L95 IRON-RICH EJECTA IN THE SUPERNOVA
... region of reverse-shock–heated ejecta. The abundances of the outer shock are consistent with LMC values, while the ejecta region shows enhanced abundances of Si, Fe, and other species. However, oxygen is not enhanced in the ejecta; the Fe/O abundance ratio there is ⲏ5 times the solar ratio. Based on ...
... region of reverse-shock–heated ejecta. The abundances of the outer shock are consistent with LMC values, while the ejecta region shows enhanced abundances of Si, Fe, and other species. However, oxygen is not enhanced in the ejecta; the Fe/O abundance ratio there is ⲏ5 times the solar ratio. Based on ...
Astronomy Astrophysics Astrophysical parameters and orbital solution of the peculiar X-ray
... higher than the interstellar value, leading to the suggestion that the system is powered by wind accretion in a very eccentric orbit (in ’t Zand et al. 2007). Pointed RXTE/PCA observations detected a very likely modulation at 346 ± 6 s during a bright X-ray flare, which was interpreted as the detect ...
... higher than the interstellar value, leading to the suggestion that the system is powered by wind accretion in a very eccentric orbit (in ’t Zand et al. 2007). Pointed RXTE/PCA observations detected a very likely modulation at 346 ± 6 s during a bright X-ray flare, which was interpreted as the detect ...
Today in Astronomy 102: black hole observations, v.2
... GRO J1655-40 (a.k.a. Nova Scorpii 1994) is an X-ray transient source discovered by NASA’s Compton Gamma-Ray Observatory (GRO) in 1994. Rapidly-variable emission in its X-ray bursts: the X-ray object is a few hundred km around. The X-ray source has a stellar companion, a star rather similar to th ...
... GRO J1655-40 (a.k.a. Nova Scorpii 1994) is an X-ray transient source discovered by NASA’s Compton Gamma-Ray Observatory (GRO) in 1994. Rapidly-variable emission in its X-ray bursts: the X-ray object is a few hundred km around. The X-ray source has a stellar companion, a star rather similar to th ...
Laboratory Studies of Organic Chemistry in Space A. Ciaravella
... Laboratory vs ISM Conditions: II In the best case the density inside the chamber is: ≈ 1.3 × 106 particle cm-3 !!! !! MUCH MORE dense (> 104 times) than the average density in ISM This value is closer to: ...
... Laboratory vs ISM Conditions: II In the best case the density inside the chamber is: ≈ 1.3 × 106 particle cm-3 !!! !! MUCH MORE dense (> 104 times) than the average density in ISM This value is closer to: ...
X-ray and UV Transients
... >10 events y-1 even if the sensitivity is 102 less. • The observed signals have UV flux~host, so confusion with (even mildly) variable sources is an issue unless additional information is available • A combined UV survey+optical SN survey like PTF will be powerful to get retrospective measurements ...
... >10 events y-1 even if the sensitivity is 102 less. • The observed signals have UV flux~host, so confusion with (even mildly) variable sources is an issue unless additional information is available • A combined UV survey+optical SN survey like PTF will be powerful to get retrospective measurements ...
The ultracompact nature of the black hole candidate X
... 47 Tuc X9 is a low mass X-ray binary (LMXB) in the globular cluster 47 Tucanae, and was previously thought to be a cataclysmic variable. However, Miller-Jones et al. (2015) recently identified a radio counterpart to X9 (inferring a radio/X-ray luminosity ratio consistent with black hole LMXBs), and ...
... 47 Tuc X9 is a low mass X-ray binary (LMXB) in the globular cluster 47 Tucanae, and was previously thought to be a cataclysmic variable. However, Miller-Jones et al. (2015) recently identified a radio counterpart to X9 (inferring a radio/X-ray luminosity ratio consistent with black hole LMXBs), and ...
Ultraluminous X-ray Sources in Andromeda Galaxy
... Proportional Counter instrument (FWHM ∼ 1’) on Einstein, it was difficult to separate these sources from the nucleus of galaxies. These observations lead to various speculations about the nature of these X-ray sources e.g. AGNs with a low accretion rate, a massive stellar mass black hole accreting a ...
... Proportional Counter instrument (FWHM ∼ 1’) on Einstein, it was difficult to separate these sources from the nucleus of galaxies. These observations lead to various speculations about the nature of these X-ray sources e.g. AGNs with a low accretion rate, a massive stellar mass black hole accreting a ...
Measuring the orbital periods of low mass X-ray binaries in the X
... the compactness of the X-ray binary systems; the size of an HMXB is about tens of solar radii but the size of an LMXB is typically less than or equal to a solar radius. However, fewer than half of X-ray binaries have known orbital periods. According to the 4th edition of catalogs of HMXBs (Liu et al ...
... the compactness of the X-ray binary systems; the size of an HMXB is about tens of solar radii but the size of an LMXB is typically less than or equal to a solar radius. However, fewer than half of X-ray binaries have known orbital periods. According to the 4th edition of catalogs of HMXBs (Liu et al ...
X-Ray Properties of Young Stars and Stellar Clusters
... ment of the stellar surface by electron beams. Thus, young stars prolifically accelerate particles to relativistic energies. In rich young stellar clusters, X-rays are also produced by shocks in O-star winds, on both small (<102 R★) and large (parsec) scales. If the region has been producing rich cl ...
... ment of the stellar surface by electron beams. Thus, young stars prolifically accelerate particles to relativistic energies. In rich young stellar clusters, X-rays are also produced by shocks in O-star winds, on both small (<102 R★) and large (parsec) scales. If the region has been producing rich cl ...
Document
... - The galaxy masses have been estimated from their SED - z~2 obscured AGNs have MBH/Mstar lower than the local relation, in contrast with unobscured AGNs ...
... - The galaxy masses have been estimated from their SED - z~2 obscured AGNs have MBH/Mstar lower than the local relation, in contrast with unobscured AGNs ...
eROSITA Mission Definition Document
... Most of the light created after the «dark ages» in the Universe comes from active centres of galaxies, emitted either by vigorous star formation processes or by prodigious supermassive black holes residing in the centre of almost every galaxy, swallowing stars and gas. It was only realized in recent ...
... Most of the light created after the «dark ages» in the Universe comes from active centres of galaxies, emitted either by vigorous star formation processes or by prodigious supermassive black holes residing in the centre of almost every galaxy, swallowing stars and gas. It was only realized in recent ...
The coronal temperatures of low-mass main
... mass-independent value of RX . It would further imply that all saturated stars have similar coronal temperatures. On the other hand, if either LX or FX are the relevant parameters, then it would indicate that among stars that lie above the saturation threshold, lower mass stars have cooler coronae t ...
... mass-independent value of RX . It would further imply that all saturated stars have similar coronal temperatures. On the other hand, if either LX or FX are the relevant parameters, then it would indicate that among stars that lie above the saturation threshold, lower mass stars have cooler coronae t ...
Results from the search for tidal disruption flares in the GALEX Deep
... holes lurking in the nuclei of normal galaxies. • The luminosity, temperature, and decay of the flare is dependent on the mass and spin of the black hole. • They may contribute to black hole growth over cosmic times, and the faint end of the AGN luminosity function. • Tidal disruption rates are sens ...
... holes lurking in the nuclei of normal galaxies. • The luminosity, temperature, and decay of the flare is dependent on the mass and spin of the black hole. • They may contribute to black hole growth over cosmic times, and the faint end of the AGN luminosity function. • Tidal disruption rates are sens ...
Computation of the off-axis effective area of the New Hard X
... angles of the X-rays reflected on the reflective surfaces. Such routines are recognized as very effective and accurate, but they are often of complex implementation and require a considerable computation time. Even if this is a viable approach, it is also possible to solve that problem from an analy ...
... angles of the X-rays reflected on the reflective surfaces. Such routines are recognized as very effective and accurate, but they are often of complex implementation and require a considerable computation time. Even if this is a viable approach, it is also possible to solve that problem from an analy ...
X-Ray and Extreme Ultraviolet Emission from Comets
... a better understanding of a number of physical phenomena: the nature of the cometary coma, other sources of X-ray emission in the solar system, the structure of the solar wind in the heliosphere, and the source of the local soft X-ray background. ...
... a better understanding of a number of physical phenomena: the nature of the cometary coma, other sources of X-ray emission in the solar system, the structure of the solar wind in the heliosphere, and the source of the local soft X-ray background. ...
Astronomy Astrophysics − Astrophysical parameters of the peculiar X-ray transient
... Context. The current generation of X-ray satellites has discovered many new X-ray sources that are difficult to classify within the well-described subclasses. The hard X-ray source IGR J11215−5952 is a peculiar transient, displaying very short X-ray outbursts every 165 days. Aims. To characterise the ...
... Context. The current generation of X-ray satellites has discovered many new X-ray sources that are difficult to classify within the well-described subclasses. The hard X-ray source IGR J11215−5952 is a peculiar transient, displaying very short X-ray outbursts every 165 days. Aims. To characterise the ...
PPT - Chandra X-Ray Observatory
... opacity strongly reduced → DAs with Teff >30,000 K can emit thermal soft X-rays from deep hot layers • However, ROSAT All-Sky Survey revealed that X-ray emission is the exception rather than the rule → additional absorbers present • ROSAT and EUVE revealed that metals are the origin, EUV spectra are ...
... opacity strongly reduced → DAs with Teff >30,000 K can emit thermal soft X-rays from deep hot layers • However, ROSAT All-Sky Survey revealed that X-ray emission is the exception rather than the rule → additional absorbers present • ROSAT and EUVE revealed that metals are the origin, EUV spectra are ...
Studies on post-flare loop prominence of 1981 April 27
... 2. The Impulsive Burst and Growth of the Post-Flare Loop The flare started before 08 : 00 UT. Due to the fact that the flare is located on the limb of the Sun, it has not been possible to determine the exact flare onset. Most observational astronomers in China suggest that the main part of the flare ...
... 2. The Impulsive Burst and Growth of the Post-Flare Loop The flare started before 08 : 00 UT. Due to the fact that the flare is located on the limb of the Sun, it has not been possible to determine the exact flare onset. Most observational astronomers in China suggest that the main part of the flare ...
Introduction to X-ray Absorption Spectroscopy, Extended X
... X-ray fluorescence for dilute samples ...
... X-ray fluorescence for dilute samples ...
L171 COULD BLACK HOLE X-RAY BINARIES BE DETECTED IN
... DC p fXtMT /tex ! 10⫺3 would be compatible with the absence of any detection in the ∼100 Galactic GCs. In contrast to post-exchange binaries, TC binaries are expected to form systems with very short orbital periods. Taking the typical closest-approach distance for TC to be 3 R,, we find the orbital ...
... DC p fXtMT /tex ! 10⫺3 would be compatible with the absence of any detection in the ∼100 Galactic GCs. In contrast to post-exchange binaries, TC binaries are expected to form systems with very short orbital periods. Taking the typical closest-approach distance for TC to be 3 R,, we find the orbital ...
Stellar-Mass Black Holes and Ultraluminous X
... more efficient outwards transfer of system GX 339-4, a key source in our understanding of black hole accretion exists in the hard state, which may have angular momentum and inwards trans- and the source of the data presented in Fig. 2. [Image produced with BinSim a steeper correlation (12), and yet ...
... more efficient outwards transfer of system GX 339-4, a key source in our understanding of black hole accretion exists in the hard state, which may have angular momentum and inwards trans- and the source of the data presented in Fig. 2. [Image produced with BinSim a steeper correlation (12), and yet ...
CANGAROO and VHE γ-ray Astronomy: Past, present and future
... • Frontiers of Topics : objects peculiar to TeV γ-rays populations and number of samples “Origin of cosmic rays” to more generally “energetic processes in the Universe” ...
... • Frontiers of Topics : objects peculiar to TeV γ-rays populations and number of samples “Origin of cosmic rays” to more generally “energetic processes in the Universe” ...
the chandra deep field–north survey. xvii. evolution of
... listed in Table 1. The precision of this curve is not well established, since it is based on a complex wavelet source detection procedure applied to a field with an inhomogeneous exposure map. We estimate that the sensitivity values could be inaccurate by as much as 30%. We have extracted our sampl ...
... listed in Table 1. The precision of this curve is not well established, since it is based on a complex wavelet source detection procedure applied to a field with an inhomogeneous exposure map. We estimate that the sensitivity values could be inaccurate by as much as 30%. We have extracted our sampl ...
Indications for an influence of Hot Jupiters
... testing for tidal or magnetic interaction effects in samples of planet-hosting stars is difficult because stellar activity hinders exoplanet detection, so that stellar samples with detected exoplanets show a bias towards low activity for small exoplanets. Aims. We aim to test if exoplanets in close ...
... testing for tidal or magnetic interaction effects in samples of planet-hosting stars is difficult because stellar activity hinders exoplanet detection, so that stellar samples with detected exoplanets show a bias towards low activity for small exoplanets. Aims. We aim to test if exoplanets in close ...
Coevolution of SMBHs and host galaxies at high z
... Estimated MBH using virial mass estimator for the few z~2 SMGs with broad lines Estimated MGAL for the majority which are host-galaxy dominated SAM results, including feedback ...
... Estimated MBH using virial mass estimator for the few z~2 SMGs with broad lines Estimated MGAL for the majority which are host-galaxy dominated SAM results, including feedback ...
History of X-ray astronomy
The history of X-ray astronomy begins in the 1920s, with interest in short wave communications for the U.S. Navy. This was soon followed by extensive study of the earth's ionosphere. By 1927, interest in the detection of X-ray and ultraviolet (UV) radiation at high altitudes inspired researchers to launch Goddard's rockets into the upper atmosphere to support theoretical studies and data gathering. The first successful rocket flight equipped with instrumentation able to detect solar ultraviolet radiation occurred in 1946. X-ray solar studies began in 1949. By 1973 a solar instrument package orbited on Skylab providing significant solar data.In 1965 the Goddard Space Flight Center program in X-ray astronomy was initiated with a series of balloon-borne experiments. In the 1970s this was followed by high altitude sounding rocket experiments, and that was followed by orbiting (satellite) observatories.The first rocket flight to successfully detect a cosmic source of X-ray emission was launched in 1962 by a group at American Science and Engineering (AS&E).X-ray wavelengths reveal information about the bodies (sources) that emit them.