The X-ray Astronomy Imaging Chain
... • X-Ray photons at “normal” or “nearnormal” incidence (photon path perpendicular to mirror, as already shown) would be transmitted (or possibly absorbed) rather than reflected. • At near-parallel incidence, X Rays “skip” off mirror surface (like stones skipping across water surface) ...
... • X-Ray photons at “normal” or “nearnormal” incidence (photon path perpendicular to mirror, as already shown) would be transmitted (or possibly absorbed) rather than reflected. • At near-parallel incidence, X Rays “skip” off mirror surface (like stones skipping across water surface) ...
Auger Effect in Biomedicine
... • It is usually initiated by X-ray photoionization of K-shell or Lshell electrons. • In heavy high-Z atoms up to 20 Auger electrons may be ejected (see Table 5.3 of Atomic Astrophysics and Spectroscopy (AAS) Pradhan and Nahar, Cambridge University Press, 2011) ...
... • It is usually initiated by X-ray photoionization of K-shell or Lshell electrons. • In heavy high-Z atoms up to 20 Auger electrons may be ejected (see Table 5.3 of Atomic Astrophysics and Spectroscopy (AAS) Pradhan and Nahar, Cambridge University Press, 2011) ...
Chandra - Cosmos
... solar panels) both key for this research. • Large fraction of Galactic LMXBs that exhibit bright (>1037 erg/s) transient outbursts have been shown to contain black holes (McClintock & Remillard 2004). • There are only ~20 such objects in the Galaxy, and each is vital for studies of accretion physics ...
... solar panels) both key for this research. • Large fraction of Galactic LMXBs that exhibit bright (>1037 erg/s) transient outbursts have been shown to contain black holes (McClintock & Remillard 2004). • There are only ~20 such objects in the Galaxy, and each is vital for studies of accretion physics ...
Magnetic Fields in Supernova Remnants and Pulsar
... • Pulsar-Wind Nebulae(PWNe): A type nebula is formed by Pulsar-Wind. It often finds in SNR shell. Sometimes also find near old Pulsar star. But it’s SNR has been vanished. • Property: 1. The distance is closer the PWNe center, The brightness is higher. These is not general structure of SNR. 2. The r ...
... • Pulsar-Wind Nebulae(PWNe): A type nebula is formed by Pulsar-Wind. It often finds in SNR shell. Sometimes also find near old Pulsar star. But it’s SNR has been vanished. • Property: 1. The distance is closer the PWNe center, The brightness is higher. These is not general structure of SNR. 2. The r ...
The X-ray Astronomy Imaging Chain
... • X-Ray photons at “normal” or “nearnormal” incidence (photon path perpendicular to mirror, as already shown) would be transmitted (or possibly absorbed) rather than reflected. • At near-parallel incidence, X Rays “skip” off mirror surface (like stones skipping across water surface) ...
... • X-Ray photons at “normal” or “nearnormal” incidence (photon path perpendicular to mirror, as already shown) would be transmitted (or possibly absorbed) rather than reflected. • At near-parallel incidence, X Rays “skip” off mirror surface (like stones skipping across water surface) ...
PPT
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
X-Ray Astronomy and Accretion Phenomena
... • X-ray detectors should be placed above the atmosphere • Chandra, XMM-Newton, Rosat, Uhuru, Integral etc are some X-ray astronomy missions. ...
... • X-ray detectors should be placed above the atmosphere • Chandra, XMM-Newton, Rosat, Uhuru, Integral etc are some X-ray astronomy missions. ...
Broggini
... 2.5 1017 atoms/cm2 L = 10 cm 13C-enriched solid target (drawbacks: degradation and possible carbon deposition) density 2·1017-1018 at/cm2 (electron gun evaporation, implantation on Au/ Ta, synthetic diamonds……) beam induced background (α,n) reactions on target impurities or along the beam line ( 10B ...
... 2.5 1017 atoms/cm2 L = 10 cm 13C-enriched solid target (drawbacks: degradation and possible carbon deposition) density 2·1017-1018 at/cm2 (electron gun evaporation, implantation on Au/ Ta, synthetic diamonds……) beam induced background (α,n) reactions on target impurities or along the beam line ( 10B ...
Puzzling X-rays from the new colliding wind binary Wolf–Rayet 65
... to log LX /Lbol = −7.2, . . ., − 7.8. The flux of the soft spectral component, F X (0.6–2.0 keV) = 8.3 × 10−15 erg s−1 cm−2 , corresponds to LX (0.6 − 2.0 keV) = 1.0 × 1031 erg s−1 which is similar to the X-ray luminosity of a single O dwarf (Oskinova 2005). Spectra observed at other epochs were als ...
... to log LX /Lbol = −7.2, . . ., − 7.8. The flux of the soft spectral component, F X (0.6–2.0 keV) = 8.3 × 10−15 erg s−1 cm−2 , corresponds to LX (0.6 − 2.0 keV) = 1.0 × 1031 erg s−1 which is similar to the X-ray luminosity of a single O dwarf (Oskinova 2005). Spectra observed at other epochs were als ...
Altair - the hottest `cool` star in X-rays
... Variability of Altair’s X-ray brightness is seen (Figure 1) at a level of roughly 30 % on timescales of a few hours and over the total observation time. This variability could in principle be due to rotational modulation or intrinsic variability of the X-ray emitting features, e.g. microflaring or c ...
... Variability of Altair’s X-ray brightness is seen (Figure 1) at a level of roughly 30 % on timescales of a few hours and over the total observation time. This variability could in principle be due to rotational modulation or intrinsic variability of the X-ray emitting features, e.g. microflaring or c ...
Chapters 5,12
... Advantages of reflecting telescopes include the fact that the light does not have to pass through any glass, there is no chromatic abberation, they can be made larger, and their weight is easier to support. ...
... Advantages of reflecting telescopes include the fact that the light does not have to pass through any glass, there is no chromatic abberation, they can be made larger, and their weight is easier to support. ...
The Sun: Our Star (Chapter 14) The source of the Sun`s energy has
... is kept constant by a “thermostat” that increases the rate if it decreases too much and decreases the rate if it increases too much. Energy generated by nuclear fusion keeps the pressure within the Sun high. This supports the weight of the Sun. It takes 100,000 years for energy to move out through t ...
... is kept constant by a “thermostat” that increases the rate if it decreases too much and decreases the rate if it increases too much. Energy generated by nuclear fusion keeps the pressure within the Sun high. This supports the weight of the Sun. It takes 100,000 years for energy to move out through t ...
The Super-slow Pulsation X-ray Pulsars in High Mass X
... Some arguments for magnetar assumption • Hard X-ray spectrum for superslow X-ray pulsars : power-law with cutoff , Γ~1.8 -2.5 magnetars above 20 keV: very hard, single power-law, Γ~1.0 -1.5 • Typical X-ray luminosity of magnetars : 1035 -1036 erg/s , 4U 2206+54/2S 0114+65: in the range of 1034 -103 ...
... Some arguments for magnetar assumption • Hard X-ray spectrum for superslow X-ray pulsars : power-law with cutoff , Γ~1.8 -2.5 magnetars above 20 keV: very hard, single power-law, Γ~1.0 -1.5 • Typical X-ray luminosity of magnetars : 1035 -1036 erg/s , 4U 2206+54/2S 0114+65: in the range of 1034 -103 ...
The new X-ray universe
... regions in AGN. Extended emission from the Seyfert 1.5 galaxy NGC 4151 shows evidence for both photoionized and collisionally ionized material in a multicomponent narrow line region. The emission line spectrum of the Seyfert 2 galaxy NGC 1068 looks remarkably similar to that of NGC 4151, but with a ...
... regions in AGN. Extended emission from the Seyfert 1.5 galaxy NGC 4151 shows evidence for both photoionized and collisionally ionized material in a multicomponent narrow line region. The emission line spectrum of the Seyfert 2 galaxy NGC 1068 looks remarkably similar to that of NGC 4151, but with a ...
MODERN PHYSICS
... 4. The Sun gets its energy from a sequence of nuclear reactions called the proton-proton cycle. These reactions take place near the Sun’s center and have the net effect 4p → He + 2e+ + 2ν + 5γ. The particles involved being (in order) are protons, helium nuclei, positrons, neutrinos, and high-energy ...
... 4. The Sun gets its energy from a sequence of nuclear reactions called the proton-proton cycle. These reactions take place near the Sun’s center and have the net effect 4p → He + 2e+ + 2ν + 5γ. The particles involved being (in order) are protons, helium nuclei, positrons, neutrinos, and high-energy ...
X-Ray Astronomy and Accretion Phenomena
... • X-ray detectors should be placed above the atmosphere • Chandra, XMM-Newton, Rosat, Uhuru, Integral etc are some X-ray astronomy missions. ...
... • X-ray detectors should be placed above the atmosphere • Chandra, XMM-Newton, Rosat, Uhuru, Integral etc are some X-ray astronomy missions. ...
Slide 1
... • Most SNR detected by Fermi have steep spectra (some exceptions, such as RXJ1713) • The predicted spectra would naively require steep diffusion D(E)~E0.7 in conflict with anisotropy measurements ...
... • Most SNR detected by Fermi have steep spectra (some exceptions, such as RXJ1713) • The predicted spectra would naively require steep diffusion D(E)~E0.7 in conflict with anisotropy measurements ...
DS11 Cosmology Homework 3 Q1. Visible light is part of a family of
... Q1. Visible light is part of a family of waves known as the electromagnetic spectrum. What is the speed of waves in the electromagnetic spectrum? ...
... Q1. Visible light is part of a family of waves known as the electromagnetic spectrum. What is the speed of waves in the electromagnetic spectrum? ...
Do flares in Saggitarius A* reflect the last stage of tidal capture
... 1. The rise and switch off rates of all flares are very similar 2. The rise-switch-off time scale is about 900 3. The light curve is similar in all wavebands ...
... 1. The rise and switch off rates of all flares are very similar 2. The rise-switch-off time scale is about 900 3. The light curve is similar in all wavebands ...
X-ray Optics How do we form an X
... curved toward the mirror, and because optical imperfections in mirror figure and mechanical tolerances in aligning the pieces of glass prevent perfect imaging on axis, it is generally advantageous to position a flat imaging detector slightly forward of the ideal on-axis focus. ...
... curved toward the mirror, and because optical imperfections in mirror figure and mechanical tolerances in aligning the pieces of glass prevent perfect imaging on axis, it is generally advantageous to position a flat imaging detector slightly forward of the ideal on-axis focus. ...
PowerPoint - Chandra X
... ESO 137-001: X-ray Tails from Galaxy Plunging into the Core of the Galaxy Cluster A3627 ...
... ESO 137-001: X-ray Tails from Galaxy Plunging into the Core of the Galaxy Cluster A3627 ...
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.