![TDE in the XMM-Newton slew survey](http://s1.studyres.com/store/data/011974082_1-15e603d1ead2cfdc16c31b9bad4772dc-300x300.png)
TDE in the XMM-Newton slew survey
... Arcavi et al. 2014; French et al. 2016 - E+A galaxies disproportionately represented in optical TDE samples ...
... Arcavi et al. 2014; French et al. 2016 - E+A galaxies disproportionately represented in optical TDE samples ...
Determining the Effect of Diffuse X-ray Emission on Point Source Detection
... Dr. Frederick Baganoff MIT Center for Space Research ...
... Dr. Frederick Baganoff MIT Center for Space Research ...
in the milky way - Chandra X
... show an artist’s representation of what it looks like from the outside. From our vantage point, we only have an edge-on view of the Milky Way, but this is still very useful. Different types of astronomical observations—some that trace the spiral arms, others that detect stars or gas and dust—can be ...
... show an artist’s representation of what it looks like from the outside. From our vantage point, we only have an edge-on view of the Milky Way, but this is still very useful. Different types of astronomical observations—some that trace the spiral arms, others that detect stars or gas and dust—can be ...
Measuring the Masses of Neutron Stars
... the envelope of the Be companion, and after the (second) supernova a bound (or disrupted) double neutron star remains, like the Hulse-Taylor binary pulsar PSR 1913+16 (or a neutron star – white dwarf system, if the mass of the Be companion is less than 8 M A). In HMXBs with an orbital period less th ...
... the envelope of the Be companion, and after the (second) supernova a bound (or disrupted) double neutron star remains, like the Hulse-Taylor binary pulsar PSR 1913+16 (or a neutron star – white dwarf system, if the mass of the Be companion is less than 8 M A). In HMXBs with an orbital period less th ...
AMUSE-Virgo on the survival of super
... AMUSE-Virgo: latest results 26/100 nuclear super-massive Point-like nuclearX-ray X-raysources source likley detected in 32p/100 black objectsholes ...
... AMUSE-Virgo: latest results 26/100 nuclear super-massive Point-like nuclearX-ray X-raysources source likley detected in 32p/100 black objectsholes ...
X-ray Binaries in Nearby Galaxies
... long-standing problem with distance estimates: very hard to study the X-ray luminosity function and spatial distribution other properties, e.g., orbital period, donor masses known only for a few systems ...
... long-standing problem with distance estimates: very hard to study the X-ray luminosity function and spatial distribution other properties, e.g., orbital period, donor masses known only for a few systems ...
First generation stars
... Galaxies Speaker: Michael Loewenstein Institute: Astrophysics Science Division, NASA/Goddard Space Flight Center, USA Time: 4:00 pm, 27 May 2010,ThursdayVenue: seminar room, KIAA, Peking University ...
... Galaxies Speaker: Michael Loewenstein Institute: Astrophysics Science Division, NASA/Goddard Space Flight Center, USA Time: 4:00 pm, 27 May 2010,ThursdayVenue: seminar room, KIAA, Peking University ...
The nature of the ultraluminous X-ray sources inside galaxies and
... These are only some of the many cases which have now been found which provide strong circumstantial evidence that QSOs originate in the centers of active galaxies and are ejected from them. Evidence based on a sample of 39 X-ray emitting QSOs associated with active galaxies, including some of the ca ...
... These are only some of the many cases which have now been found which provide strong circumstantial evidence that QSOs originate in the centers of active galaxies and are ejected from them. Evidence based on a sample of 39 X-ray emitting QSOs associated with active galaxies, including some of the ca ...
Acta Polytechnica
... 3. Sample and the Suzaku data The 5th Japanese satellite, Suzaku [23], is equipped with X-ray CCD imaging spectrometers (XIS; [20]) and HXD [33] and enables sensitive broad-band X-ray observations thanks to the low and stable background levels. In particular, the PIN detectors of the HXD instrument ...
... 3. Sample and the Suzaku data The 5th Japanese satellite, Suzaku [23], is equipped with X-ray CCD imaging spectrometers (XIS; [20]) and HXD [33] and enables sensitive broad-band X-ray observations thanks to the low and stable background levels. In particular, the PIN detectors of the HXD instrument ...
Living alongside Monsters: Matter around Central Massive Black Holes Q. Daniel Wang
... isolation and with strong winds. – Fine filamentary structures of ionized diffuse gas indicating profound influence of local strong magnetic field. – Compact nebulae, tracing various stages of massive ...
... isolation and with strong winds. – Fine filamentary structures of ionized diffuse gas indicating profound influence of local strong magnetic field. – Compact nebulae, tracing various stages of massive ...
A search for ultra-high-energy gamma rays at the South Pole
... Detection of high-energy cosmic and gamma rays is rather complicated. Because of the very low flux above 100 terraelectronvolts (approximately 1 per square meter per year), a very large area detector is required, and one must make use of the fact that both the cosmic and gamma rays generate cascades ...
... Detection of high-energy cosmic and gamma rays is rather complicated. Because of the very low flux above 100 terraelectronvolts (approximately 1 per square meter per year), a very large area detector is required, and one must make use of the fact that both the cosmic and gamma rays generate cascades ...
High Energy Phenomena in Supergiant X-ray Binaries - HAL-Insu
... rapid outbursts lasting only for hours, faint quiescent emission, and high energy spectra requiring a BH or NS accretor. The flares rise in tens of minutes, last for ∼ 1 hour, their frequency is ∼ 7 days, and their luminosity L x ∼ 1036 erg s−1 at the outburst peak. IGR J17544-2619, archetype of SFX ...
... rapid outbursts lasting only for hours, faint quiescent emission, and high energy spectra requiring a BH or NS accretor. The flares rise in tens of minutes, last for ∼ 1 hour, their frequency is ∼ 7 days, and their luminosity L x ∼ 1036 erg s−1 at the outburst peak. IGR J17544-2619, archetype of SFX ...
Chandra Characterization of X-ray Emission in the Young F
... HD113766B has a similar inclination, it could have an equatorial rotation velocity on the order of 400 km s-1 consistent with the observations. We thus note the possible x-ray periodicity in our HD113766B data for future reference, but also note that we do not understand its source if it is real. It ...
... HD113766B has a similar inclination, it could have an equatorial rotation velocity on the order of 400 km s-1 consistent with the observations. We thus note the possible x-ray periodicity in our HD113766B data for future reference, but also note that we do not understand its source if it is real. It ...
VLT identifications in the Chandra/XMM
... obscuration fraction (ratio of type2/type-1 AGN) from 4:1 in the local universe to much larger covering fractions (10:1) at high redshifts (see also Fabian et al., 1998). The gas to dust ratio in high-redshift, high-luminosity AGN could be completely different from the usually assumed galactic value ...
... obscuration fraction (ratio of type2/type-1 AGN) from 4:1 in the local universe to much larger covering fractions (10:1) at high redshifts (see also Fabian et al., 1998). The gas to dust ratio in high-redshift, high-luminosity AGN could be completely different from the usually assumed galactic value ...
A propelling neutron star in the enigmatic Be-star γ Cassiopeia
... orbital frequency, C 1 is a numerical coefficient which determines turbulent viscosity through the Prandtl law and hence viscous stresses in the convective shell. Plugging into (12) the density distribution in the shell, ρ A = ρ B (RB /RA )3/2 , as given by (8) and expressing it through the X-ray ...
... orbital frequency, C 1 is a numerical coefficient which determines turbulent viscosity through the Prandtl law and hence viscous stresses in the convective shell. Plugging into (12) the density distribution in the shell, ρ A = ρ B (RB /RA )3/2 , as given by (8) and expressing it through the X-ray ...
ppt - MIT Haystack Observatory
... while the radio transients in Bower et al. have been reexamined and the transient rate revised downward significantly (Frail et al. 2012), it is true that the radio probability distribution for radio-active stellar sources has not been investigated. The overlap in parameter space with other types of ...
... while the radio transients in Bower et al. have been reexamined and the transient rate revised downward significantly (Frail et al. 2012), it is true that the radio probability distribution for radio-active stellar sources has not been investigated. The overlap in parameter space with other types of ...
! • Supermassive Black Holes (SMBH) at Work: Effects of
... •Lnuc~2x1042 erg/s •Likely merger driven outburst (e.g., Mackie/ Fabbiano98) •Massive SMBH is willing and able to disrupt atmosphere given sufficient fuel; outburst power ~ 5x1058 ergs (Lanz+10) •Such outbursts at early epochs could disrupt star formation ...
... •Lnuc~2x1042 erg/s •Likely merger driven outburst (e.g., Mackie/ Fabbiano98) •Massive SMBH is willing and able to disrupt atmosphere given sufficient fuel; outburst power ~ 5x1058 ergs (Lanz+10) •Such outbursts at early epochs could disrupt star formation ...
Non-thermal hard X-ray emission from stellar coronae
... dynamics and gravitational settling towards the disk ...
... dynamics and gravitational settling towards the disk ...
Document
... Blazars at very high energies Bazars are powerful gamma-ray sources. The most powerful of them have equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST ...
... Blazars at very high energies Bazars are powerful gamma-ray sources. The most powerful of them have equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST ...
Cygnus X-1
... a very inconsistent source for X-ray emissions. The emissions of X-rays for Cygnus X-1 flicker in hundredth of a second bursts. It is also been proven that Cygnus X-1 is smaller than the Earth. Strangely enough, Cygnus X-1 has a companion star called HDE 226868. HDE 226868 is a supergiant with a tem ...
... a very inconsistent source for X-ray emissions. The emissions of X-rays for Cygnus X-1 flicker in hundredth of a second bursts. It is also been proven that Cygnus X-1 is smaller than the Earth. Strangely enough, Cygnus X-1 has a companion star called HDE 226868. HDE 226868 is a supergiant with a tem ...
Black Holes in Binary Systems and Galaxy Nuclei
... the mass distribution of BHs has been considered by Postnov and Cherepashchuk (2003). Deficit of low-mass BH and the gap in the range (2 – 4) MSun may be due to enhanced quantum evaporation of BH which have been suggested in some multidimensional models of gravity (e.g. Randall and Sundrom, 1999). I ...
... the mass distribution of BHs has been considered by Postnov and Cherepashchuk (2003). Deficit of low-mass BH and the gap in the range (2 – 4) MSun may be due to enhanced quantum evaporation of BH which have been suggested in some multidimensional models of gravity (e.g. Randall and Sundrom, 1999). I ...
Multi-Wavelength Observations of Known, and Searches
... population of pre-High-Mass X-ray Binaries is predicted. ...
... population of pre-High-Mass X-ray Binaries is predicted. ...
The Evolution of Coronal X
... The long mission lives of XMM and Chandra have allowed long term monitoring of a few solar type stars. It seems that larger X-ray variations are present in older stars like the Sun. There are now a couple of examples where the variation appears to approach that seen in the Sun. We can conclude that ...
... The long mission lives of XMM and Chandra have allowed long term monitoring of a few solar type stars. It seems that larger X-ray variations are present in older stars like the Sun. There are now a couple of examples where the variation appears to approach that seen in the Sun. We can conclude that ...
PowerPoint Presentation - Isolated Neutron Stars, solid crust
... Over the last few years, intense observational resources have been devoted to study the faint thermal emission from neutron stars and to search for features in their spectrum. Isolated neutron stars play a key role in compact objects astrophysics: these are the only sources in which we can see direc ...
... Over the last few years, intense observational resources have been devoted to study the faint thermal emission from neutron stars and to search for features in their spectrum. Isolated neutron stars play a key role in compact objects astrophysics: these are the only sources in which we can see direc ...
History of X-ray astronomy
![](https://commons.wikimedia.org/wiki/Special:FilePath/Saturn_comp.jpg?width=300)
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.