Normal Stars - Chandra X
... distinct impression of a twisted sheet of gas in the process of unwinding itself. The photograph was taken by the extreme ultraviolet spectroheliograph instrument of the U.S. Naval Research Laboratory.) If solar flares were more powerful or frequent the climate could be severely affected, as would t ...
... distinct impression of a twisted sheet of gas in the process of unwinding itself. The photograph was taken by the extreme ultraviolet spectroheliograph instrument of the U.S. Naval Research Laboratory.) If solar flares were more powerful or frequent the climate could be severely affected, as would t ...
Physics 127 Descriptive Astronomy Homework #3 Key (Chapter 2
... 2-4. If you double the Kelvin temperature of a hot piece of steel, how much more energy will it radiate per second? The Stefan-Boltzmann Equation (p.43) tells us that the energy radiated per second from a black body is proportion to its temperature in Kelvins raised to the fourth power. We expect ou ...
... 2-4. If you double the Kelvin temperature of a hot piece of steel, how much more energy will it radiate per second? The Stefan-Boltzmann Equation (p.43) tells us that the energy radiated per second from a black body is proportion to its temperature in Kelvins raised to the fourth power. We expect ou ...
Alfven wave
... vs = (gP/r)½ = (gkT/mmH)½ Where P, T and r are pressure, temperature and density and g is the ratio of specific heats for the gas ...
... vs = (gP/r)½ = (gkT/mmH)½ Where P, T and r are pressure, temperature and density and g is the ratio of specific heats for the gas ...
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 ...
Document
... • Spectroscopy is far more powerful than imaging “A spectrum is worth a thousand pictures” • Every element or object in the Universe has unique spectral signature (like DNA) • Radiation absorption and emission highly efficient at resonant energies corresponding to atomic transitions in heavy element ...
... • Spectroscopy is far more powerful than imaging “A spectrum is worth a thousand pictures” • Every element or object in the Universe has unique spectral signature (like DNA) • Radiation absorption and emission highly efficient at resonant energies corresponding to atomic transitions in heavy element ...
Presentazione di PowerPoint
... Detailed X-ray Spectral Analysis of faint X-ray sources: Towards an universal distribution of intrinsic absorption (selection effects can be easily modelled in X-rays) >~80% of the AGNs agree with simple unification models (TypeI/TypeII ...
... Detailed X-ray Spectral Analysis of faint X-ray sources: Towards an universal distribution of intrinsic absorption (selection effects can be easily modelled in X-rays) >~80% of the AGNs agree with simple unification models (TypeI/TypeII ...
Multiwavelength Imaging of Planetary Nebulae: Resolving Disentangling PN Structure
... 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 astrophysical systems such as wind-blown bubbles. In this dissertation we present the results of an X-ray study of PNe, a ...
... 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 astrophysical systems such as wind-blown bubbles. In this dissertation we present the results of an X-ray study of PNe, a ...
The ultra-luminous x-ray sources near center of M82
... X-ray sources at central region of M82 X-ray sources and star clusters correlation Lightcurves of target transient source ...
... X-ray sources at central region of M82 X-ray sources and star clusters correlation Lightcurves of target transient source ...
X-ray Observations of Cosmic Accelerators Greg Madejski SLAC/KIPAC
... - from the progenitor + those already present in the ambient medium - can be studied via narrow-band imaging corresponding to energies of atomic transitions for specific elements ...
... - from the progenitor + those already present in the ambient medium - can be studied via narrow-band imaging corresponding to energies of atomic transitions for specific elements ...
The Galactic Super Star Cluster Westerlund 1
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
High Energy Astrophysics and Transient Science (or, a tale of radio
... luminosities greater than 1036 erg/s and are at large (kpc) distances ...
... luminosities greater than 1036 erg/s and are at large (kpc) distances ...
NGC 5746 :: NGC 5746 Handout - Chandra X
... Caption: Chandra's observation of the hot halo (blue) surrounding the optical disk (white) of NGC 5746 should help astronomers better understand how galaxies form. Spiral galaxies are thought to form from enormous clouds of intergalactic gas that collapse to form spinning disks of stars and gas. The ...
... Caption: Chandra's observation of the hot halo (blue) surrounding the optical disk (white) of NGC 5746 should help astronomers better understand how galaxies form. Spiral galaxies are thought to form from enormous clouds of intergalactic gas that collapse to form spinning disks of stars and gas. The ...
PowerPoint - Chandra X
... In Stephan’s Quintet collisions of the galaxies with each other and with the hot gas are stripping cool gas from spiral galaxies and transforming them into elliptical galaxies. Reference: G. Trinchieri et al. 2003 Astron. & Astrophys. (in ...
... In Stephan’s Quintet collisions of the galaxies with each other and with the hot gas are stripping cool gas from spiral galaxies and transforming them into elliptical galaxies. Reference: G. Trinchieri et al. 2003 Astron. & Astrophys. (in ...
Polarimeter - Raman Research Institute
... mission of the Indian Space Research Organisation (ISRO). A laboratory model was made and tested successfully and it was redesigned for a flight unit. Fabrication of an engineering model is in final stages. The instrument consists of position sensitive proportional counter detectors and works in the ...
... mission of the Indian Space Research Organisation (ISRO). A laboratory model was made and tested successfully and it was redesigned for a flight unit. Fabrication of an engineering model is in final stages. The instrument consists of position sensitive proportional counter detectors and works in the ...
Feigelson, E. (PSU)
... z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-15 keV) X-rays should penetrate 1-100 g/cm2. Igea & Glassgold 1997 & 1999; Fromang et al. 2002; Matsumura & Pudritz 2003 & 2006; Alexander et al. 2004; Salmeron & Wardle 2005; I ...
... z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-15 keV) X-rays should penetrate 1-100 g/cm2. Igea & Glassgold 1997 & 1999; Fromang et al. 2002; Matsumura & Pudritz 2003 & 2006; Alexander et al. 2004; Salmeron & Wardle 2005; I ...
Complex Spatio-Spectral Structure of Diffuse X-Ray
... - Hard X-ray light curve increases with a lower rate of ~20% /yr (f ~ t4). As of 2008-1, f (3-10 keV) = 5.2 x 10-13 erg/cm2/s, Lx = 1.6 x 1035 erg/s. - Cross-comparisons among different X-ray instruments are consistent. - Radio emission shows an evolution of the spectral index: currently S ~ -0.8 ...
... - Hard X-ray light curve increases with a lower rate of ~20% /yr (f ~ t4). As of 2008-1, f (3-10 keV) = 5.2 x 10-13 erg/cm2/s, Lx = 1.6 x 1035 erg/s. - Cross-comparisons among different X-ray instruments are consistent. - Radio emission shows an evolution of the spectral index: currently S ~ -0.8 ...
ppt
... • Every output class needs substantial representation in the training set. • Overlap between classes should be minimized. • Classifier accuracy can be improved with additional information (i.e., flux in different bandpass), but not always! ...
... • Every output class needs substantial representation in the training set. • Overlap between classes should be minimized. • Classifier accuracy can be improved with additional information (i.e., flux in different bandpass), but not always! ...
The Big Four:
... • Effects on matter/light outside the horizon – gravitational attraction of other bodies – “dark star” with mass 3M Sun • distinguish from normal star, white dwarf, neutron star ...
... • Effects on matter/light outside the horizon – gravitational attraction of other bodies – “dark star” with mass 3M Sun • distinguish from normal star, white dwarf, neutron star ...
Solar-B - to Nobeyama Radio Observatory
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
... Largest optical telescope ever to observe the Sun from space Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm Vector magnetic field measurement at the photosphere • X-Ray Telescope (XRT) Highest angular resolution imaging at > 3 MK corona Wide temperature coverage from below 1 MK to ab ...
Black Holes in M83 - Astronomical Society of the Pacific
... • Similar ultra-luminous X-ray sources (ULXs), presumed to be X-ray emitting black holes, found in other galaxies also show blue counterparts in optical images. • Astronomers usually attribute the blue light to a young, massive, blue companion star in orbit around the black hole. Material from the b ...
... • Similar ultra-luminous X-ray sources (ULXs), presumed to be X-ray emitting black holes, found in other galaxies also show blue counterparts in optical images. • Astronomers usually attribute the blue light to a young, massive, blue companion star in orbit around the black hole. Material from the b ...
9. Fascinating observations. But how much is well understood?
... After all these details and strange features found under the extreme conditions of NSs I am afraid you will feel a bit confused. I am sorry! All these many faces belong to this same object that we call neutron star. I use here the singular deliberately since it is now believed that there exists only ...
... After all these details and strange features found under the extreme conditions of NSs I am afraid you will feel a bit confused. I am sorry! All these many faces belong to this same object that we call neutron star. I use here the singular deliberately since it is now believed that there exists only ...
Folie 1
... Lobster (LU, UK), wide field X-ray monitor ART (IKI, Russia), X-ray concentrator based on Kumakhov optics or coded-mask X-ray telescopes as a fallback GRB (IKI, Russia), gamma ray burst detector ...
... Lobster (LU, UK), wide field X-ray monitor ART (IKI, Russia), X-ray concentrator based on Kumakhov optics or coded-mask X-ray telescopes as a fallback GRB (IKI, Russia), gamma ray burst detector ...
Dublin - University of Warwick
... Signatures of merging BHs (disruption rates 1 per decade) Possible accelerators of ultra-high energy cosmic rays ...
... Signatures of merging BHs (disruption rates 1 per decade) Possible accelerators of ultra-high energy cosmic rays ...
Discovering X-ray Bright Neutron Stars for Current and Next-Generation
... • A new, X-ray bright neutron star • The hottest INS known • As an INS: High in the Galactic halo and too hot for its age • As an X-ray bright MSP: Possibly closer than RXS J1856 • Possibly the closest neutron star to Earth – good for LIGO • Not detected as radio pulsar (Hessels+07, A&A, ...
... • A new, X-ray bright neutron star • The hottest INS known • As an INS: High in the Galactic halo and too hot for its age • As an X-ray bright MSP: Possibly closer than RXS J1856 • Possibly the closest neutron star to Earth – good for LIGO • Not detected as radio pulsar (Hessels+07, A&A, ...
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.