Broad Relativistic Iron Lines from Neutron Star LMXBs
... (c) A study of accretion-ejection in X-ray binaries provides an important tool to probe the strong gravity regime. ...
... (c) A study of accretion-ejection in X-ray binaries provides an important tool to probe the strong gravity regime. ...
Black Hole Binaries in Quiescence
... XRBs are a key precursor class for gravitational wave sources – empirical demographics are key for use of LIGO as an astronomical facility Transients with duty cycle >50 years recurrence time unavailable, so total numbers cannot be inferred A0620 is an exception: archival optical data shows outburst ...
... XRBs are a key precursor class for gravitational wave sources – empirical demographics are key for use of LIGO as an astronomical facility Transients with duty cycle >50 years recurrence time unavailable, so total numbers cannot be inferred A0620 is an exception: archival optical data shows outburst ...
Strongly Interacting Supernovae - The National Centre for Radio
... Swift observations started from Sep 4 until Dec 2012. No X-ray emission during the decay of 2012 outburst i.e t<22nd Sept (3-sigma~3E-3 cps). ...
... Swift observations started from Sep 4 until Dec 2012. No X-ray emission during the decay of 2012 outburst i.e t<22nd Sept (3-sigma~3E-3 cps). ...
Today in Astronomy 102: observations of stellar
... directly in images, but we can measure orbital speeds and periods well enough to work out what the orbit is, using the Doppler effect. 25 October 2001 ...
... directly in images, but we can measure orbital speeds and periods well enough to work out what the orbit is, using the Doppler effect. 25 October 2001 ...
Chandra Observation of Pulsar Wind Nebula
... between the ejecta and a bulk of materials in the interior of the remnant, which is most likely between SN ejecta and the stripped envelop of the companion star. We obtained a stripped mass of ≤0.0083Mʘ,which is consistent with that observed for two extragalactic Ia SNe (Leonard 2007) and close to ...
... between the ejecta and a bulk of materials in the interior of the remnant, which is most likely between SN ejecta and the stripped envelop of the companion star. We obtained a stripped mass of ≤0.0083Mʘ,which is consistent with that observed for two extragalactic Ia SNe (Leonard 2007) and close to ...
X-ray studies of star and planet formation Eric Feigelson
... Near- and mid-infrared surveys can readily detect photospheres of the full IMF, including proto-brown dwarfs, out to 1-2 kpc. But, except in the closest star forming regions (e.g. Taurus, Orion), the fields are very badly (factors ~ few-100) contaminated by Galactic field stars. Chandra is typically ...
... Near- and mid-infrared surveys can readily detect photospheres of the full IMF, including proto-brown dwarfs, out to 1-2 kpc. But, except in the closest star forming regions (e.g. Taurus, Orion), the fields are very badly (factors ~ few-100) contaminated by Galactic field stars. Chandra is typically ...
Active X-ray Optics - High Energy Astrophysics Division
... physical limits: the Chandra mirror would have been diffraction limited at ∼20 milli-arcsec (van Speybroeck 2000, private communication), while the thermal line widths of 1 keV temperature plasmas are of order 100 km s−1 , so the ’thermal limit’ to X-ray spectroscopy is λ/∆λ ∼6000 (Elvis 2001). More ...
... physical limits: the Chandra mirror would have been diffraction limited at ∼20 milli-arcsec (van Speybroeck 2000, private communication), while the thermal line widths of 1 keV temperature plasmas are of order 100 km s−1 , so the ’thermal limit’ to X-ray spectroscopy is λ/∆λ ∼6000 (Elvis 2001). More ...
Non-thermal hard X-ray emission from stellar coronae
... yield spectral fits of similar quality Simbol-X Workshop, Bologna, May 2007 ...
... yield spectral fits of similar quality Simbol-X Workshop, Bologna, May 2007 ...
Credit: X-ray: NASA/CXC/UMass/D. Wang et al.; Optical: Caltech/SSC/S.Stolovy
... Total X-ray flux distribution: use full 3 Ms X-ray light curve (300s bins, 10,000 data points; Neilsen+ 14b) A different perspective: move beyond distinct flares, think about quiescent and variable processes Similar work in NIR (Dodds-Eden+ ‘11; Witzel+ ’12) ...
... Total X-ray flux distribution: use full 3 Ms X-ray light curve (300s bins, 10,000 data points; Neilsen+ 14b) A different perspective: move beyond distinct flares, think about quiescent and variable processes Similar work in NIR (Dodds-Eden+ ‘11; Witzel+ ’12) ...
Chandra, Spitzer & VLA Observations of Young Clusters Scott Wolk - CxC/CfA
... The X-Ray data indicate a distance of ~600pc. Using two independent methods we find a total cluster size of about 300 stars. There appear to be 9 transition disks - 5 seen in X-rays. ...
... The X-Ray data indicate a distance of ~600pc. Using two independent methods we find a total cluster size of about 300 stars. There appear to be 9 transition disks - 5 seen in X-rays. ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... Although there’s not good reason to think that these young O stars have convection or magnetic dynamos, they may have magnetic fields that remain from the the collapsing interstellar clouds out of which they formed In fact, q1 Ori C itself has recently had a magnetic field detected on it: A large s ...
... Although there’s not good reason to think that these young O stars have convection or magnetic dynamos, they may have magnetic fields that remain from the the collapsing interstellar clouds out of which they formed In fact, q1 Ori C itself has recently had a magnetic field detected on it: A large s ...
Spectral-Type Trends: Absorption
... stellar luminosity or surface temperature. So, an X-ray emission trend would be very surprising. But stellar winds are stronger and denser for hotter and more luminous stars, so an X-ray hardness trend governed by wind attenuation is expected.) To explore the effect of wind absorption, we have devel ...
... stellar luminosity or surface temperature. So, an X-ray emission trend would be very surprising. But stellar winds are stronger and denser for hotter and more luminous stars, so an X-ray hardness trend governed by wind attenuation is expected.) To explore the effect of wind absorption, we have devel ...
New INTEGRAL High Mass X
... cutoffpl : ph. index = 1.6 Ec = 60 keV 3 gaussians at 6.4 keV, 7.099 keV and 7.45 keV ...
... cutoffpl : ph. index = 1.6 Ec = 60 keV 3 gaussians at 6.4 keV, 7.099 keV and 7.45 keV ...
An Analysis of the Behavior of Vela X-1
... – Occurs suddenly without a transition phase (almost like a switch) – Not an eclipse but count rate drops to below detection limits, almost 0. ...
... – Occurs suddenly without a transition phase (almost like a switch) – Not an eclipse but count rate drops to below detection limits, almost 0. ...
Sharp Images of Galaxy Groups: Chandra and XMM Uncover New
... cavity) is ~few x 1056 erg • Current radio source is far too weak to produce cavities in required time. But a very modest AGN (1041 - 1042 erg s-1) would suffice. • Cavities are seen in ~20% of clusters. Is the same true for groups? ...
... cavity) is ~few x 1056 erg • Current radio source is far too weak to produce cavities in required time. But a very modest AGN (1041 - 1042 erg s-1) would suffice. • Cavities are seen in ~20% of clusters. Is the same true for groups? ...
ChESS: ChaMP Extended Stellar Survey
... We have systemati ally sear hed for opti al mat hes to X-ray sour es from the Chandra Multi-wavelength Proje t (ChaMP; Green et al. 2004) using the Ty ho, GSC, SDSS, and ChaMP opti al follow-up atalogs. We nd over 200 stellar X-ray sour es overing a magnitude range V = 10 19. This forms an X-ray ...
... We have systemati ally sear hed for opti al mat hes to X-ray sour es from the Chandra Multi-wavelength Proje t (ChaMP; Green et al. 2004) using the Ty ho, GSC, SDSS, and ChaMP opti al follow-up atalogs. We nd over 200 stellar X-ray sour es overing a magnitude range V = 10 19. This forms an X-ray ...
Soft X-Ray Polarimetry
... The author has been working on soft X-ray polarimetry concepts using multilayer-coated optics for over 15 years, starting with a very simple design 18 emulating an experiment performed using the Extreme Ultraviolet Explorer 23 . Several missions have been proposed to NASA programs based on this appr ...
... The author has been working on soft X-ray polarimetry concepts using multilayer-coated optics for over 15 years, starting with a very simple design 18 emulating an experiment performed using the Extreme Ultraviolet Explorer 23 . Several missions have been proposed to NASA programs based on this appr ...
Activity: Multiwavelength Bingo - Chandra X
... Activity: Multiwavelength Bingo background: Almost everything that we know about distant objects in the Universe comes from studying the light that is emitted or reflected by them. The entire range of energies of light is called the electromagnetic spectrum. Our eyes are sensitive only to a narrow b ...
... Activity: Multiwavelength Bingo background: Almost everything that we know about distant objects in the Universe comes from studying the light that is emitted or reflected by them. The entire range of energies of light is called the electromagnetic spectrum. Our eyes are sensitive only to a narrow b ...
SSS in young stellar populations: progenitors of the
... (Kahabka et al. 2006): B0-3e star, duty cycle unknown – Suzaku J0105-72 in SMC (Takei et al. 2008, this conference): B0 star? similar duty cycle, optical ID less certain ...
... (Kahabka et al. 2006): B0-3e star, duty cycle unknown – Suzaku J0105-72 in SMC (Takei et al. 2008, this conference): B0 star? similar duty cycle, optical ID less certain ...
High energy universe – Satellite missions
... an effective collecting area of 8000 cm 2 and an energy resolution of 10%. Its field of view is two steradians with an ability to locate a source within 1–5 arc minutes. It works at a time resolution of 10 microseconds. Its operating modes are all sky survey as well as the pointed mode with a capaci ...
... an effective collecting area of 8000 cm 2 and an energy resolution of 10%. Its field of view is two steradians with an ability to locate a source within 1–5 arc minutes. It works at a time resolution of 10 microseconds. Its operating modes are all sky survey as well as the pointed mode with a capaci ...
Advanced information on the Nobel Prize in Physics 2002, 8 October
... the detector must be elevated to such an altitude that only about one millionth of the column mass of the atmosphere remains between the detector and the source. This requires a rocket flight to at least 80 km above the ground. X-rays at higher energies penetrate further down into the atmosphere, e. ...
... the detector must be elevated to such an altitude that only about one millionth of the column mass of the atmosphere remains between the detector and the source. This requires a rocket flight to at least 80 km above the ground. X-rays at higher energies penetrate further down into the atmosphere, e. ...
Chandra - Cosmos
... M33 SNRs: More to come • Strong emission lines suggest it is O-rich (J. Hughes et al., in prep) • We are detecting the ejecta directly! • Very young; a gem for studying heavy element creation and distribution. ...
... M33 SNRs: More to come • Strong emission lines suggest it is O-rich (J. Hughes et al., in prep) • We are detecting the ejecta directly! • Very young; a gem for studying heavy element creation and distribution. ...
404.06 Stephen Drake
... useful: suspect this star must have frequent smaller flares • New study of optical photometry: what is the cause of the periodic variation and what is the ‘true’ period? • Magnetic field measurement would be very desirable • Is the (wide) binarity of this system a factor in flare properties? ...
... useful: suspect this star must have frequent smaller flares • New study of optical photometry: what is the cause of the periodic variation and what is the ‘true’ period? • Magnetic field measurement would be very desirable • Is the (wide) binarity of this system a factor in flare properties? ...
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.