Astrophysical S-factor of P PНеP PС radiative capture at low energies
... The sum of all three E2 transitions, which describes the experimental behavior of the astrophysical Sfactor at energies from 0.9 to 4.0 MeV is shown by the solid line in figure 7. Our calculated S-factor at the energy 300 keV caused by the E2 process with the transition from the D wave to the GS of ...
... The sum of all three E2 transitions, which describes the experimental behavior of the astrophysical Sfactor at energies from 0.9 to 4.0 MeV is shown by the solid line in figure 7. Our calculated S-factor at the energy 300 keV caused by the E2 process with the transition from the D wave to the GS of ...
Document
... 2. Absolute measurements of the La radiation flux. The absolute measurements of the La radiation intensity by means of a vacuum monochromator would have required preliminary calibration of the whole recording apparatus, i.e., the determination of the admittance coefficient of the vacuum monochromato ...
... 2. Absolute measurements of the La radiation flux. The absolute measurements of the La radiation intensity by means of a vacuum monochromator would have required preliminary calibration of the whole recording apparatus, i.e., the determination of the admittance coefficient of the vacuum monochromato ...
(1) and
... Steady nuclear fusion in laboratory is very difficult, almost impossible to keep hot plasma for long time is difficult. Laboratory plasma is always transient in a short time scale. Space plasma is also transient, but the time scale is extremely long quasi-stable Space is better than laboratory ...
... Steady nuclear fusion in laboratory is very difficult, almost impossible to keep hot plasma for long time is difficult. Laboratory plasma is always transient in a short time scale. Space plasma is also transient, but the time scale is extremely long quasi-stable Space is better than laboratory ...
X-ray emission from young pulsar, PWN and SNRs
... • The fact that most of the X-ray filament tails point away from Sgr A* suggests that there exists a radial flow from GC. This flow (Galactic wind) blows the pulsar wind particles to the anti-GC direction and shapes the cometary morphology. These filaments thus represent PWNe in strong windy ...
... • The fact that most of the X-ray filament tails point away from Sgr A* suggests that there exists a radial flow from GC. This flow (Galactic wind) blows the pulsar wind particles to the anti-GC direction and shapes the cometary morphology. These filaments thus represent PWNe in strong windy ...
The Radio and X-ray Jet
... In the radio it looks quite different, as can be seen in these three images, taken at different resolutions. It seems to have a jet of relativistic particles squirting out in both directions. ...
... In the radio it looks quite different, as can be seen in these three images, taken at different resolutions. It seems to have a jet of relativistic particles squirting out in both directions. ...
ULXs: General Properties and Variability - X
... 1 inside X-ray ionized nebula – strong HeII 4686 and [OI] 6300 – requires 3-13x1039 ergs/sec to produce observed optical emission lines 4+ in bubble-like nebulae, 200-400 pc – 2+ with probable O-star counterpart 4+ in other nebulae ...
... 1 inside X-ray ionized nebula – strong HeII 4686 and [OI] 6300 – requires 3-13x1039 ergs/sec to produce observed optical emission lines 4+ in bubble-like nebulae, 200-400 pc – 2+ with probable O-star counterpart 4+ in other nebulae ...
A diffusive description of the focused transport of solar energetic
... scale that characterizes the change in B0 is large compared to the spatial dimension of the particles’ gyration motion. In this case it can be assumed that B0 is constant for a single gyration, and the first adiabatic invariant is conserved. For a particle moving in a diverging magnetic field, this ...
... scale that characterizes the change in B0 is large compared to the spatial dimension of the particles’ gyration motion. In this case it can be assumed that B0 is constant for a single gyration, and the first adiabatic invariant is conserved. For a particle moving in a diverging magnetic field, this ...
The Case for a Kilometer-Scale High Energy Neutrino Detector
... are underway to develop instruments that may push astronomy to wavelengths smaller than 10−14 cm by mapping the sky in high energy neutrinos instead. Neutrino astronomy, born with the identification of thermonuclear fusion in the sun and the particle processes controlling the fate of a nearby supern ...
... are underway to develop instruments that may push astronomy to wavelengths smaller than 10−14 cm by mapping the sky in high energy neutrinos instead. Neutrino astronomy, born with the identification of thermonuclear fusion in the sun and the particle processes controlling the fate of a nearby supern ...
Signatures of the first stars in the 21cm Emission and Absorption
... temperatures out to a radius much larger than the HII region. • X-rays from the stellar photosphere heat the medium. • X-ray ionizations also produce injected Lyα photons, which turn out to dominate for the surface temperatures of metal-free stars. These yields a dominant absorption signal from a `` ...
... temperatures out to a radius much larger than the HII region. • X-rays from the stellar photosphere heat the medium. • X-ray ionizations also produce injected Lyα photons, which turn out to dominate for the surface temperatures of metal-free stars. These yields a dominant absorption signal from a `` ...
Two-Dimensional Integrated Circuits for Hybrid
... voltages in steps of 10 to 20 mV (depending on the amplitude) and counted for 5 ms at each step. From these data we determined, for each cell, the threshold at which the number of counts had fallen to half the value expected from the pulse frequency, using linear interpolation between the nearest st ...
... voltages in steps of 10 to 20 mV (depending on the amplitude) and counted for 5 ms at each step. From these data we determined, for each cell, the threshold at which the number of counts had fallen to half the value expected from the pulse frequency, using linear interpolation between the nearest st ...
Einestein`s photoelectric equation does not establish photons as
... attention of the readers to a publication by Panarella [5]. He carried out the measurements of the diffraction patterns due to a pin hole illuminated by a CW He-Ne laser beam whose intensity was systematically reduced by carefully calibrated steps. He found out that when the beam power drops below f ...
... attention of the readers to a publication by Panarella [5]. He carried out the measurements of the diffraction patterns due to a pin hole illuminated by a CW He-Ne laser beam whose intensity was systematically reduced by carefully calibrated steps. He found out that when the beam power drops below f ...
Document
... correct for image degrading sources from inside and outside the spacecraft. This includes correction systems for large aperture space telescopes that require control across the entire wavefront, typically at low temporal bandwidth. The following technologies are sought: ...
... correct for image degrading sources from inside and outside the spacecraft. This includes correction systems for large aperture space telescopes that require control across the entire wavefront, typically at low temporal bandwidth. The following technologies are sought: ...
Educator`s Guide - Ott Planetarium
... Spectroscopy is the study of how electromagnetic radiation, which we’ve just introduced, interacts with atoms. Atoms absorb and emit radiation across the entire spectrum; with each atom having a unique pattern. By analyzing the data that is collected by the the space telescopes, scientist use these ...
... Spectroscopy is the study of how electromagnetic radiation, which we’ve just introduced, interacts with atoms. Atoms absorb and emit radiation across the entire spectrum; with each atom having a unique pattern. By analyzing the data that is collected by the the space telescopes, scientist use these ...
Sensitivity of SK to Reactor Neutrinos
... A “micro-SuperK” is also being built to test anti-corrosion ...
... A “micro-SuperK” is also being built to test anti-corrosion ...
NGC 6231: a young open cluster under X-rays
... • The canonical relation is tightly constrained V but still not understood on firm theoretical ground ! • Our sample is inhomogeneous in terms of spectral sub-type and luminosity class same mechanism for all • Confirmed by a recent study by Anthokin et al. on Cyg OB2 • Very limited room for the B ...
... • The canonical relation is tightly constrained V but still not understood on firm theoretical ground ! • Our sample is inhomogeneous in terms of spectral sub-type and luminosity class same mechanism for all • Confirmed by a recent study by Anthokin et al. on Cyg OB2 • Very limited room for the B ...
Additive manufacturing and high resolution X-ray optics
... Aluminium rms roughness = 22nm Titanium = optical surface not achieved ...
... Aluminium rms roughness = 22nm Titanium = optical surface not achieved ...
erice_091014 - Astronomy & Astrophysics Group
... BUT Still strong case for a wide-spectrum high-energy monitoring satellite. e.g. 5 of the 9 SGBs in Berger et al (2007) had only X-ray positions, but these were measured to ~6 arcseconds. GW triggers from ET network would locate source to ~10 sq. deg. With only optical afterglows, that leaves ~107 g ...
... BUT Still strong case for a wide-spectrum high-energy monitoring satellite. e.g. 5 of the 9 SGBs in Berger et al (2007) had only X-ray positions, but these were measured to ~6 arcseconds. GW triggers from ET network would locate source to ~10 sq. deg. With only optical afterglows, that leaves ~107 g ...
red shift - Scoilnet
... moves towards us, and decrease in pitch when it moves away. This is called the Doppler Effect. This is what makes an ambulance sound suddenly lower when it goes past us. Light is another type of wave, so the Doppler Effect applies to light as well. When a star’s light is red shifted, the star must b ...
... moves towards us, and decrease in pitch when it moves away. This is called the Doppler Effect. This is what makes an ambulance sound suddenly lower when it goes past us. Light is another type of wave, so the Doppler Effect applies to light as well. When a star’s light is red shifted, the star must b ...
The spin and orbit of the newly discovered pulsar IGR J17480-2446
... data segments (for a total of 127) around the periodicity indicated by the power spectrum. The resulting variance profiles are fitted following Leahy (1987) and the uncertainties affecting the period estimates are evaluated accordingly. The best-fitting orbital solution we obtain with this technique ...
... data segments (for a total of 127) around the periodicity indicated by the power spectrum. The resulting variance profiles are fitted following Leahy (1987) and the uncertainties affecting the period estimates are evaluated accordingly. The best-fitting orbital solution we obtain with this technique ...
High Energy Phenomena in Supergiant X-ray Binaries - HAL-Insu
... rapid outbursts lasting only for hours, faint quiescent emission, and high energy spectra requiring a BH or NS accretor. The flares rise in tens of minutes, last for ∼ 1 hour, their frequency is ∼ 7 days, and their luminosity L x ∼ 1036 erg s−1 at the outburst peak. IGR J17544-2619, archetype of SFX ...
... rapid outbursts lasting only for hours, faint quiescent emission, and high energy spectra requiring a BH or NS accretor. The flares rise in tens of minutes, last for ∼ 1 hour, their frequency is ∼ 7 days, and their luminosity L x ∼ 1036 erg s−1 at the outburst peak. IGR J17544-2619, archetype of SFX ...
Accelerator Experiments and Theoretical Models for the Electron Screening Effect in
... to prevent a congestion of them and the data acquisition system. Therefore grounded Al-foils of thicknesses from 120 150 g cm2 were placed in front of the detectors. The thickness is sufficient in order to block deuterons up to 60 keV and let pass all other ejectiles. The detector voltage puls ...
... to prevent a congestion of them and the data acquisition system. Therefore grounded Al-foils of thicknesses from 120 150 g cm2 were placed in front of the detectors. The thickness is sufficient in order to block deuterons up to 60 keV and let pass all other ejectiles. The detector voltage puls ...
ppt - ciera
... Chandra and XMM fields reveals no new 530 s pulsars, so there is a <0.5% chance of finding a magnetar in any field (Nechita, Gaensler, Muno, et al. in prep). • The pulsar is well within the cluster, with a <10% chance of being an unrelated X-ray source. ...
... Chandra and XMM fields reveals no new 530 s pulsars, so there is a <0.5% chance of finding a magnetar in any field (Nechita, Gaensler, Muno, et al. in prep). • The pulsar is well within the cluster, with a <10% chance of being an unrelated X-ray source. ...
Astronomical spectroscopy
... The objective translates angles into positions on the detector. Each position (pixel) of the detector ‘sees’ a given angle of the parallel (collimated) beam The collimated beam is never perfectly parallel, because either of the limited diameter of the beam, which produces diffraction = 1.22 /D1, ...
... The objective translates angles into positions on the detector. Each position (pixel) of the detector ‘sees’ a given angle of the parallel (collimated) beam The collimated beam is never perfectly parallel, because either of the limited diameter of the beam, which produces diffraction = 1.22 /D1, ...
ASPERA-3: Analyser of Space Plasmas and
... empirical model of the solar wind plasma flow near Mars developed by Kallio & Koskinen (1999), Barabash et al. (2002) numerically solved the kinetic equation and obtained the global distribution of oxygen ions. This distribution was then converted to the corresponding ENA flux. It was found that the ...
... empirical model of the solar wind plasma flow near Mars developed by Kallio & Koskinen (1999), Barabash et al. (2002) numerically solved the kinetic equation and obtained the global distribution of oxygen ions. This distribution was then converted to the corresponding ENA flux. It was found that the ...
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.