Strongly Interacting Supernovae - The National Centre for Radio
... If detected in radio, follow with Swift-XRT (PI: Soderberg). Follow radio bright and/or Swift detected Type IIN supernova with ChandraXO. Get spectroscopy, separate from nearby ...
... If detected in radio, follow with Swift-XRT (PI: Soderberg). Follow radio bright and/or Swift detected Type IIN supernova with ChandraXO. Get spectroscopy, separate from nearby ...
PPT - University of Arizona
... We have written everything as a function of frequency, ν However, you can also integrate these quantities over ν, either ν= 0 or ν over some passband. ...
... We have written everything as a function of frequency, ν However, you can also integrate these quantities over ν, either ν= 0 or ν over some passband. ...
ASTRONOMY 120
... How do molecules produce spectral lines unrelated to the movement of electrons between energy levels? (3 points) Molecules can rotate and they can vibrate. These two motions have quantized energy levels just like the motions of electrons between orbitals. Changes in the rotational or vibrational sta ...
... How do molecules produce spectral lines unrelated to the movement of electrons between energy levels? (3 points) Molecules can rotate and they can vibrate. These two motions have quantized energy levels just like the motions of electrons between orbitals. Changes in the rotational or vibrational sta ...
Electron-positron An.. - SCIPP - University of California, Santa Cruz
... When matter and anti-matter collide, they destroy each other in a flash of high-energy radiation The gamma rays emitted in the annihilation are easily detectable In an electron-positron annihilation the g-rays are emitted linearly Sometimes the electron and positron form a brief bond through the ele ...
... When matter and anti-matter collide, they destroy each other in a flash of high-energy radiation The gamma rays emitted in the annihilation are easily detectable In an electron-positron annihilation the g-rays are emitted linearly Sometimes the electron and positron form a brief bond through the ele ...
Astronomy Learning Objectives and Study Questions for Chapter 3 1
... 6. Explain how adaptive optics is used to improve the "seeing" of many ground-based optical telescopes and how interferometry is used to improve the resolution of radio telescopes. 1. Different colors of light correspond to electromagnetic waves with different _____. A. speeds B. amplitudes C. inten ...
... 6. Explain how adaptive optics is used to improve the "seeing" of many ground-based optical telescopes and how interferometry is used to improve the resolution of radio telescopes. 1. Different colors of light correspond to electromagnetic waves with different _____. A. speeds B. amplitudes C. inten ...
PowerPoint - Chandra X
... Chandra Science Highlight Stephan’s Quintet: A Compact Group of Galaxies about 280 Million Light Years from Earth Chandra X-ray Observatory ACIS Image. ...
... Chandra Science Highlight Stephan’s Quintet: A Compact Group of Galaxies about 280 Million Light Years from Earth Chandra X-ray Observatory ACIS Image. ...
Justin Kiehne: Next Generation X-ray Observatory
... X-ray astrophysics and astronomy require increasingly high resolution optics for the study of the most distant stellar objects. As resolution improves, light weight must be maintained for increasing photon collection area. X-ray observations are made from space so limitations imposed by launch must ...
... X-ray astrophysics and astronomy require increasingly high resolution optics for the study of the most distant stellar objects. As resolution improves, light weight must be maintained for increasing photon collection area. X-ray observations are made from space so limitations imposed by launch must ...
Gravitationally redshifted absorption lines in the x
... for 16 X-ray bursts from GS 1826-24. The three temperature phases are defined according to the spectral fits with the EPIC-pn data. An absorbed blackbody model is superimposed in red. The Ne x line at 12.1 (with 3.4 σ confidence) Å is included in the low-temperature spectrum. ...
... for 16 X-ray bursts from GS 1826-24. The three temperature phases are defined according to the spectral fits with the EPIC-pn data. An absorbed blackbody model is superimposed in red. The Ne x line at 12.1 (with 3.4 σ confidence) Å is included in the low-temperature spectrum. ...
PowerPoint - Chandra X
... With an age of about 200 million years this is the oldest isolated pulsar ever detected in X-rays. Among pulsar that have not been spun-up in a binary system, it is over 10 times older than the previous record holder with an X-ray detection. At a distance of 770 light years, it is one of the nearest ...
... With an age of about 200 million years this is the oldest isolated pulsar ever detected in X-rays. Among pulsar that have not been spun-up in a binary system, it is over 10 times older than the previous record holder with an X-ray detection. At a distance of 770 light years, it is one of the nearest ...
atom and valence electron signals – x-rays – gamma-rays
... analyzed with a spectroscopy system, a gamma-ray energy spectrum can be produced. A detailed analysis of this spectrum is typically used to determine the identity and quantity of gamma emitters present in a gamma source, and is a vital tool in radiometric assay. The gamma spectrum is characteristic ...
... analyzed with a spectroscopy system, a gamma-ray energy spectrum can be produced. A detailed analysis of this spectrum is typically used to determine the identity and quantity of gamma emitters present in a gamma source, and is a vital tool in radiometric assay. The gamma spectrum is characteristic ...
Astronomy Astrophysics + Infrared identification of 2XMM J191043.4
... 0.5 kpc. On the other hand, Brγ is the most prominent feature in Be stars in the K band, while He i 2.058 μm is found in early-type Be stars, up to B2.5 (Clark and Steele 2000). Therefore, assuming a B0V star, the intrinsic colour would be (H − K)0 = −0.05 (Ducati et al. 2001) and E(H−K) = 1.27, als ...
... 0.5 kpc. On the other hand, Brγ is the most prominent feature in Be stars in the K band, while He i 2.058 μm is found in early-type Be stars, up to B2.5 (Clark and Steele 2000). Therefore, assuming a B0V star, the intrinsic colour would be (H − K)0 = −0.05 (Ducati et al. 2001) and E(H−K) = 1.27, als ...
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 ...
PG_Lecture_Dec18_2008
... In the quiet solar corona, and to a 1st approximation in active regions (or maybe even flares), there is ionization equilibrium: Number of ionizations/unit vol. and time = No. of recombinations/unit vol. and time: Ne N(X+m) Q(T) = Ne N(X+m+1) α(T) where Q(T) = rate coefft. of ionization, α(T) = rate ...
... In the quiet solar corona, and to a 1st approximation in active regions (or maybe even flares), there is ionization equilibrium: Number of ionizations/unit vol. and time = No. of recombinations/unit vol. and time: Ne N(X+m) Q(T) = Ne N(X+m+1) α(T) where Q(T) = rate coefft. of ionization, α(T) = rate ...
HOW TO HOLD A DEAD STAR IN YOUR HAND - Chandra X
... blue, wispy arcs in the image show where the acceleration is taking place in an expanding shock wave generated by the explosion. The red and green regions show material from the destroyed star that has been heated to millions of degrees by the explosion. NASA’s Chandra X-ray Observatory has observed ...
... blue, wispy arcs in the image show where the acceleration is taking place in an expanding shock wave generated by the explosion. The red and green regions show material from the destroyed star that has been heated to millions of degrees by the explosion. NASA’s Chandra X-ray Observatory has observed ...
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! ...
ppt - 中央研究院物理所
... a promising new detection channel for neutrinos, without strict lower bound on En & the channel for WIMP direct detection ! involves new energy range at low energy, many experimental challenges & much room to look for scientific surprises ...
... a promising new detection channel for neutrinos, without strict lower bound on En & the channel for WIMP direct detection ! involves new energy range at low energy, many experimental challenges & much room to look for scientific surprises ...
Electromagnetic Spectrum
... resulting from the motion of electric charges and the magnetic fields that they produce. ...
... resulting from the motion of electric charges and the magnetic fields that they produce. ...
View from the space
... appears like a perfect graph paper. Actually, the graph paper appearance is caused by the ends of many tiny square tubes on a spherical surface. The sides of the tubes are very flat and shiny mirrors, and their precise geometrical arrangement means that parallel light rays are all reflected to a foc ...
... appears like a perfect graph paper. Actually, the graph paper appearance is caused by the ends of many tiny square tubes on a spherical surface. The sides of the tubes are very flat and shiny mirrors, and their precise geometrical arrangement means that parallel light rays are all reflected to a foc ...
PowerPoint - Chandra X
... Chandra Science Highlights IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio ...
... Chandra Science Highlights IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio ...
Y.Ueda_Future_HE_Mission2006 - X
... population of Compton thick AGNs in the universe. We have not fully understand the XRB origin yet. The population synthesis model is being almost established below 6-8 keV. However, we have to note that there are a few critical assumptions are made when extrapolating it to above 8 keV. To fully unde ...
... population of Compton thick AGNs in the universe. We have not fully understand the XRB origin yet. The population synthesis model is being almost established below 6-8 keV. However, we have to note that there are a few critical assumptions are made when extrapolating it to above 8 keV. To fully unde ...
Astronomy news
... is also consistent with neutron star models", says Tiengo. More importantly, the discovery of pulsations opens the way for the determination of timing-dependent parameters that are crucial for more detailed modeling of the star’s ...
... is also consistent with neutron star models", says Tiengo. More importantly, the discovery of pulsations opens the way for the determination of timing-dependent parameters that are crucial for more detailed modeling of the star’s ...
Part B
... Mass about 1 solar mass, with radius of about 15 to 30 km. Neutron stars have overall densities of 1017 kg/m3. During neutron star formation angular momentum and magnetic flux are conserved. Both are inversely proportional to the square of the radius, giving rotation periods between about 1.4 ms to ...
... Mass about 1 solar mass, with radius of about 15 to 30 km. Neutron stars have overall densities of 1017 kg/m3. During neutron star formation angular momentum and magnetic flux are conserved. Both are inversely proportional to the square of the radius, giving rotation periods between about 1.4 ms to ...
Equation of state constraints for the cold dense matter inside neutron
... J1810.8-260. Care is taken to use only the hard state bursts where it is thought that the NS surface alone is emitting. We then use a Markov chain Monte Carlo algorithm within a Bayesian framework to obtain a parameterized equation of state (EoS) of cold dense matter from our initial mass and radius ...
... J1810.8-260. Care is taken to use only the hard state bursts where it is thought that the NS surface alone is emitting. We then use a Markov chain Monte Carlo algorithm within a Bayesian framework to obtain a parameterized equation of state (EoS) of cold dense matter from our initial mass and radius ...
X-ray astronomy detector
X-ray astronomy detectors are instruments that detect X-rays for use in the study of X-ray astronomy.X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray emission from celestial 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 part of space science.X-ray astronomy detectors have been designed and configured primarily for energy and occasionally for wavelength detection using a variety of techniques usually limited to the technology of the time.