Paper 3 (pdf)
... The effective area estimate can be used to predict the minimum detectable polarization5 (MDP) for potential targets. Extragalactic sources such as the BL Lac object PKS 2155−304 are expected to be highly polarized in the soft X-ray band. In a 10,000 s observation of PKS 2155−304, this instrument cou ...
... The effective area estimate can be used to predict the minimum detectable polarization5 (MDP) for potential targets. Extragalactic sources such as the BL Lac object PKS 2155−304 are expected to be highly polarized in the soft X-ray band. In a 10,000 s observation of PKS 2155−304, this instrument cou ...
Background Science - Faulkes Telescope Project
... surface, until it becomes unstable. The enormous explosion from these stars ejects material into the surroundings at very high velocities, sweeping up the surrounding gas into a shell or a giant bubble. This is known as a supernova remnant. The ejected material and the swept-up compressed gas are ve ...
... surface, until it becomes unstable. The enormous explosion from these stars ejects material into the surroundings at very high velocities, sweeping up the surrounding gas into a shell or a giant bubble. This is known as a supernova remnant. The ejected material and the swept-up compressed gas are ve ...
stars
... • J. C. Brown, Dept. of Physics and Astronomy, University of Glasgow, UK • J. P. Cassinelli, Dept of Astronomy, University of Wisconsin-Madison, USA ...
... • J. C. Brown, Dept. of Physics and Astronomy, University of Glasgow, UK • J. P. Cassinelli, Dept of Astronomy, University of Wisconsin-Madison, USA ...
Black Holes, Part 9, Star Eaters
... the UV band, into the hard-x-rays band. The extreme energy emission takes the resulting spectrum far outside the visible band. ...
... the UV band, into the hard-x-rays band. The extreme energy emission takes the resulting spectrum far outside the visible band. ...
Sharp Images of Galaxy Groups: Chandra and XMM Uncover New
... • Detection only at 1.4 GHz in SW “tail”: 1.2±0.4 mJy • Where detected, the equipartition magnetic field pressure is a factor of a few less than the thermal pressure, but could be increased by adjustments in filling factor, presence of relativistic protons… ...
... • Detection only at 1.4 GHz in SW “tail”: 1.2±0.4 mJy • Where detected, the equipartition magnetic field pressure is a factor of a few less than the thermal pressure, but could be increased by adjustments in filling factor, presence of relativistic protons… ...
Living alongside Monsters: Matter around Central Massive Black Holes Q. Daniel Wang
... • The 1.9µm filter is sensitive to the stellar continuum emission. • The 1.87µm filter covers the Pα line. • Subtracting the 1.9µm map from the 1.87µm map adaptively. A net Pα line emission map (see the poster by Dong et al.; 415.01) . ...
... • The 1.9µm filter is sensitive to the stellar continuum emission. • The 1.87µm filter covers the Pα line. • Subtracting the 1.9µm map from the 1.87µm map adaptively. A net Pα line emission map (see the poster by Dong et al.; 415.01) . ...
Chandra`s X-ray vision seeks out black holes
... found in our galaxy. Although a few of the objects had previously been recorded, this is the first time they have been detected in such large numbers. This may help to explain their relationship to star formation and the production of even more massive black holes. Kimberly Weaver, of NASA’s Goddard ...
... found in our galaxy. Although a few of the objects had previously been recorded, this is the first time they have been detected in such large numbers. This may help to explain their relationship to star formation and the production of even more massive black holes. Kimberly Weaver, of NASA’s Goddard ...
Deep $ I $-band imaging of $ z=\ mathsf {5.99} $ quasar
... & Krawczynski 2002). The highest redshift quasars are among the earliest objects in the Universe. The X-ray emission produced close to the central black hole is related intimately to the processes in the central engine and therefore offers the possibility to probe directly the processes occurring in ...
... & Krawczynski 2002). The highest redshift quasars are among the earliest objects in the Universe. The X-ray emission produced close to the central black hole is related intimately to the processes in the central engine and therefore offers the possibility to probe directly the processes occurring in ...
Disks around low-mass stars in extreme environments
... Problem of many injection scenarios: In most clusters (e.g., Orion Nebula Cluster), all stars formed at ~ the same time. When the first supernova happens (after > 4 Myr), most low-mass stars have already largely dispersed their disks (i.e. planetesimal formation is already finished). ...
... Problem of many injection scenarios: In most clusters (e.g., Orion Nebula Cluster), all stars formed at ~ the same time. When the first supernova happens (after > 4 Myr), most low-mass stars have already largely dispersed their disks (i.e. planetesimal formation is already finished). ...
Low-Res Version - Chandra X
... as radio, infra-red, ultra-violet and gamma, cannot be seen with the human eye, and thus do not have any "color". To see the invisible wavelengths, we need detectors that are especially designed to see those other wavelengths, such as the instruments on Chandra. Sometimes images taken by telescopes ...
... as radio, infra-red, ultra-violet and gamma, cannot be seen with the human eye, and thus do not have any "color". To see the invisible wavelengths, we need detectors that are especially designed to see those other wavelengths, such as the instruments on Chandra. Sometimes images taken by telescopes ...
Millisecond Pulsar Binaries at Transition
... There should be more out there, but not identified Indeed, there is a group so-called Very Faint X-ray Binaries (VFXBs; e.g., Heinke et al. 2014), with quiescenct Lx~10^33 erg/s The point is these VFXBs could be considered as the transitional systems too if the neutron stars do not accrete and thus ...
... There should be more out there, but not identified Indeed, there is a group so-called Very Faint X-ray Binaries (VFXBs; e.g., Heinke et al. 2014), with quiescenct Lx~10^33 erg/s The point is these VFXBs could be considered as the transitional systems too if the neutron stars do not accrete and thus ...
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) ...
Analysis of Two Pulsating X-ray Sources
... A “hot spot” on a white dwarf can occur if a white dwarf with a magnetic field accretes matter from the companion star, and the accretion Illustration of an Accretion Powered Pulsar disk is disrupted at small radii by the white dwarf’s magnetosphere. Material would then travel along the magnetic fie ...
... A “hot spot” on a white dwarf can occur if a white dwarf with a magnetic field accretes matter from the companion star, and the accretion Illustration of an Accretion Powered Pulsar disk is disrupted at small radii by the white dwarf’s magnetosphere. Material would then travel along the magnetic fie ...
Non-thermal hard X-ray emission from stellar coronae
... radiation, winds, and energetic particles originating from the central star ⇒ heating, ionization, evaporation How is planetary formation affected? ...
... radiation, winds, and energetic particles originating from the central star ⇒ heating, ionization, evaporation How is planetary formation affected? ...
$doc.title
... the globular luster, hen e allowing short lifetime systems to exist today. In both the Milky Way and ellipti al galaxies, GCs are known to have 100 times as many bright LMXBs per unit mass as the eld. In fa t, theoreti al models have some diÆ ulties produ ing LMXBs outside globular lusters. The ...
... the globular luster, hen e allowing short lifetime systems to exist today. In both the Milky Way and ellipti al galaxies, GCs are known to have 100 times as many bright LMXBs per unit mass as the eld. In fa t, theoreti al models have some diÆ ulties produ ing LMXBs outside globular lusters. The ...
Read the article
... smaller spiral (light months), seem to exist in the galactic center. Among the O/B stars moving close to SgrA* only S2 has been seen to complete two-third of its Keplerian orbit around SgrA* (Schödel et al. 2002). The Keplerian orbits of the other stars are more a matter of guess. Apart from S2, th ...
... smaller spiral (light months), seem to exist in the galactic center. Among the O/B stars moving close to SgrA* only S2 has been seen to complete two-third of its Keplerian orbit around SgrA* (Schödel et al. 2002). The Keplerian orbits of the other stars are more a matter of guess. Apart from S2, th ...
Article PDF - IOPscience
... Of the 71 transient X-ray binaries containing neutron stars or black holes listed in a 1992 catalog of high- and low-mass X-ray binaries (van Paradijs 1995), three are in the Small Magellanic Cloud (SMC) and two are in the Large Magellanic Cloud (LMC), of which one is a 69 ms pulsar. The optical com ...
... Of the 71 transient X-ray binaries containing neutron stars or black holes listed in a 1992 catalog of high- and low-mass X-ray binaries (van Paradijs 1995), three are in the Small Magellanic Cloud (SMC) and two are in the Large Magellanic Cloud (LMC), of which one is a 69 ms pulsar. The optical com ...
Chandra - Cosmos
... • Large fraction of Galactic LMXBs that exhibit bright (>1037 erg/s) transient outbursts have been shown to contain black holes (McClintock & Remillard 2004). • There are only ~20 such objects in the Galaxy, and each is vital for studies of accretion physics in the strong gravity regime. Finding mor ...
... • Large fraction of Galactic LMXBs that exhibit bright (>1037 erg/s) transient outbursts have been shown to contain black holes (McClintock & Remillard 2004). • There are only ~20 such objects in the Galaxy, and each is vital for studies of accretion physics in the strong gravity regime. Finding mor ...
Slides from Dr. Frank`s Lecture17
... 1) The binary separation decreases because of gravitational radiation and other angular momentum losses. 2) The component stars will evolve and change size (for example becoming a red giant) Conclusion: Long period (wide) binaries may never become interacting while short period (close) binaries are ...
... 1) The binary separation decreases because of gravitational radiation and other angular momentum losses. 2) The component stars will evolve and change size (for example becoming a red giant) Conclusion: Long period (wide) binaries may never become interacting while short period (close) binaries are ...
Document
... INTRODUCTIONu The hot, diffuse, x-ray emitting interstellar medium of the Milky Way Galaxy appears almost featureless, unless it is observed in the soft x-ray band. In 1995, complex structures, visible only between 0.1 and 2.0keV, were revealed by the ROSAT all-sky survey. The XMM-Newton observatory ...
... INTRODUCTIONu The hot, diffuse, x-ray emitting interstellar medium of the Milky Way Galaxy appears almost featureless, unless it is observed in the soft x-ray band. In 1995, complex structures, visible only between 0.1 and 2.0keV, were revealed by the ROSAT all-sky survey. The XMM-Newton observatory ...
Chandra Emission Line Diagnostics of Sco
... been discovered that hot stars are strong x-ray sources. New models are being created to explain these data. Our sun produces x-rays through a magnetic dynamo created by the interaction of convection and rotation. It was theorized that hot stars did not have this convective envelope. However, some r ...
... been discovered that hot stars are strong x-ray sources. New models are being created to explain these data. Our sun produces x-rays through a magnetic dynamo created by the interaction of convection and rotation. It was theorized that hot stars did not have this convective envelope. However, some r ...
Projet d`observation
... energy due to Thomson scattering by a factor exp(- Neστ)” (στ: Thomson cross-section) ...
... energy due to Thomson scattering by a factor exp(- Neστ)” (στ: Thomson cross-section) ...
rastieee
... Many interesting astrophysical objects such as black holes, neutron stars, clusters of galaxies, gamma-ray bursts are intense X-ray emitters. The high energy emission from such exotic objects are often transient that may last from a few seconds to months depending on the nature of the object. Since ...
... Many interesting astrophysical objects such as black holes, neutron stars, clusters of galaxies, gamma-ray bursts are intense X-ray emitters. The high energy emission from such exotic objects are often transient that may last from a few seconds to months depending on the nature of the object. Since ...
HE and VHE emission from X-ray binaries
... Since these sources are located in the Galactic plane, a sensitivity better by a factor X with respect to current instruments means detecting ~3X sources. • Binaries with short orbital periods, difficult for Be but likely for O donors, should be ‘on’ all the time, although strong variability due to ...
... Since these sources are located in the Galactic plane, a sensitivity better by a factor X with respect to current instruments means detecting ~3X sources. • Binaries with short orbital periods, difficult for Be but likely for O donors, should be ‘on’ all the time, although strong variability due to ...
404.06 Stephen Drake
... You can use `all-sky monitor’ X-ray observations, e.g., Swift BAT, MAXI, etc., => given present sensitivity levels ~10-9 erg cm-2 s-1, only the largest flares will be found: e.g., Swift detections of stellar flares from the active binary systems Algol, II Peg & HR 1099 and the M4.5V star EV Lac an ...
... You can use `all-sky monitor’ X-ray observations, e.g., Swift BAT, MAXI, etc., => given present sensitivity levels ~10-9 erg cm-2 s-1, only the largest flares will be found: e.g., Swift detections of stellar flares from the active binary systems Algol, II Peg & HR 1099 and the M4.5V star EV Lac an ...
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical 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 the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation.X-ray emission is expected from astronomical objects that contain extremely hot gasses at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). Although X-rays have been observed emanating from the Sun since the 1940s, the discovery in 1962 of the first cosmic X-ray source was a surprise. This source is called Scorpius X-1 (Sco X-1), the first X-ray source found in the constellation Scorpius. The X-ray emission of Scorpius X-1 is 10,000 times greater than its visual emission, whereas that of the Sun is about a million times less. In addition, the energy output in X-rays is 100,000 times greater than the total emission of the Sun in all wavelengths. Based on discoveries in this new field of X-ray astronomy, starting with Scorpius X-1, Riccardo Giacconi received the Nobel Prize in Physics in 2002. It is now known that such X-ray sources as Sco X-1 are compact stars, such as neutron stars or black holes. Material falling into a black hole may emit X-rays, but the black hole itself does not. The energy source for the X-ray emission is gravity. Infalling gas and dust is heated by the strong gravitational fields of these and other celestial objects.Many thousands of X-ray sources are known. In addition, the space between galaxies in galaxy clusters is filled with a very hot, but very dilute gas at a temperature between 10 and 100 megakelvins (MK). The total amount of hot gas is five to ten times the total mass in the visible galaxies.