sources of hard and soft x-ray emission in solar flares: mhd simulation
... The energy ~1032 erg, which is necessary for solar flare is accumulated in the magnetic field of the current sheet. Fast energy release at the current sheet transfer to unstable state causes the observational manifestations, which are explained by the electrodynamical model of the solar flare. The m ...
... The energy ~1032 erg, which is necessary for solar flare is accumulated in the magnetic field of the current sheet. Fast energy release at the current sheet transfer to unstable state causes the observational manifestations, which are explained by the electrodynamical model of the solar flare. The m ...
High Energy Astrophysics and Transient Science (or, a tale of radio
... Multiple optical observations made, also X-ray upper limits from RXTE ASM and MAXI No optical counterpart to (stacked) m ~22.5. No bright X-ray counterpart. These limits rule out: accreting binary (CV, X-ray binary), AGN What is left? Some flavour of neutron star? However, there are no pulsations Ne ...
... Multiple optical observations made, also X-ray upper limits from RXTE ASM and MAXI No optical counterpart to (stacked) m ~22.5. No bright X-ray counterpart. These limits rule out: accreting binary (CV, X-ray binary), AGN What is left? Some flavour of neutron star? However, there are no pulsations Ne ...
An Archive of Chandra Observations of Regions of Star Formation...
... The archive is designed to aid both the X-ray astronomer with a desire to compare X-ray datasets and the star formation astronomer wishing to compare stars across the spectrum. It brings together Chandra data on open clusters and other bright, variable, young stars for the study of the various physi ...
... The archive is designed to aid both the X-ray astronomer with a desire to compare X-ray datasets and the star formation astronomer wishing to compare stars across the spectrum. It brings together Chandra data on open clusters and other bright, variable, young stars for the study of the various physi ...
Study of the X-ray Source Population and the Dark Matter
... Wide-Field Imager Owing to the large effective area, large field of view, and high spatial and time resolution, the Wide Field Imager of the Athena Xray Observatory will make it possible to study X-ray sources down to very low flux limits. In Draco dSph, e.g., we will be able to observe X-ray source ...
... Wide-Field Imager Owing to the large effective area, large field of view, and high spatial and time resolution, the Wide Field Imager of the Athena Xray Observatory will make it possible to study X-ray sources down to very low flux limits. In Draco dSph, e.g., we will be able to observe X-ray source ...
NGC 5746 :: NGC 5746 Handout - Chandra X
... collapse to form spinning disks of stars and gas. The Chandra data and computer simulations show that the likely origin of NGC 5746's hot halo is the gradual inflow of intergalactic matter left over from the formation of the galaxy. Hot gas flowing outward has been observed in galaxies with vigorous ...
... collapse to form spinning disks of stars and gas. The Chandra data and computer simulations show that the likely origin of NGC 5746's hot halo is the gradual inflow of intergalactic matter left over from the formation of the galaxy. Hot gas flowing outward has been observed in galaxies with vigorous ...
X-ray Sources in Nearby Galaxies Q. Daniel Wang University of Massachusetts
... • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scattering, & synchrotr ...
... • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scattering, & synchrotr ...
Bez tytułu slajdu
... u) which protects us from falling the nucleus of 58Fe, for example, to a quark state. Chandra X-ray observation of RX J1856.5-3754 (or the C58 pulsar), the remnants of a supernova noted on Earth in AD 1181, reveal that the neutron star in the core has a temperature much lower than expected. This sug ...
... u) which protects us from falling the nucleus of 58Fe, for example, to a quark state. Chandra X-ray observation of RX J1856.5-3754 (or the C58 pulsar), the remnants of a supernova noted on Earth in AD 1181, reveal that the neutron star in the core has a temperature much lower than expected. This sug ...
ppt - UCL
... inferred from the X-ray data. The companion was previously thought to be a main sequence B3 star ...
... inferred from the X-ray data. The companion was previously thought to be a main sequence B3 star ...
X-ray astronomy - University of Warwick
... – Data from old missions available – Uniform data format, calibration and analysis recipes – High level products often available ...
... – Data from old missions available – Uniform data format, calibration and analysis recipes – High level products often available ...
ppt - SLAC
... prominent emission lines of helium and nitrogen, and type WC in which carbon, oxygen and helium lines dominate. They are named after the French astronomers Charles Wolf (1827-1918) and Georges Rayet (1839-1906) who studied the first example in 1867. “ ...
... prominent emission lines of helium and nitrogen, and type WC in which carbon, oxygen and helium lines dominate. They are named after the French astronomers Charles Wolf (1827-1918) and Georges Rayet (1839-1906) who studied the first example in 1867. “ ...
LETG Spring, 2015
... over the last few years. Can the cliché “solar-stellar” connection come to the rescue? Probably not, but it’s a reasonable place to start to understand solar behavior we cannot observe at the present time. Fortunately, we only have to go a parsec or so to get to a star reasonably close to the Sun in ...
... over the last few years. Can the cliché “solar-stellar” connection come to the rescue? Probably not, but it’s a reasonable place to start to understand solar behavior we cannot observe at the present time. Fortunately, we only have to go a parsec or so to get to a star reasonably close to the Sun in ...
Radio-quiet Isolated Neutron Stars
... Obtain an upper limit of 2.7% on the unaccelerated pulse fraction in 2000/03 for 55ks by LETG and HRC-S data. ...
... Obtain an upper limit of 2.7% on the unaccelerated pulse fraction in 2000/03 for 55ks by LETG and HRC-S data. ...
ppt
... R. J. Hanisch, A. A. Suchkov, R. L. White Space Telescope Science Institute T. A. McGlynn, E. L. Winter, M. F. Corcoran NASA Goddard Space Flight Center W. Voges Max-Planck-Institute for Extraterrestrial Physics ...
... R. J. Hanisch, A. A. Suchkov, R. L. White Space Telescope Science Institute T. A. McGlynn, E. L. Winter, M. F. Corcoran NASA Goddard Space Flight Center W. Voges Max-Planck-Institute for Extraterrestrial Physics ...
Astronomy news
... A 70ks long observation of RX J1856 was carried out with XMM staring on 2006 Oct. 24 at 00:30 UT. After data reduction, the event files result in net exposure times of 47 and 68 ks for the pn and MOS. Due to the very soft spectrum of RX J1856, they started timing analysis using the data of pn camera ...
... A 70ks long observation of RX J1856 was carried out with XMM staring on 2006 Oct. 24 at 00:30 UT. After data reduction, the event files result in net exposure times of 47 and 68 ks for the pn and MOS. Due to the very soft spectrum of RX J1856, they started timing analysis using the data of pn camera ...
The activities of the Astronomical Institute of the Slovak Academy of
... The activities of the Astronomical Institute of the Slovak Academy of Sciences (AISAS), Tatranská Lomnica (http://www.astro.sk), related to COSPAR, were devoted to the research in solar and stellar physics using different satellite observations, mainly in the UV, XUV and X-ray spectral regions. Main ...
... The activities of the Astronomical Institute of the Slovak Academy of Sciences (AISAS), Tatranská Lomnica (http://www.astro.sk), related to COSPAR, were devoted to the research in solar and stellar physics using different satellite observations, mainly in the UV, XUV and X-ray spectral regions. Main ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean density of PMS stars of ∼750 stars deg−2. Our sensitivity limit ...
... emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean density of PMS stars of ∼750 stars deg−2. Our sensitivity limit ...
L129 DISCOVERY OF A NEW 89 SECOND X
... variable pulse shape with energy (Fig. 2) is characteristic of accretion-powered neutron star systems, in which the emergent X-ray emission pattern is determined by the geometry and the distribution of matter in the vicinity. The scattering cross section is also energy dependent, and hence the pulse ...
... variable pulse shape with energy (Fig. 2) is characteristic of accretion-powered neutron star systems, in which the emergent X-ray emission pattern is determined by the geometry and the distribution of matter in the vicinity. The scattering cross section is also energy dependent, and hence the pulse ...
Multiwavelength Imaging of Planetary Nebulae: Resolving Disentangling PN Structure
... Disentangling PN Structure Advisor: Joel Kastner Thursday, August 6th, 10:00am Location: Carlson Center 76-1125 Abstract: Planetary nebulae (PNe) represent the late stages of low-mass stellar evolution. The formation of the myriad of PNe morphologies involves processes that are present in many other ...
... Disentangling PN Structure Advisor: Joel Kastner Thursday, August 6th, 10:00am Location: Carlson Center 76-1125 Abstract: Planetary nebulae (PNe) represent the late stages of low-mass stellar evolution. The formation of the myriad of PNe morphologies involves processes that are present in many other ...
parents_weekend_2006 - Astronomy at Swarthmore College
... Micah Walter-Range (’06) and Steve St. Vincent (’07) are making computer models of the x-ray emitting plasma on some of the most massive and luminous stars in the Galaxy; like the star at the center of the Orion Nebula. ...
... Micah Walter-Range (’06) and Steve St. Vincent (’07) are making computer models of the x-ray emitting plasma on some of the most massive and luminous stars in the Galaxy; like the star at the center of the Orion Nebula. ...
Solar-B - to Nobeyama Radio Observatory
... Solar-B data, together with analysis software tools, will be opened to the world solar physics (and related) communities as quickly as possible. (hopefully in a few months after data acquisition) We welcome proposals for observation plans from outside the Solar-B team. (Details TBD) Collaborative ob ...
... Solar-B data, together with analysis software tools, will be opened to the world solar physics (and related) communities as quickly as possible. (hopefully in a few months after data acquisition) We welcome proposals for observation plans from outside the Solar-B team. (Details TBD) Collaborative ob ...
X-ray effects on protoplanetary disks
... magnetic flares are ubiquitous throughout the epoch of planet formation, 103 above solar levels. The astrophysics resembles gigantic solar flares. • X-rays can efficiently irradiate protoplanetary disks. X-ray evidence: IR evidence: ...
... magnetic flares are ubiquitous throughout the epoch of planet formation, 103 above solar levels. The astrophysics resembles gigantic solar flares. • X-rays can efficiently irradiate protoplanetary disks. X-ray evidence: IR evidence: ...
9. Fascinating observations. But how much is well understood?
... pulse period t P and large derivative t&P . For this purpose we present a t P - t&P diagram (9.5) and look for systems at the upper right. There are 2 kinds of data points, black filled circles and red squares. The first belong to the class of Soft Gamma Repeters (SGR). They are transient sources wh ...
... pulse period t P and large derivative t&P . For this purpose we present a t P - t&P diagram (9.5) and look for systems at the upper right. There are 2 kinds of data points, black filled circles and red squares. The first belong to the class of Soft Gamma Repeters (SGR). They are transient sources wh ...
The ultra-luminous x-ray sources near center of M82
... off-nuclear X-ray sources (not at the center) with isotropic luminosities much higher than the Eddington limit for a solar mass black hole (Lx ~ 1.381038 erg/s) Typical X-ray luminosities of ULXs are in between 1039 erg/s and 1041 erg/s (AGN > 1041 erg/s) ...
... off-nuclear X-ray sources (not at the center) with isotropic luminosities much higher than the Eddington limit for a solar mass black hole (Lx ~ 1.381038 erg/s) Typical X-ray luminosities of ULXs are in between 1039 erg/s and 1041 erg/s (AGN > 1041 erg/s) ...
X-ray spectrometer
... Hard X-ray imaging satellite NuSTAR • NASA’s Small Explorer mission, slated to fly in 2011-2012 • Two identical coaligned grazing incidence hard X-ray telescopes: – Multilayer coated segmented glass optics – Actively shielded solid state CdZnTe pixel detectors • Extendable mast provides 10-m focal ...
... Hard X-ray imaging satellite NuSTAR • NASA’s Small Explorer mission, slated to fly in 2011-2012 • Two identical coaligned grazing incidence hard X-ray telescopes: – Multilayer coated segmented glass optics – Actively shielded solid state CdZnTe pixel detectors • Extendable mast provides 10-m focal ...
X-ray Observations of Cosmic Accelerators Greg Madejski SLAC/KIPAC
... • Tools of X-ray astronomy: detectors and telescopes • Observations: Zoo of X-ray sources in the sky • Case studies and “X-ray insights” into the questions of particle acceleration in the cosmos: today - supernova remnants and X-ray binaries ...
... • Tools of X-ray astronomy: detectors and telescopes • Observations: Zoo of X-ray sources in the sky • Case studies and “X-ray insights” into the questions of particle acceleration in the cosmos: today - supernova remnants and X-ray binaries ...
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.