Particle kinematics in solar flares: observations - ETH E
... This thesis is devoted to the study of particle acceleration and propagation processes in solar flares. Solar flares are amongst the most powerful and energetic activity phenomena our Sun exhibits. They release energy of the order of 1032 erg in seconds to minutes. In the process, electrons and prot ...
... This thesis is devoted to the study of particle acceleration and propagation processes in solar flares. Solar flares are amongst the most powerful and energetic activity phenomena our Sun exhibits. They release energy of the order of 1032 erg in seconds to minutes. In the process, electrons and prot ...
PowerPoint format
... Determination of the chemical enrichment history of the Galaxy and the Universe via high resolution spectroscopy of the oldest stars in the Milky Way and gas clouds illuminated by distant quasars. • High-resolution (R=50-150,000) spectroscopy of faint objects at uv-optical wavelengths ...
... Determination of the chemical enrichment history of the Galaxy and the Universe via high resolution spectroscopy of the oldest stars in the Milky Way and gas clouds illuminated by distant quasars. • High-resolution (R=50-150,000) spectroscopy of faint objects at uv-optical wavelengths ...
Ch 5 notes on telescopes
... iv. Have poor angular resolution because of diffraction 1. Can be used in tandem 2. Interferometry – a technique that makes it possible to produce radio images of angular resolution higher than the best optical telescopes v. Advantages: 1. operate 24hrs day 2. can be made through cloudy skies and ev ...
... iv. Have poor angular resolution because of diffraction 1. Can be used in tandem 2. Interferometry – a technique that makes it possible to produce radio images of angular resolution higher than the best optical telescopes v. Advantages: 1. operate 24hrs day 2. can be made through cloudy skies and ev ...
The keV–TeV connection in gamma-ray binaries
... The gamma-ray emission from astrophysical sources is arguably different from the emission in the rest of the electromagnetic spectrum because it cannot be generated by hot matter. High energy gamma radiation is therefore an indication that non-thermal processes, which are able to concentrate a large ...
... The gamma-ray emission from astrophysical sources is arguably different from the emission in the rest of the electromagnetic spectrum because it cannot be generated by hot matter. High energy gamma radiation is therefore an indication that non-thermal processes, which are able to concentrate a large ...
New challenges in Nuclear Structure
... First excited states in nuclei close to the drip lines Neutron rich nuclei at (very) high spins Structure of the heaviest nuclei close to the “line of stability” ...
... First excited states in nuclei close to the drip lines Neutron rich nuclei at (very) high spins Structure of the heaviest nuclei close to the “line of stability” ...
Conference AS11 - Thirty Meter Telescope
... While the default design for HROS called for a rectangular entrance aperture for a point source spectrograph, we will build an array of several one square arc second hexagonal fiber bundles. In order to take advantage of improved performance when the seeing disk decreases, we are considering using ...
... While the default design for HROS called for a rectangular entrance aperture for a point source spectrograph, we will build an array of several one square arc second hexagonal fiber bundles. In order to take advantage of improved performance when the seeing disk decreases, we are considering using ...
Radio and X-ray signatures of merging neutron stars
... Thus, our strongest prediction is the presence of an X-ray precursor to the neutron star merger. This precursor should be dominated by approximately thermal emission from the wind component, which progressively hardens as the binary approaches merger. For magnetars B15 , 1; this can approach energ ...
... Thus, our strongest prediction is the presence of an X-ray precursor to the neutron star merger. This precursor should be dominated by approximately thermal emission from the wind component, which progressively hardens as the binary approaches merger. For magnetars B15 , 1; this can approach energ ...
10. Electromagnetic waves
... wavelength – The distance between two matching points on neighbouring waves, which is measured in metres. ...
... wavelength – The distance between two matching points on neighbouring waves, which is measured in metres. ...
The Flow of Energy Out of the Sun
... The program that you will use today is designed to teach you how photons travel from the core of the Sun to the surface and how they interact with matter on their way into space. They interact in two general regions with two different effects: 1. The solar atmosphere is a thin layer of gas that make ...
... The program that you will use today is designed to teach you how photons travel from the core of the Sun to the surface and how they interact with matter on their way into space. They interact in two general regions with two different effects: 1. The solar atmosphere is a thin layer of gas that make ...
Surface temperature distribution and absorption features in Isolated
... the equation of state (EoS) P = P (ρ), if the medium is barotrope. It is determined by the model adopted to describe the matter inside the star. This system of differential equations is solved imposing the boundary conditions ρ(0) = ρc and P (R? ) = 0. Once the NS radius R? is fixed, the solution pr ...
... the equation of state (EoS) P = P (ρ), if the medium is barotrope. It is determined by the model adopted to describe the matter inside the star. This system of differential equations is solved imposing the boundary conditions ρ(0) = ρc and P (R? ) = 0. Once the NS radius R? is fixed, the solution pr ...
R&D towards huge liquid argon detectors for nucleon
... energy scale, etc should be investigated with electron/muon beam) • Charged pions (hadron interaction in medium, electric field dependence) NuFact09 at Chicago ...
... energy scale, etc should be investigated with electron/muon beam) • Charged pions (hadron interaction in medium, electric field dependence) NuFact09 at Chicago ...
Lecture ppt - UCO/Lick Observatory
... the science you want to do • Example 1: Search for planets around nearby stars – You can use the star itself for tip-tilt info – Little negative impact of image motion smearing • Example 2: Studies of high-redshift galaxies – Tip-tilt stars will be rare – Trade-off between fraction of sky where you ...
... the science you want to do • Example 1: Search for planets around nearby stars – You can use the star itself for tip-tilt info – Little negative impact of image motion smearing • Example 2: Studies of high-redshift galaxies – Tip-tilt stars will be rare – Trade-off between fraction of sky where you ...
The Flow of Energy Out of the Sun
... Most atoms in the Sun, and other stars, are said to be ionized because the intense temperatures have stripped off most of their electrons. Electron scattering occurs when a photon encounters an electron and causes it to vibrate or oscillate. The energy stolen from the photon in this process is re-ra ...
... Most atoms in the Sun, and other stars, are said to be ionized because the intense temperatures have stripped off most of their electrons. Electron scattering occurs when a photon encounters an electron and causes it to vibrate or oscillate. The energy stolen from the photon in this process is re-ra ...
Photon-Graviton Recycling as Cause of Gravitation
... galaxy surface brightness tests in a direction which would further support static models. The surface brightness of galaxies would be diminished by an extra factor of (1 + z)−1 due to time dilation, bringing the total reduction to (1 + z)−2. The extra factor significantly reduces the discrepancy bet ...
... galaxy surface brightness tests in a direction which would further support static models. The surface brightness of galaxies would be diminished by an extra factor of (1 + z)−1 due to time dilation, bringing the total reduction to (1 + z)−2. The extra factor significantly reduces the discrepancy bet ...
High Energy Astrophysics T. J.
... to an unprecedented set of instruments in orbit now. These instruments include XMM-Newton, Chandra and INTEGRAL. The first two are large X-ray instruments, one specialised in imaging (Chandra) the other in spectroscopy (XMM), because of its very large collecting area. INTEGRAL is sensitive above few ...
... to an unprecedented set of instruments in orbit now. These instruments include XMM-Newton, Chandra and INTEGRAL. The first two are large X-ray instruments, one specialised in imaging (Chandra) the other in spectroscopy (XMM), because of its very large collecting area. INTEGRAL is sensitive above few ...
transparencies - Rencontres de Moriond
... Pointing instruments (e.g. air Cherenkov) generally have better sensitivity than survey instruments. Counter example: Glast. Narrow field-of-view problems: i) you necessarily have an a priori discovery goal - serendipity almost ruled out. ii) While looking at one sleeping blazar, another can flare b ...
... Pointing instruments (e.g. air Cherenkov) generally have better sensitivity than survey instruments. Counter example: Glast. Narrow field-of-view problems: i) you necessarily have an a priori discovery goal - serendipity almost ruled out. ii) While looking at one sleeping blazar, another can flare b ...
Lecture 9 PPT
... • Cosmetic quality: Uniformity of response across pixels, dead pixels • Stability: does the pixel response vary with time? Page 31 ...
... • Cosmetic quality: Uniformity of response across pixels, dead pixels • Stability: does the pixel response vary with time? Page 31 ...
Super-Eddington outburst in a binary system: V4641 Sgr Mikhail Revnivtsev, Marat Gilfanov
... Low mass X-ray binary • Optical companion is small M < High mass X-ray binary M . Ratio of the accretion disk size to the companion star size is • Optical companion is large M > 3 − 5M . Ratio of the accretion ...
... Low mass X-ray binary • Optical companion is small M < High mass X-ray binary M . Ratio of the accretion disk size to the companion star size is • Optical companion is large M > 3 − 5M . Ratio of the accretion ...
MS word document
... pointed to the need for multi-slit near IR spectrometers to get the maximum mutliplex advantage from such instruments. They suggested using resolutions of greater than 3500 since, with a 2048 square detector, this would fully cover an atmospheric window and at the same time make OH suppression possi ...
... pointed to the need for multi-slit near IR spectrometers to get the maximum mutliplex advantage from such instruments. They suggested using resolutions of greater than 3500 since, with a 2048 square detector, this would fully cover an atmospheric window and at the same time make OH suppression possi ...
The Flow of Energy Out of the Sun
... Most atoms in the Sun, and other stars, are said to be ionized because the intense temperatures have stripped off most of their electrons. Electron scattering occurs when a photon encounters an electron and causes it to vibrate or oscillate. The energy stolen from the photon in this process is re-ra ...
... Most atoms in the Sun, and other stars, are said to be ionized because the intense temperatures have stripped off most of their electrons. Electron scattering occurs when a photon encounters an electron and causes it to vibrate or oscillate. The energy stolen from the photon in this process is re-ra ...
TheFlowOfEnergyOutOf..
... Most atoms in the Sun, and other stars, are said to be ionized because the intense temperatures have stripped off most of their electrons. Electron scattering occurs when a photon encounters an electron and causes it to vibrate or oscillate. The energy stolen from the photon in this process is re-ra ...
... Most atoms in the Sun, and other stars, are said to be ionized because the intense temperatures have stripped off most of their electrons. Electron scattering occurs when a photon encounters an electron and causes it to vibrate or oscillate. The energy stolen from the photon in this process is re-ra ...
Folie 1
... • Optical CCDs produce one electron per photon. Many photons have to be detected before a measurable signal can be produced. A single X-ray photon can produce 100-1000 electrons (1 electron per 3.6 eV of energy). With low amplifier noise this can be measured. Thus X-ray CCDs are photon counting devi ...
... • Optical CCDs produce one electron per photon. Many photons have to be detected before a measurable signal can be produced. A single X-ray photon can produce 100-1000 electrons (1 electron per 3.6 eV of energy). With low amplifier noise this can be measured. Thus X-ray CCDs are photon counting devi ...
幻灯片 1
... does not make sense in a classical model with electrons orbiting around a nucleus, but can be explained by atomic wavefunctions|an electron with a high principal quantum number (and little angular momentum) has a nite probability of being found at small radial distances. The study of X-rays has deve ...
... does not make sense in a classical model with electrons orbiting around a nucleus, but can be explained by atomic wavefunctions|an electron with a high principal quantum number (and little angular momentum) has a nite probability of being found at small radial distances. The study of X-rays has deve ...
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.