3 edition of Solar EUV, XUV and soft x-ray telescope facilities found in the catalog.
Solar EUV, XUV and soft x-ray telescope facilities
G. L. Withbroe
by National Aeronautics and Space Administration, Goddard Space Flight Center, Smithsonian Institution, Astrophysical Observatory in Greenbelt, MD, Cambridge, MA
Written in English
Microfiche. [Washington, D.C. : National Aeronautics and Space Administration, 1984] 1 microfiche.
|Statement||[George L. Withbroe, principal investigator].|
|Series||NASA CR -- 170602., NASA contractor report -- NASA CR-170602.|
|Contributions||Smithsonian Astrophysical Observatory., Goddard Space Flight Center.|
|The Physical Object|
Abstract. We have developed seven compact soft X-ray/EUV (XUV) multilayer coated and two compact FUV interference film coated Cassegrain and Ritchey-Chretien telescopes for a rocket borne observatory, the Multi-Spectral Solar Telescope Array. The telescope consists of a package of (a) a normal-incidence (NI) EUV telescope and (b) a grazing-incidence (GI) soft X-ray telescope. The NI telescope chiefly provides images of low corona (whose temperature 1 MK or even lower) with ultra-high angular resolution ("/pixel) in 3 wavelength bands (, , and 94 angstroms).Cited by: 2.
SXT is a X-ray focusing telescope operating in the energy range keV (X-rays are often again detected as individual photons. They are quantified in terms of their energy rather than their wavelength, purely due to initial development of X-ray detectors without optics. 1 keV photon is approximately nm (for comparison, a blue light photon has an energy of about 3 eV). Solar EUV Irradiance Solar Extreme Ultraviolet (EUV) is solar radiation that covers the wavelengths 10 – nm of the electromagnetic spectrum. It is highly energetic and it is absorbed in the upper atmosphere, which not only heats the upper atmosphere but also .
The Solar EUV Experiment (SEE) includes two instruments to measure the solar VUV spectral irradiance from to nm. The EUV Grating Spectrograph (EGS) is a normal incidence Rowland circle spectrograph and has a spectral range of 25 to nm with a nm spectral resolution. The EGS photon-counting detector is a CODACON array detector ( G. Mollenstedt, and M. Mozer, “EUV and soft x-ray images of the sun on March 11th, ,” Solar Phys 81 (). H. Bräuninger, P. Predehl, and K. P. Beuermann, “Transmission grating efficiencies for wavelengths betweenFile Size: 64KB.
In the field
Pakistan election, 2002
Genji Monogatari (Tut Books. L)
Blueprint Soviet Eco
Pool of the Pink Lilies
How to meditate
Introduction to mathematical statistics.
Eye of the beholder
Lieut. Henry R. Lemly.
Hands-on guide to oscilloscopes
Adam International Review
Facility class, high resolution instrumentation can enable maximum spatial, spectral and temporal resolutions and provide understanding of the complex physical conditions in the outer solar atmosphere and the mechanisms responsible for these conditions.
The scientific rationale for facility class instruments operating in the EUV, XUV, and soft X ray spectral ranges are discussed.
Solar EUV, XUV and soft X-ray telescope facilities. By G. Withbroe. Abstract. Facility class, high resolution instrumentation can enable maximum spatial, spectral and temporal resolutions and provide understanding of the complex physical conditions in the outer solar atmosphere and the mechanisms responsible for these conditions.
The Author: G. Withbroe. In this paper we have reviewed our achievements in soft X-ray and extreme ultraviolet (EUV) optics. Up to now, the research system of soft X-ray and EUV optics has been established, including light sources, detectors, calibrations, optical testing and machining of super smooth mirrors, and fabrications of multilayer film mirrors.
Based on our achievements, we have developed two types of solar Cited by: 4. by the Solar EUV-XUV-Soft X-ray Telescope Fac flty Definition Team esta-blished by NASA. It discusses the scientific rationale for facility class Instru-ments operating in the EUV, XUV and soft X-ray srFictral ranges and describes possible configurations for these facilities.
Team Members and Consultants a W. Behring G. Brueckner a R. Chase. The scientific importance of the Advanced Solar Observatory (ASO) is discussed with emphasis on its soft X-ray, XUV, and EUV facilities.
The principal achievement expected from the ASO's SXR/XUV and EUV telescope is a greatly improved resolution of the magnetic structure and activity in the transition region and corona. Observations from these facilities, combined with complementary Author: Ron Moore, David Bohlin.
The Solar X-EUV imaging telescope (XEIT), which operates in the Åwavelength bands and the Å EUV emission line, is designed to monitor and predict solar activities resulting in variations. X-ray bright points, and CME ejecta moving away from the sun at km/sec. To meet these objectives, the SXI images the solar corona in the soft X-ray to extreme ultraviolet (XUV to EUV) region of the electromagnetic spectrum.
Full-disk solar images are provided with a X array with 5 arc second pixels in several wavelength bands. Abstract The space solar EUV and X ray imaging camera is the core of the solar EUV and X ray imaging telescope, which is designed to monitor and predict solar activities, such as CMEs, flare and coronal hole.
This paper presents a comprehensive description of the camera, from the detector selection to the electronics system design, and gives.
XUV multilayer mirror and XUV filter support leading-edge attosecond science and are applied to next generation lithography research. NTT-AT, providing not only elements but also optical systems, is the best partner for customers who engage in research and development in the XUV, EUV, and X-ray fields.
Solar Images to be made by unique X-ray telescope April 2, A unique cluster of telescopes that make X-rays take a U-turn has been selected for a fourth flight to capture "multicolored" images that will help us understand why the sun's outer atmosphere is so hot.
Get this from a library. Solar EUV, XUV and soft x-ray telescope facilities: final report of the facility definition team. [G L Withbroe; Smithsonian Astrophysical Observatory.; Goddard Space Flight Center.].
Space solar telescope in soft X-ray and EUV band Article in Science in China Series G Physics Mechanics and Astronomy 52(11) November with 17 Reads How we measure 'reads'.
10 December EUV and soft x-ray telescope-spectrometer for imaging spectroscopy on the Solar Orbiter mission: grazing-incidence configuration.
Luca Poletto, Giuseppe Tondello, Massimo Landini. Author Affiliations + Proceedings VolumeUV/EUV and Visible Space Cited by: 2. Solar Gamma- X- and EUV Radiation It seems that you're in USA. We have a The Structure of Solar Active Regions from EUV and Soft X-Ray Observations.
Pages Brueckner, G. Preview Buy Chap19 € Fe xxiv Emission in Solar Flares Observed with the NRL/ATM XUV Slitless Spectrograph. Pages Widing, Kenneth G. Brand: Springer Netherlands.  Solar extreme ultraviolet (EUV; 10– nm) and soft X‐ray (XUV; 0–10 nm) radiation are major heat sources for the Mars thermosphere as well as the primary source of ionization that creates the ionosphere.
In investigations of Mars thermospheric chemistry and dynamics, solar irradiance models are used to account for variations in this by: 8. PROCEEDINGS VOLUME Optics for EUV, X-Ray, and Gamma-Ray Astronomy II. Editor(s): Wavelength separation of plus and minus orders of soft-x-ray–EUV multilayer-coated gratings at near-normal incidence Characterization of a hard-x-ray telescope at a synchrotron facility.
is solar extreme ultraviolet (EUV; 10–nm) and soft X-ray (XUV; 0–10nm) radiation. Solar irradiance varies with solar longitude on solar cycle, solar rotation, and solar ﬂare time scales. Uncertainties in EUV and XUV irradiance illuminating Venus, Earth, and Mars limit the usefulness of thermospheric codes in studies of their File Size: 1MB.
Other solar feature observations include flare properties, newly emerging active regions, X-ray bright points, and CME ejecta moving away from the sun at km/sec. To meet these objectives, the SXI images the solar corona in the soft X-ray to extreme ultraviolet (XUV to EUV) region of the electromagnetic spectrum.
Full-disk solar images are. X-ray and ultraviolet (UV) observations of the outer solar atmosphere have been used for many decades to measure the fundamental parameters of the solar plasma. This review focuses on the optically thin emission from the solar atmosphere, mostly found at UV and X-ray (XUV) wavelengths, and discusses some of the diagnostic methods that have been used to measure electron densities, Cited by: While solar cycle variability near nm is only about 10%, the solar cycle variability T.
Woods et al.: TIMED Solar EUV Experiment at shorter wavelengths is typically a factor of 2 to 3 for chromospheric emissions and as much as a factor of 10 to for coronal by:. A High-Resolution Solar Telescope Cluster is intended to carry out studies of solar internal dynamics and the photosphere, chromosphere and low corona at visible, UV, EUV, XUV and soft X-ray wavelengths.
A Pinhole/Occulter Facility would perform high-resolution studies of the outer corona and solar wind in the visible and UV regions, and of.Len Culhane 13th September, Role of XUV and X-ray Observations Solar Plasma Spectroscopy 2 Introduction and Summary • Photon wavelength and energy ranges - XUV/EUV: Å – Å or keV – keV - Soft X-ray: 1 Å – Å or 10 keV – keV.Advances in X-Ray/EUV Optics and Components XV Wednesday - Thursday 26 - 27 August Conference Sessions Conditions in which off-plane diffraction can efficiently provide high spectral resolving power in EUV/soft x-ray monochromators Paper Author(s): Werner H.
Jark, Elettra-Sincrotrone Trieste S.C.p.A. (Italy) XUV gratings.