heavier ions and blows continuously from t ...
X-ray astronomy detector
X-ray astronomy detectors are instruments that detect X-rays for use in the study of X-ray astronomy.X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray emission from celestial 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 part of space science.X-ray astronomy detectors have been designed and configured primarily for energy and occasionally for wavelength detection using a variety of techniques usually limited to the technology of the time.