A neutron star with a carbon atmosphere in the Cassiopeia A
... neutron star surface, which would probably result in X-ray pulsations as the hot spot rotated with the star. However, these pulsations have not been detected.4,15 Fits to the data were performed using an additional (temperature) component, for example, a second blackbody or atmosphere spectrum, whic ...
... neutron star surface, which would probably result in X-ray pulsations as the hot spot rotated with the star. However, these pulsations have not been detected.4,15 Fits to the data were performed using an additional (temperature) component, for example, a second blackbody or atmosphere spectrum, whic ...
telescope
... X-ray and Gamma-ray telescopes are usually on Earth-orbiting satellites or high-flying balloons since the Earth's atmosphere is opaque to this part of the electromagnetic spectrum. For instance, the ASTROSAT astronomy mission will be launched in 2010. It will be loaded on a satellite in a 650-km, ne ...
... X-ray and Gamma-ray telescopes are usually on Earth-orbiting satellites or high-flying balloons since the Earth's atmosphere is opaque to this part of the electromagnetic spectrum. For instance, the ASTROSAT astronomy mission will be launched in 2010. It will be loaded on a satellite in a 650-km, ne ...
Measuring the orbital periods of low mass X-ray binaries in the X
... some are located in globular clusters so their optical counterparts are difficult to identify in such crowded regions with a large number of stars. Even if the optical counterparts are known, measuring the orbital Doppler effects from the companion for some LMXBs is still very difficult because they ...
... some are located in globular clusters so their optical counterparts are difficult to identify in such crowded regions with a large number of stars. Even if the optical counterparts are known, measuring the orbital Doppler effects from the companion for some LMXBs is still very difficult because they ...
Transparencies - Rencontres de Moriond
... For photon-noise dominated observations, the S/N gain proportional to D at fixed time and flux, the speed (1/ time required to reach given S/N ) to D2 ). For sky limited observations of point-like sources at natural seeing (0.7 at V, 0.4” FWHM at K), the S/N proportional to D , the speed to D 2. H ...
... For photon-noise dominated observations, the S/N gain proportional to D at fixed time and flux, the speed (1/ time required to reach given S/N ) to D2 ). For sky limited observations of point-like sources at natural seeing (0.7 at V, 0.4” FWHM at K), the S/N proportional to D , the speed to D 2. H ...
From: BXSVR0::OWOCKI 12-JAN-2001 10:16:41.12 To: DCOHEN
... are too low for collisional de-excitation or collisional excitation from excited states to be important; however, this assumption is not strictly a good one: metastable levels do get populated, and collisions (and even some radiative transitions in the UV that affect X-ray lines -- see Wayne and Joe ...
... are too low for collisional de-excitation or collisional excitation from excited states to be important; however, this assumption is not strictly a good one: metastable levels do get populated, and collisions (and even some radiative transitions in the UV that affect X-ray lines -- see Wayne and Joe ...
Status of the search for Gravitational Waves
... where LIGO noise is high - we see the inspiral Higher-mass systems (BBH) merge or ring down in-band. ...
... where LIGO noise is high - we see the inspiral Higher-mass systems (BBH) merge or ring down in-band. ...
gamma rays interaction with matter
... cannot remain indefinitely in an excited state, thus: 1. The atom emits x rays and returns to the ground state. 2. Auger electrons are emitted from the outer electronic shells carrying out the excitation energy. This secondary radiation is also later absorbed and occurs in scintillators used in gamm ...
... cannot remain indefinitely in an excited state, thus: 1. The atom emits x rays and returns to the ground state. 2. Auger electrons are emitted from the outer electronic shells carrying out the excitation energy. This secondary radiation is also later absorbed and occurs in scintillators used in gamm ...
The Virgo interferometer for Gravitational Wave detection
... – Increased sensitivity in merge and ringdown phase (GR, EOS) – Increased number of pulsars (EOS, population, ) – Stochastic background (cosmological and astrophysical) – Coincidences with g and X-ray satellites, observatories, …(system dynamics) ...
... – Increased sensitivity in merge and ringdown phase (GR, EOS) – Increased number of pulsars (EOS, population, ) – Stochastic background (cosmological and astrophysical) – Coincidences with g and X-ray satellites, observatories, …(system dynamics) ...
Document
... Why is cooling sensitive to the neutron star interior? The interior of a proto-neutron star loses energy at a rapid rate by neutrino emission. Within ~10 to 100 years, the thermal evolution time of the crust, heat transported by electron conduction into the interior, where it is radiated away by neu ...
... Why is cooling sensitive to the neutron star interior? The interior of a proto-neutron star loses energy at a rapid rate by neutrino emission. Within ~10 to 100 years, the thermal evolution time of the crust, heat transported by electron conduction into the interior, where it is radiated away by neu ...
Measuring difficult reaction rates involving
... - 32S(p,d)31S ; 31P(3He,t)31S(p)30P new levels - -decay of 31Cl to 31S (p decay) new levels - HI rxs. populating levels in 31S (p, ) estimate - Based on models, rate is higher than now believed. Re-evaluation of the 30P(p,)31S astrophysical reaction rate from study of the T=1/2 mirror nucle ...
... - 32S(p,d)31S ; 31P(3He,t)31S(p)30P new levels - -decay of 31Cl to 31S (p decay) new levels - HI rxs. populating levels in 31S (p, ) estimate - Based on models, rate is higher than now believed. Re-evaluation of the 30P(p,)31S astrophysical reaction rate from study of the T=1/2 mirror nucle ...
SPIE - Twinkle Space Mission
... The same architecture can be viewed in Figure 2-2 and Figure 2-3 where the two channels have been separated and shown in projection views for clarity. The two projections are referred to as “Plan” and “Elevation”. The latter being the dispersion plane where the separation of rays caused by the diff ...
... The same architecture can be viewed in Figure 2-2 and Figure 2-3 where the two channels have been separated and shown in projection views for clarity. The two projections are referred to as “Plan” and “Elevation”. The latter being the dispersion plane where the separation of rays caused by the diff ...
TWINKLE – A Low Earth Orbit Visible and Infrared Exoplanet
... The Infra-Red Science Instrument is on the other hand an original design, the details of which are outlined in full in a sister paper in this conference [7]. The goal of this design was to allow from a single incoming high F-number beam, the split in two separate channels (given the broadband nature ...
... The Infra-Red Science Instrument is on the other hand an original design, the details of which are outlined in full in a sister paper in this conference [7]. The goal of this design was to allow from a single incoming high F-number beam, the split in two separate channels (given the broadband nature ...
Chapter 3 Telescopes - UT Austin (Astronomy)
... between waves over the distance between individual telescopes ...
... between waves over the distance between individual telescopes ...
doc - IRAM
... Short answer/summary: Use warm or cold dichroics allowing for several focal planes in several or one cryostat. LEKIDs are promising for a multicolor instrument. Key points of the discussion: Warm dichroics efficiencies ~95%, for small incidence angles. Work ongoing to develop dichroics efficient a ...
... Short answer/summary: Use warm or cold dichroics allowing for several focal planes in several or one cryostat. LEKIDs are promising for a multicolor instrument. Key points of the discussion: Warm dichroics efficiencies ~95%, for small incidence angles. Work ongoing to develop dichroics efficient a ...
The Local Bubble
... all,A or due to ISM are filled with hot gas, then in principle cavities in the red) are potential SXRB sources if they po-rather lar plot of the unabsorbed (foreground) 0.25between keV diffuse background charge exchange reactions solar windknowledge ions andof the 3D geometry of the ISM may be used t ...
... all,A or due to ISM are filled with hot gas, then in principle cavities in the red) are potential SXRB sources if they po-rather lar plot of the unabsorbed (foreground) 0.25between keV diffuse background charge exchange reactions solar windknowledge ions andof the 3D geometry of the ISM may be used t ...
Solar chromospheric flares: energy release, transport and radiation
... by a magnetic convulsion propagating downwards, with roughly the same total energy (as indicated by studies of flare and CME energetics) but launched into a much smaller volume and onto a field which is line-tied at the photosphere. This Poynting-flux picture is far less developed than the electron ...
... by a magnetic convulsion propagating downwards, with roughly the same total energy (as indicated by studies of flare and CME energetics) but launched into a much smaller volume and onto a field which is line-tied at the photosphere. This Poynting-flux picture is far less developed than the electron ...
What caused the GeV flare of PSR B1259-63?
... however, that the emission from the cone seen at a given location is not isotropic). The cone axis is oriented along the lineof-centres joining the Be star to the pulsar. The cone apex is located at the standoff distance between the two winds (≈0.6× the orbital separation from the Be star for η = 0.5 ...
... however, that the emission from the cone seen at a given location is not isotropic). The cone axis is oriented along the lineof-centres joining the Be star to the pulsar. The cone apex is located at the standoff distance between the two winds (≈0.6× the orbital separation from the Be star for η = 0.5 ...
Tools of Astronomy - Indiana University Astronomy
... X-rays do not reflect off mirrors the same way that visible light does X-ray photons penetrate into the mirror in much the same way that bullets slam into a wall X-rays ricochet off mirrors like bullets off a wall X-ray telescopes are very different from optical telescopes. ...
... X-rays do not reflect off mirrors the same way that visible light does X-ray photons penetrate into the mirror in much the same way that bullets slam into a wall X-rays ricochet off mirrors like bullets off a wall X-ray telescopes are very different from optical telescopes. ...
Radiation Environment of the Chandra X-ray Observatory yr
... Instrument Module (ISTM). On a translation table within the 15Th/I, reside the two focal-plane instruments the Advanced CCD Tmaging Spectrometer (ACTS) and the High-Resolution Camera (HRC). The ACTS focal plane (shown without optical blocking filters) contains 4 CCDs in the square Imaging (T) array ...
... Instrument Module (ISTM). On a translation table within the 15Th/I, reside the two focal-plane instruments the Advanced CCD Tmaging Spectrometer (ACTS) and the High-Resolution Camera (HRC). The ACTS focal plane (shown without optical blocking filters) contains 4 CCDs in the square Imaging (T) array ...
Photoneutron cross sections for samarium isotopes: Toward a
... fitting and the energy linearity of the γ -ray detector in its response to multiphotons. For each neutron measurement run we recorded the γ -ray spectra, when the laser is on in the full power mode. Multiple photons were detected simultaneously, generating a so-called pile-up spectrum. Before or aft ...
... fitting and the energy linearity of the γ -ray detector in its response to multiphotons. For each neutron measurement run we recorded the γ -ray spectra, when the laser is on in the full power mode. Multiple photons were detected simultaneously, generating a so-called pile-up spectrum. Before or aft ...
Studies of Gamma-Ray Burst Prompt Emission with RHESSI and NCT by
... irregular gamma-ray emission. This initial “prompt” emission is followed by “afterglow” emission at other wavelengths that fades smoothly over hours to years. GRB prompt emission has been observed with ever-increasing sophistication for more than four decades, but many details of its origin remain u ...
... irregular gamma-ray emission. This initial “prompt” emission is followed by “afterglow” emission at other wavelengths that fades smoothly over hours to years. GRB prompt emission has been observed with ever-increasing sophistication for more than four decades, but many details of its origin remain u ...
Nucleon mean-free path in the medium
... in nuclear matter. The effect of temperature is relevant in an area of about 20 MeV around the Fermi surface. By switching on temperature, the mean-free path at the Fermi surface becomes finite due to thermal damping. Thermal effects are otherwise negligible for the very high and low energy behaviou ...
... in nuclear matter. The effect of temperature is relevant in an area of about 20 MeV around the Fermi surface. By switching on temperature, the mean-free path at the Fermi surface becomes finite due to thermal damping. Thermal effects are otherwise negligible for the very high and low energy behaviou ...
Lecture 2. Isolated Neutron Stars – I.
... UHURU The satellite was launched on December 12, 1970. The program was ended in March 1973. The other name SAS-1 2-20 keV The first full sky survey. 339 sources. ...
... UHURU The satellite was launched on December 12, 1970. The program was ended in March 1973. The other name SAS-1 2-20 keV The first full sky survey. 339 sources. ...
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.