Measurement of the 52Fe mass via the precise proton
... proton decay, since the ion is stopped in the detector, the energy loss of β particle as well as proton is summed up. However, due to the small rate of energy loss, β particle escapes from the detector and leaves an energy of tens to hundreds keV in the detector depending on the implanted depth and ...
... proton decay, since the ion is stopped in the detector, the energy loss of β particle as well as proton is summed up. However, due to the small rate of energy loss, β particle escapes from the detector and leaves an energy of tens to hundreds keV in the detector depending on the implanted depth and ...
Article PDF - IOPscience
... the effects on the average rate of variations in the effective detection efficiency for a point source as its image passes over the grid structure of the PSPC window. The count rate varies about the overall average of 3.79 counts s21 on timescales from several minutes to hours. (For comparison, we c ...
... the effects on the average rate of variations in the effective detection efficiency for a point source as its image passes over the grid structure of the PSPC window. The count rate varies about the overall average of 3.79 counts s21 on timescales from several minutes to hours. (For comparison, we c ...
X-ray Astronomy and the search for Black Holes
... • The hard X-rays are optical thin, thermal emission from the accreting plasma, as also seen in magnetic and non-magnetic CVs • These symbiotic stars have harder spectra than non-magnetic CVs • Yet they are unlikely to have a magnetic white dwarf • Non-magnetic CVs can have high temperatures if the ...
... • The hard X-rays are optical thin, thermal emission from the accreting plasma, as also seen in magnetic and non-magnetic CVs • These symbiotic stars have harder spectra than non-magnetic CVs • Yet they are unlikely to have a magnetic white dwarf • Non-magnetic CVs can have high temperatures if the ...
A Legacy Study of Stellar Life Cycles in the Galactic Center
... • Unusual for an XRB to be in outburst for so long (Chen et al. 1997). • Microquasars and some pulsars might have required luminosity and hard spectrum in high state • Fluorescent line seen in Sgr B2, Sgr C, and central parsecs of Galaxy, so would need multiple microquasars, such as GRS 1915+10, but ...
... • Unusual for an XRB to be in outburst for so long (Chen et al. 1997). • Microquasars and some pulsars might have required luminosity and hard spectrum in high state • Fluorescent line seen in Sgr B2, Sgr C, and central parsecs of Galaxy, so would need multiple microquasars, such as GRS 1915+10, but ...
Draft A101 Slide Set #1 - Astronomical Society of the Pacific
... X-rays into sharp images. It includes two focusing X-ray telescopes which capture images, and also measure the energy of each incoming X-ray. Essential to the NuSTAR design is a deployable mast which extended to 10 meters after launch. This mast separates the X-ray optics from the detectors, a neces ...
... X-rays into sharp images. It includes two focusing X-ray telescopes which capture images, and also measure the energy of each incoming X-ray. Essential to the NuSTAR design is a deployable mast which extended to 10 meters after launch. This mast separates the X-ray optics from the detectors, a neces ...
Source Variability - Center for Astrophysics and Space
... Wavefront Interference =s (where s is fringe spacing) ...
... Wavefront Interference =s (where s is fringe spacing) ...
What is X-ray Astronomy? - High Energy Astrophysics
... 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 ...
What Are the Faint X-ray Transients Near the Galactic Center?
... Another LMXB (0.1 pc from Sgr A*) with Periodic Eclipses ...
... Another LMXB (0.1 pc from Sgr A*) with Periodic Eclipses ...
X-RAY VISION
... medical x-rays penetrate skin to reveal bone, cosmic versions pierce clouds of gas and dust to reveal hidden objects in our galaxy and beyond. Until now, no NASA mission has been able to focus high-energy x-rays to make a clear, high-quality image. The Nuclear Spectroscopic Telescope Array (NuSTAR), ...
... medical x-rays penetrate skin to reveal bone, cosmic versions pierce clouds of gas and dust to reveal hidden objects in our galaxy and beyond. Until now, no NASA mission has been able to focus high-energy x-rays to make a clear, high-quality image. The Nuclear Spectroscopic Telescope Array (NuSTAR), ...
Status of the EXL calorimeter
... Gamma sum energy, m and individual energies 95% 4P coverage, e=80% for Eg= 2-4 MeV Stopping 300 MeV protons DE = 2-3% for gs and 1% for fast protons Bins in polar angle of 1o-4o for Doppler Correction Total of about 1500 crystals of 20 cm in length 2 Phases : 1.7 + 0.6 M€ if CsI ...
... Gamma sum energy, m and individual energies 95% 4P coverage, e=80% for Eg= 2-4 MeV Stopping 300 MeV protons DE = 2-3% for gs and 1% for fast protons Bins in polar angle of 1o-4o for Doppler Correction Total of about 1500 crystals of 20 cm in length 2 Phases : 1.7 + 0.6 M€ if CsI ...
Supporting material for Lecture 2
... object (or reflected light for non-luminous objects like asteroids); it is the object's apparent magnitude as seen from a certain location. For stars it is 10 parsecs (32.6 light years). ...
... object (or reflected light for non-luminous objects like asteroids); it is the object's apparent magnitude as seen from a certain location. For stars it is 10 parsecs (32.6 light years). ...
ppt - UCL
... High-resolution RGS spectra allowed us to determine the absorbing column density for the X-ray emitting region. From the depth of the O I absorption edge, we infer an intrinsic nH <~ 1020 cm-2 (figure above). This rules out wind accretion as the main mechanism of mass transfer, and suggests that acc ...
... High-resolution RGS spectra allowed us to determine the absorbing column density for the X-ray emitting region. From the depth of the O I absorption edge, we infer an intrinsic nH <~ 1020 cm-2 (figure above). This rules out wind accretion as the main mechanism of mass transfer, and suggests that acc ...
GROUP V: Summary talk
... the RHESSI data (close collaboration with all WGs) and other available sources of information on high energy particles 2. Discuss new theories on particle acceleration 3. Connecting theories on particle acceleration with the global magnetic topologies hosting flares and CMEs ...
... the RHESSI data (close collaboration with all WGs) and other available sources of information on high energy particles 2. Discuss new theories on particle acceleration 3. Connecting theories on particle acceleration with the global magnetic topologies hosting flares and CMEs ...
High energy universe – Satellite missions
... sensitivity of 5 10 6 photons/cm2/sec at 1 MeV. It is the first time that a space facility to observe a single source simultaneously in optical, x-ray and gamma rays has been built. It is expected to operate for 2–5 years. The GLAST is scheduled to be launched in 2005. The primary instrument onboa ...
... sensitivity of 5 10 6 photons/cm2/sec at 1 MeV. It is the first time that a space facility to observe a single source simultaneously in optical, x-ray and gamma rays has been built. It is expected to operate for 2–5 years. The GLAST is scheduled to be launched in 2005. The primary instrument onboa ...
The theme “Research of fundamental interactions in nucleus at low
... high purity Germanium cryogenic detectors with simultaneous measurement of phonon and ionization signals at a temperature about 20 mK. Recoiled nucleus produces less ionization in a crystal than an electron does, thus analysis of phonon/ionization ratio allowing an excellent event-by-event discrimin ...
... high purity Germanium cryogenic detectors with simultaneous measurement of phonon and ionization signals at a temperature about 20 mK. Recoiled nucleus produces less ionization in a crystal than an electron does, thus analysis of phonon/ionization ratio allowing an excellent event-by-event discrimin ...
Astroparticle physics 1. stellar astrophysics and solar neutrinos
... • Gravitational waves: not today... • Elementary particles: cosmic-rays. ...
... • Gravitational waves: not today... • Elementary particles: cosmic-rays. ...
Presentation 1: Spectroscopy
... A partial energy level diagram for helium-like ions, such as Si+12 (see the FIR panel inset on the Chandra spectrum figure). The resonance transition (R) is strongest, but the intercombination (I) and forbidden (F) lines can also be strong. Electrons in the longlived, or metastable, 3S state can be ...
... A partial energy level diagram for helium-like ions, such as Si+12 (see the FIR panel inset on the Chandra spectrum figure). The resonance transition (R) is strongest, but the intercombination (I) and forbidden (F) lines can also be strong. Electrons in the longlived, or metastable, 3S state can be ...
A Tale of Two (Solar) Telescopes: something old, something
... B, 2 MK, for broad 0.06-6 keV band. Now XMM has moved closer to Chandra, less challenging to our expectations for stellar cycles. In hindsight, extreme darkening of Alpha Cen seen by XMM in 0.2-2 keV band has precedence on Sun, but was not so obvious in stars during ROSAT era owing to poor energy di ...
... B, 2 MK, for broad 0.06-6 keV band. Now XMM has moved closer to Chandra, less challenging to our expectations for stellar cycles. In hindsight, extreme darkening of Alpha Cen seen by XMM in 0.2-2 keV band has precedence on Sun, but was not so obvious in stars during ROSAT era owing to poor energy di ...
X-Ray Telescope
... Suzaku: Jp-US X-ray satellite Successfully launched on 2005 July 10th. XIS (X-ray Imaging Spectrometer) Improved X-ray CCD with high efficiency and good energy response Low and stable background Energy band : 0.2-12keV XRT (X-Ray Telescope) Large effective area 410cm2 @1.5keV ...
... Suzaku: Jp-US X-ray satellite Successfully launched on 2005 July 10th. XIS (X-ray Imaging Spectrometer) Improved X-ray CCD with high efficiency and good energy response Low and stable background Energy band : 0.2-12keV XRT (X-Ray Telescope) Large effective area 410cm2 @1.5keV ...
Solution to Problem Set 1 1. The total number of nucleons in one
... The stellar masses are in the range of 0.1 − 100M [1 mark] At the lower limit, the gravity is balanced by the degenerate pressure of electrons, and the central temperature is too low to initiate the nuclear burning. [2 marks] Very massive stars are dominated by radiation pressure, such radiation do ...
... The stellar masses are in the range of 0.1 − 100M [1 mark] At the lower limit, the gravity is balanced by the degenerate pressure of electrons, and the central temperature is too low to initiate the nuclear burning. [2 marks] Very massive stars are dominated by radiation pressure, such radiation do ...
A Chandra Observation of the Massive Star-Forming
... 38 ksec Chandra/ACIS-I observation (FOV~17'X17'), centered on the O3 star Pismis 24-1 (N35). Blue circles show regions used for photon extraction. ...
... 38 ksec Chandra/ACIS-I observation (FOV~17'X17'), centered on the O3 star Pismis 24-1 (N35). Blue circles show regions used for photon extraction. ...
9. Fascinating observations. But how much is well understood?
... sources which undergo repeted bursting of subsecond duration. Sometimes they exhibit luminous superflares lasting some 100 seconds but their repetition has not yet been observed. The other class of high field objects are the Anomalous X-ray Pulsars (AXP).They were discovered as pulsating X-ray sourc ...
... sources which undergo repeted bursting of subsecond duration. Sometimes they exhibit luminous superflares lasting some 100 seconds but their repetition has not yet been observed. The other class of high field objects are the Anomalous X-ray Pulsars (AXP).They were discovered as pulsating X-ray sourc ...
Using Technology To See Beyond The Visible
... but has different wavelengths and frequencies from those of light. Wavelength is a measurement of the distance from one point on a wave (such as the crest) to the ...
... but has different wavelengths and frequencies from those of light. Wavelength is a measurement of the distance from one point on a wave (such as the crest) to the ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... sensitivity limit is LX ∼ 5 · 1028 erg s−1. By using COUP data as template, we estimate that we have completeness of WTTs sample above LX ∼ 1029.3 erg s−1 but that a fraction > 50% could be undetected below 1029.3 erg s−1, at masses ≤ 0.8 − 1M ⊙. We observe also that the fraction of X-rays detected ...
... sensitivity limit is LX ∼ 5 · 1028 erg s−1. By using COUP data as template, we estimate that we have completeness of WTTs sample above LX ∼ 1029.3 erg s−1 but that a fraction > 50% could be undetected below 1029.3 erg s−1, at masses ≤ 0.8 − 1M ⊙. We observe also that the fraction of X-rays detected ...
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.