Document
... In the figure the spectra of the source for three angles of observation is shown: 60 degrees (solid line), 82 degrees (dotted line) and 90 degrees (dash-dotted line). In the last case the contribution of both hemispheres was taken into account, in the first two cases it wasn’t necessary. ...
... In the figure the spectra of the source for three angles of observation is shown: 60 degrees (solid line), 82 degrees (dotted line) and 90 degrees (dash-dotted line). In the last case the contribution of both hemispheres was taken into account, in the first two cases it wasn’t necessary. ...
Measurement of very low (α,n) cross sections of astrophysical interest
... Experimentally the cross sections at the relevant energies (Gamow window) have not been measured and currently they are estimated from extrapolations. The limiting factor in the measurements has been the relatively high level of neutron background in comparison with the weak reaction rates expected ...
... Experimentally the cross sections at the relevant energies (Gamow window) have not been measured and currently they are estimated from extrapolations. The limiting factor in the measurements has been the relatively high level of neutron background in comparison with the weak reaction rates expected ...
intro - Big Bear Solar Observatory
... - are in agreement with the concept that a solar flare is the collective energy released by an avalanche of reconnection events at small-scale discontinuities of the magnetic field (the self-organized criticality concept ) (Parker 1987; Longcope and Noonan 2000 ; Charbonneau, McIntosh, Liu and Bogda ...
... - are in agreement with the concept that a solar flare is the collective energy released by an avalanche of reconnection events at small-scale discontinuities of the magnetic field (the self-organized criticality concept ) (Parker 1987; Longcope and Noonan 2000 ; Charbonneau, McIntosh, Liu and Bogda ...
Ten Years Of XMM-Newton: Scientific Achievements And Future Prospects Norbert Schartel
... Spacecraft status is very good ...
... Spacecraft status is very good ...
Investigation of substrates and mounting techniques for the High
... of flat panel displays are deposited. They must be extremely smooth on all length scales up to the size of the displays (~30cm), and must have good mechanical properties. We have studied a number of these glasses and selected two, Schott and Desag AF-45 and D-263 as potential candidates for forming ...
... of flat panel displays are deposited. They must be extremely smooth on all length scales up to the size of the displays (~30cm), and must have good mechanical properties. We have studied a number of these glasses and selected two, Schott and Desag AF-45 and D-263 as potential candidates for forming ...
The ultracompact nature of the black hole candidate X
... and background spectra using specextract. We chose an extraction radius of 1.800 for the source region. For lightcurve analysis, we barycentered the time stamps. 47 Tuc X9 is near the crowded center of the cluster. Thus, for extracting background spectra, we used an annulus with inner and outer radi ...
... and background spectra using specextract. We chose an extraction radius of 1.800 for the source region. For lightcurve analysis, we barycentered the time stamps. 47 Tuc X9 is near the crowded center of the cluster. Thus, for extracting background spectra, we used an annulus with inner and outer radi ...
M.Ishida_Future_HE_Mission2006 - X
... Accretion onto WD takes place through an optically thick Keplerian disc (T~105K). Hard X-rays are radiated from the Boundary Layer which is optically thin/geometrically thick with T~108K. The rotation speed of WD at its surface is usually much smaller than vK(R*) (~5000km/s). For settling do ...
... Accretion onto WD takes place through an optically thick Keplerian disc (T~105K). Hard X-rays are radiated from the Boundary Layer which is optically thin/geometrically thick with T~108K. The rotation speed of WD at its surface is usually much smaller than vK(R*) (~5000km/s). For settling do ...
Direct reactions - Michigan State University
... hitting the target for each energy bin) because that is what determines the event rate. This is the same situation in the center of a star. The number density of particles is M.B. distributed, but the number of particles passing through an area per second is E e - E / kT distributed, and so is the ...
... hitting the target for each energy bin) because that is what determines the event rate. This is the same situation in the center of a star. The number density of particles is M.B. distributed, but the number of particles passing through an area per second is E e - E / kT distributed, and so is the ...
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... the dire t supernova s enario an only work through a tuning of the birth ki k velo ity and dire tion of the neutron star (Kalogera 1998). This problem may be alleviated by invoking ommon envelope evolution to remove mu h of the mass of the supernova progenitor prior to the explosion (e.g. van den ...
... the dire t supernova s enario an only work through a tuning of the birth ki k velo ity and dire tion of the neutron star (Kalogera 1998). This problem may be alleviated by invoking ommon envelope evolution to remove mu h of the mass of the supernova progenitor prior to the explosion (e.g. van den ...
Word document
... 2) A double slit pattern is formed on a wall that is 2 m from the slits with 589-nm light. The tenth interference minimum appears 7.26 mm from the central maximum. Find the spacing of the slits. 3) Two parallel slits are separated by 0.25 mm and illuminated with green light at a wavelength of 546.1 ...
... 2) A double slit pattern is formed on a wall that is 2 m from the slits with 589-nm light. The tenth interference minimum appears 7.26 mm from the central maximum. Find the spacing of the slits. 3) Two parallel slits are separated by 0.25 mm and illuminated with green light at a wavelength of 546.1 ...
Evolution of Planetary Science Activities in SPL
... research was largely aimed at developing theoretical models for explaining new observations made either by planetary spacecraft-based instruments or by space-based or ground-based telescopes. The studies include aurora and airglow emissions in the atmospheres of the outer planets and ultraviolet emi ...
... research was largely aimed at developing theoretical models for explaining new observations made either by planetary spacecraft-based instruments or by space-based or ground-based telescopes. The studies include aurora and airglow emissions in the atmospheres of the outer planets and ultraviolet emi ...
The future of gamma-ray astronomy
... mode. In this mode the telescope is kept stationary, and the sky is scanned as Earth rotates. They reported [12] a non-random component in the arrival times of cosmic ray events for time separation of ...
... mode. In this mode the telescope is kept stationary, and the sky is scanned as Earth rotates. They reported [12] a non-random component in the arrival times of cosmic ray events for time separation of ...
CV - iucaa
... workshop, Pune, February 2015 • “Observing facilities and time domain activities in India”, International Conference on Computational Physics — Global Observatory Network for Solar System Observations (GONSSO), Singapore, January 2015 • “Seeing what we hear: Electromagnetic counterparts to gravitati ...
... workshop, Pune, February 2015 • “Observing facilities and time domain activities in India”, International Conference on Computational Physics — Global Observatory Network for Solar System Observations (GONSSO), Singapore, January 2015 • “Seeing what we hear: Electromagnetic counterparts to gravitati ...
The Reflection Component from Cygnus X
... straint on the BH mass is 14.8 ± 1.0 M⊙ (Orosz et al. 2011). Cyg X-1 has been instrumental in improving our understanding of accreting BHs, their spectral states, and the relationship between the accretion disk and the jet (see Remillard & McClintock 2006 for a review of BH binaries). Currently, a m ...
... straint on the BH mass is 14.8 ± 1.0 M⊙ (Orosz et al. 2011). Cyg X-1 has been instrumental in improving our understanding of accreting BHs, their spectral states, and the relationship between the accretion disk and the jet (see Remillard & McClintock 2006 for a review of BH binaries). Currently, a m ...
PDF
... ASCA optical axis. This puts the source at the edge of the SIS detectors, limiting the utility of these data. We do not consider them further, focusing instead on the GIS instruments which have a much larger (250 ) FOV. The effective exposure time for the GIS is 2 × 11.5 ks. The image obtained from ...
... ASCA optical axis. This puts the source at the edge of the SIS detectors, limiting the utility of these data. We do not consider them further, focusing instead on the GIS instruments which have a much larger (250 ) FOV. The effective exposure time for the GIS is 2 × 11.5 ks. The image obtained from ...
Lecture 6 telescopes
... D larger than optical case, but wavelength much larger (cm's to m's), e.g. for wavelength = 1 cm, diameter = 100 m, resolution = 20". ...
... D larger than optical case, but wavelength much larger (cm's to m's), e.g. for wavelength = 1 cm, diameter = 100 m, resolution = 20". ...
Today in Astronomy 102: observations of stellar
... Search for such objects near visible stars. Most stars have stellar companions; if such a companion became a black hole, and the two were close enough together, material from the visible star could fall into the black hole, creating an X-ray source. Difficulty: X-rays are absorbed strongly by th ...
... Search for such objects near visible stars. Most stars have stellar companions; if such a companion became a black hole, and the two were close enough together, material from the visible star could fall into the black hole, creating an X-ray source. Difficulty: X-rays are absorbed strongly by th ...
Radiative Processes in Astrophysics
... Emission coefficient for coherent, isotropic scattering can be found simply by equating the power absorbed per unit volume and frequency ranges to corresponding power emitted: where &! is the SCATTERING COEFFICIENT Dividing by &! we find the source function for scattering equals mean intensity of th ...
... Emission coefficient for coherent, isotropic scattering can be found simply by equating the power absorbed per unit volume and frequency ranges to corresponding power emitted: where &! is the SCATTERING COEFFICIENT Dividing by &! we find the source function for scattering equals mean intensity of th ...
Computation of the off-axis effective area of the New Hard X
... wavelength, λ. This is the reason why this problem has been so far faced along with ray-tracing methods, aimed at reconstructing each X-ray path throughout the mirror shells assembly, and more specifically at sampling the incidence angles of the X-rays reflected on the reflective surfaces. Such rou ...
... wavelength, λ. This is the reason why this problem has been so far faced along with ray-tracing methods, aimed at reconstructing each X-ray path throughout the mirror shells assembly, and more specifically at sampling the incidence angles of the X-rays reflected on the reflective surfaces. Such rou ...
ANTARES: a deep-sea neutrino telescope
... The aims of this first phase, which is now ending, were to measure the deep-sea water properties, to find a convenient detector site, and to master the sea technologies required to deploy, connect and run large and complex pieces of apparatus offshore in a deep-sea environment. In parallel, studies ...
... The aims of this first phase, which is now ending, were to measure the deep-sea water properties, to find a convenient detector site, and to master the sea technologies required to deploy, connect and run large and complex pieces of apparatus offshore in a deep-sea environment. In parallel, studies ...
Martin`s presentation
... No current plans for a Chandra-class sub-arcsec - mission - world-wide No space agency developing high resolution X-ray mirrors Reason: Cannot make a bigger Chandra mirrors are heavy ...
... No current plans for a Chandra-class sub-arcsec - mission - world-wide No space agency developing high resolution X-ray mirrors Reason: Cannot make a bigger Chandra mirrors are heavy ...
CEA
... energies Lower S/N for WXM due to offset Durations increase by 65% at lower energies Hard-to-soft spectral evolution Peak energy flux in the 4-25 keV band is 1/3 of 50-300 keV Peak photon flux is ~4 times higher in the 4-25 keV ...
... energies Lower S/N for WXM due to offset Durations increase by 65% at lower energies Hard-to-soft spectral evolution Peak energy flux in the 4-25 keV band is 1/3 of 50-300 keV Peak photon flux is ~4 times higher in the 4-25 keV ...
SUPERNOVA EMISSION FROM GAMMA RAYS TO THE INFRARED
... The decays usually occur by electron capture, (electron) or + (positron) channels to an excited state in the (A,Z+1), (A,Z1) daughter nucleus. This state deexcites by the emission of gamma rays, with energies often exceeding the first step. Ex for 56Co: ...
... The decays usually occur by electron capture, (electron) or + (positron) channels to an excited state in the (A,Z+1), (A,Z1) daughter nucleus. This state deexcites by the emission of gamma rays, with energies often exceeding the first step. Ex for 56Co: ...
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.