E/DE
... Hot stars are thought not to have outer convection zones, magnetic fields, or the associated magnetic dynamo and corona that our sun has. Thus their discovery 20 years ago as relatively strong soft X-ray sources was a surprise. Hot stars do have strong radiation-driven winds. These winds are subject ...
... Hot stars are thought not to have outer convection zones, magnetic fields, or the associated magnetic dynamo and corona that our sun has. Thus their discovery 20 years ago as relatively strong soft X-ray sources was a surprise. Hot stars do have strong radiation-driven winds. These winds are subject ...
This presentation - Fermi Gamma
... • SAS-2 – discovered 2 pulsars (1972) • COS-B – about 25 sources (1975-82) • Most unidentified, but 1 quasar • Diffuse extra-galactic background • Compton GRO – four instruments • Opened up the gamma-ray Universe ...
... • SAS-2 – discovered 2 pulsars (1972) • COS-B – about 25 sources (1975-82) • Most unidentified, but 1 quasar • Diffuse extra-galactic background • Compton GRO – four instruments • Opened up the gamma-ray Universe ...
Hard X-ray Sky - High Energy Astrophysics
... pixels (<16”, 90% conf. radii positions), 5 – 600 keV •SXI: 0.6m Wolter-I X-ray mirrors, CCD 0.3 – 10 keV •IRT: 1.1m optical/IR telescope & obj. prism: 0.3-2.5μm spectra & z’s ...
... pixels (<16”, 90% conf. radii positions), 5 – 600 keV •SXI: 0.6m Wolter-I X-ray mirrors, CCD 0.3 – 10 keV •IRT: 1.1m optical/IR telescope & obj. prism: 0.3-2.5μm spectra & z’s ...
Father of the X-Ray
... the same thing: electromagnetic radiation. The only differences between them all are the frequency and wavelengths of the different types of waves. X-Rays are mostly blocked out of the atmosphere because of the frequency of the waves. Because of this, X-Ray observatories, like the Chandra, have to b ...
... the same thing: electromagnetic radiation. The only differences between them all are the frequency and wavelengths of the different types of waves. X-Rays are mostly blocked out of the atmosphere because of the frequency of the waves. Because of this, X-Ray observatories, like the Chandra, have to b ...
The JANUS X-Ray Flash Monitor
... normally in survey mode. X-ray events are collected from 40 detectors, graded to eliminate cosmic rays, and placed into a ring buffer (sized to store ~2000 seconds of data) by the FPGAs on the FPB. Next, the science software searches the buffered data using the same sophisticated triggering algorith ...
... normally in survey mode. X-ray events are collected from 40 detectors, graded to eliminate cosmic rays, and placed into a ring buffer (sized to store ~2000 seconds of data) by the FPGAs on the FPB. Next, the science software searches the buffered data using the same sophisticated triggering algorith ...
Paul Green - Chandra X-Ray Observatory (CXC)
... Professor Philip Morrison of Cornell thinks the X rays may be generated when starlight picks up energy from high-speed electrons far out in space. Professor Minoru Oda of M.I.T. figures that the X rays come from a magnetic field surrounding the edges of the galactic nucleus. British Cosmologist Fred ...
... Professor Philip Morrison of Cornell thinks the X rays may be generated when starlight picks up energy from high-speed electrons far out in space. Professor Minoru Oda of M.I.T. figures that the X rays come from a magnetic field surrounding the edges of the galactic nucleus. British Cosmologist Fred ...
What is X-ray Astronomy? - Extreme Universe Laboratory
... X-rays don’t reflect off a normal mirror – they get absorbed. Only by striking a mirror at a glancing angle, about 1o, do X-rays reflect. Then they act like visible light and can be focused ...
... X-rays don’t reflect off a normal mirror – they get absorbed. Only by striking a mirror at a glancing angle, about 1o, do X-rays reflect. Then they act like visible light and can be focused ...
PowerPoint - Chandra X
... The image shows X-ray data from Chandra (purple) from the star CoRot-2A, along with optical infrared data from the Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT) and the Two Micron All Sky Survey (2MASS). ...
... The image shows X-ray data from Chandra (purple) from the star CoRot-2A, along with optical infrared data from the Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT) and the Two Micron All Sky Survey (2MASS). ...
X-ray astronomy - University of Warwick
... • Assuming optically-thin thermal plasma emission with kT=6 keV and interstellar absorption of NH=1020cm-2, estimate the 2-10 keV energy flux of SU UMa • Further calculate the XMM-Newton RGS count rate, and determine how long an observation is required to accumulate ...
... • Assuming optically-thin thermal plasma emission with kT=6 keV and interstellar absorption of NH=1020cm-2, estimate the 2-10 keV energy flux of SU UMa • Further calculate the XMM-Newton RGS count rate, and determine how long an observation is required to accumulate ...
Astronomers Learn to Work in Space
... V-2 Rocket October 10, 1946 Ultraviolet spectrum of sun 340 nm – 240 nm Bead entrance UV film ...
... V-2 Rocket October 10, 1946 Ultraviolet spectrum of sun 340 nm – 240 nm Bead entrance UV film ...
Slide 1
... Where would the heavier elements be? Where would the light elements be? Explain your reasoning. You may wish to read more first. ...
... Where would the heavier elements be? Where would the light elements be? Explain your reasoning. You may wish to read more first. ...
Pounds K. - X-ray Astronomy and Cosmology group group
... Ariel 5 Scout B-1 launch 15 October 1974 500 km circular, equatorial orbit 129 kg S/C into equatorial LEO 10 rpm spin with axis control by gas jets, later by magnetorquer operated for 5.5 years to re-entry in ...
... Ariel 5 Scout B-1 launch 15 October 1974 500 km circular, equatorial orbit 129 kg S/C into equatorial LEO 10 rpm spin with axis control by gas jets, later by magnetorquer operated for 5.5 years to re-entry in ...
Solar Flares
... Solar flares are sudden localised brightening in the solar atmosphere, seen in all bands of the solar EM emission, from radio to 100 MeV. The amount of the released energy reaches 1027 J. ...
... Solar flares are sudden localised brightening in the solar atmosphere, seen in all bands of the solar EM emission, from radio to 100 MeV. The amount of the released energy reaches 1027 J. ...
pptx - Particle Physics and Particle Astrophysics
... X-rays: detection and sources • Modern X-ray telescopes use focusing optics • however, X-rays do not reflect at normal incidence • hence use grazing incidence optics • any part of a parabola focuses light to a point • use the high part of the curve instead of the bowl at the bottom ...
... X-rays: detection and sources • Modern X-ray telescopes use focusing optics • however, X-rays do not reflect at normal incidence • hence use grazing incidence optics • any part of a parabola focuses light to a point • use the high part of the curve instead of the bowl at the bottom ...
Many-body Physics in Neutrino Detection and Dark Matter Searches
... Many-body physics is essential for sub-keV detectors of neutrinos and dark matter. ...
... Many-body physics is essential for sub-keV detectors of neutrinos and dark matter. ...
X-ray Observations of Cosmic Accelerators Greg Madejski SLAC/KIPAC
... -> Flares come from dissipation of gravitational energy What is the origin of the hot plasma? Observed X-ray spectra (up to at least 100 keV) indicate that accretion disks must be sites of vigorous particle acceleration - Most likely associated with “plasma viscosity” provided by the magneto-rotatio ...
... -> Flares come from dissipation of gravitational energy What is the origin of the hot plasma? Observed X-ray spectra (up to at least 100 keV) indicate that accretion disks must be sites of vigorous particle acceleration - Most likely associated with “plasma viscosity” provided by the magneto-rotatio ...
Discovery of 7-13 HZ quasi-periodic oscillations in the new X
... (see the power density spectrum) in the recently discovered X-ray transient XTE J1806-246 (IAUC 6891 ) in data obtained on May 3 1998 21:03-22:31 UT with the proportional counter array (PCA) onboard the Rossi X-ray Timing Explorer. The total PCA count rate varied between approximately 7000 and 8000 ...
... (see the power density spectrum) in the recently discovered X-ray transient XTE J1806-246 (IAUC 6891 ) in data obtained on May 3 1998 21:03-22:31 UT with the proportional counter array (PCA) onboard the Rossi X-ray Timing Explorer. The total PCA count rate varied between approximately 7000 and 8000 ...
Astro2006_0526
... supercritical accretion disk and jets. Basing on observational data of SS433 and published 2D-simulations of supercritical accretion disks we estimate parameters of the funnel in the disk/wind of SS433 and discuss formation of the jets. We argue that the UV radiation of the SS433 disk (~50000 K, ~10 ...
... supercritical accretion disk and jets. Basing on observational data of SS433 and published 2D-simulations of supercritical accretion disks we estimate parameters of the funnel in the disk/wind of SS433 and discuss formation of the jets. We argue that the UV radiation of the SS433 disk (~50000 K, ~10 ...
rastieee
... intense X-ray emitters. The high energy emission from such exotic objects are often transient that may last from a few seconds to months depending on the nature of the object. Since the atmosphere absorbs X-rays, observations of these interesting objects must be made in space. There are various larg ...
... intense X-ray emitters. The high energy emission from such exotic objects are often transient that may last from a few seconds to months depending on the nature of the object. Since the atmosphere absorbs X-rays, observations of these interesting objects must be made in space. There are various larg ...
Feigelson, E. (PSU)
... z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-15 keV) X-rays should penetrate 1-100 g/cm2. Igea & Glassgold 1997 & 1999; Fromang et al. 2002; Matsumura & Pudritz 2003 & 2006; Alexander et al. 2004; Salmeron & Wardle 2005; I ...
... z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-15 keV) X-rays should penetrate 1-100 g/cm2. Igea & Glassgold 1997 & 1999; Fromang et al. 2002; Matsumura & Pudritz 2003 & 2006; Alexander et al. 2004; Salmeron & Wardle 2005; I ...
Electromagnetic spectrum - Purdue Physics
... Cones are highly concentrated in a region near the center of the retina called the fovea. The maximum concentration of cones is roughly 180,000 per mm2 there and the density decreases rapidly outside of the fovea to less than 5,000 per mm2. Note the blind spot caused by the optic nerve, which is voi ...
... Cones are highly concentrated in a region near the center of the retina called the fovea. The maximum concentration of cones is roughly 180,000 per mm2 there and the density decreases rapidly outside of the fovea to less than 5,000 per mm2. Note the blind spot caused by the optic nerve, which is voi ...
! • Supermassive Black Holes (SMBH) at Work: Effects of
... in NGC4342 and NGC4291, respectively. Thus, the ob- an extreme outlier (5.1σ outlier) served values are factors of ≈60 and ≈13 times larger •NGC4342 than the predicted ones. From the intrinsic scatter of is less (3.4σ outlier) •NGC4291 the relation (0.30 dex) extreme and the uncertainty of the black ...
... in NGC4342 and NGC4291, respectively. Thus, the ob- an extreme outlier (5.1σ outlier) served values are factors of ≈60 and ≈13 times larger •NGC4342 than the predicted ones. From the intrinsic scatter of is less (3.4σ outlier) •NGC4291 the relation (0.30 dex) extreme and the uncertainty of the black ...
hotstar_xrays
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=cDl/lov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=cDl/lov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
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.