共查询到20条相似文献，搜索用时 515 毫秒
1.
A. Benmoussa J.-F. Hochedez W. K. Schmutz U. SchÜhle M. NeslÁdek Y. Stockman U. Kroth M. Richter A. Theissen Z. Remes K. Haenen V. Mortet S. Koller J. P. Halain R. Petersen M. Dominique M. D’Olieslaeger 《Experimental Astronomy》2003,16(3):141-148
Fabrication, packaging and experimental results on the calibration of metal-semiconductor-metal (MSM) photodetectors made on diamond are reported. LYRA (Lyman- RAdiometer onboard PROBA-2) will use diamond detectors for the first time in space for a solar physics instrument. A set of measurement campaigns was designed to obtain the XUV-to-VIS responsivity of the devices and other characterizations. The measurements of responsivity in EUV and VUV spectral ranges (40–240 nm) have been carried out by the Physkalisch-Technische Bundesanstalt (PTB) in Germany at the electron storage ring BESSY II. The longer wavelength range from 210 to 1127 nm was measured with monochromatic light by using a Xe-lamp at IMO-IMOMEC. The diamond detectors exhibit a photoresponse which lie in the 35–65 mA/W range at 200 nm (corresponding to an external quantum efficiency of 20–40%) and indicate a visible rejection ratio (200–500 nm) higher than four orders of magnitude. 相似文献
2.
Bruce Swinyard Peter Clegg Sarah Leeks Matt Griffin Tanya Lim Martin Burgdorf 《Experimental Astronomy》2000,10(2-3):157-176
The performance of the ten doped germaniumphotoconducting detectors on the Infrared SpaceObservatory Long Wavelength Spectrometer is discussed. This instrument was designed to make spectroscopicmeasurements of astronomical sources in the wavelengthrange from 43 to 198 m. It employed* a combination of stressed and unstressed Ge:Ga detectorsand one Ge:Be detector coupled to Infrared Labs JF-4integrating amplifiers. The performance of thedetectors was affected by the ionising radiation inthe space environment. The Noise Equivalent Power ofthe detectors increased by a factor of 4 compared tothat measured during ground testing. We show thatthis was the result of reducing the operating bias,and therefore the responsivity, of the detectors andusing shorter integration ramps to alleviate theeffects of the ionising radiation impacts.
ast ISO exhausted its helium supply on 8 April 1998. 相似文献
3.
Rodger I. Thompson 《Experimental Astronomy》1994,3(1-4):93-100
NICMOS is a second generation instrument for the Hubble Space Telescope to provide imaging and spectroscopic capabilities in the near infrared region. NICMOS utilizes HgCdTe detectors in three cameras, one with grisms, to image in the 0.8–2.5 mm spectral region. 相似文献
4.
Alix Lombard Anny Cazenave Kien DoMinh Cecile Cabanes R. Steven Nerem 《Global and Planetary Change》2005,48(4):155
In this paper we compare sea level trends observed at a few selected tide gauges of good quality records with thermosteric (i.e., due to ocean temperature change) sea level trends over 1950–1998 using different gridded ocean temperature data sets from Levitus et al. (2000) [Levitus, S., Stephens, C., Antonov, J.I., Boyer, T.P., 2000. Yearly and Year-Season Upper Ocean Temperature Anomaly Fields, 1948–1998. U.S. Gov. Printing Office, Washington, D.C. pp. 23.], Ishii et al. (2003) [Ishii, M., Kimoto, M., Kachi, M., 2003. Historical ocean subsurface temperature analysis with error estimates, Mon. Weather Rev., 131, 51–73.] and Levitus et al. (2005) [Levitus S., Antonov, J.I., Boyer, T.P., 2005. Warming of the world ocean, 1955–2003. Geophys. Res. Lett. 32, L02604. doi:10.1029/2004GL021592.]. When using the Levitus data, we observe very high thermosteric rates at sites located along the northeast coast of the US, north of 37°N. Such high rates are not observed with the Ishii data. Elsewhere, thermosteric rates agree reasonably well whatever the data set. Excluding the northeast US coastline sites north of 37°N, we compare tide gauge-based sea level trends with thermosteric trends and note that, in spite of a significant correlation, the latter are too small to explain the observed trends. After correcting for thermosteric sea level trends, residual (observed minus thermosteric) trends have an average value of 1.4 ± 0.5 mm/year, which should have an eustatic (i.e., due to ocean mass change) origin. This result supports the recent investigation by Miller and Douglas (2004) [Miller, L., Douglas, B.C., 2004. Mass and volume contributions to 20th century global sea level rise. Nature 428, 406–408.] which suggests that a dominant eustatic contribution is needed to explain the rate of sea level rise of the last decades observed by tide gauges, and shows that Cabanes et al. (2001) [Cabanes, C., Cazenave, A., Le Provost, C., 2001. Sea level rise during past 40 years determined from satellite and in situ observations. Science 294, 840–842.] arrived at an incorrect conclusion due to peculiarities in the gridded Levitus et al. (2000) [Levitus, S., Stephens, C., Antonov, J.I., and Boyer, T.P., 2000. Yearly and Year-Season Upper Ocean Temperature Anomaly Fields, 1948–1998. U.S. Gov. Printing Office, Washington, D.C. pp. 23.] data set. 相似文献
5.
G. J. Fishman 《Astrophysics and Space Science》1981,75(1):125-134
The research program in gamma-ray burst astronomy at the NASA/Marshall Space Flight Center is described. Large-area scintillation detector arrays have been flown on high-altitude balloons, and an array is being developed for the Gamma-Ray Observatory. The design of these detectors is described along with results obtained from previous balloon flights.Paper presented at the International Gamma-Ray Burst Symposium, Toulouse, France, 26–28 November, 1979. 相似文献
6.
We describe how the ISO-SWS (Infrared Space Observatory – Short Wavelength Spectrometer) software packages detect various glitch events i.e. high energy particle hits effecting the SWS detectors. A rough classification of glitch types is given. The events cause an instantaneous change in the slope of the SWS detector read outs followed by a distortion of the further samples, so called glitch tails. As a consequence the S/N ratio and photometric accuracy are reduced.Different strategies, how to remove the resulting distortion of the detectorread-out-ramp after a hit, are presented. The methods of the basic SWS software packages, the Pipeline and Interactive Analysis, will be discussed. The Pipeline has to treat glitch effects automatically. The Interactive Analysis system provides the user with a comfortable Graphical User Interface (GUI) for Trend Analysis, detailed analysis of certain glitches and the testing of new algorithms. 相似文献
7.
S. Cecchini H. Dekhissi G. Giacomelli G. Mandrioli A. R. Margiotta L. Patrizii F. Predieri P. Serra M. Spurio 《Astroparticle Physics》1993,1(4):369-376
We present measurements of fragmentation cross sections of relativistic nuclei and upper limits for the production probability of nuclear fragments with fractional charge using CR39 nuclear track detectors and an automated scanning system. The measurements of the total and partial charge changing fragmentation cross sections concern 16 GeV/nucleon oxygen ions, 14.5 GeV/nucleon silicon ions and 200 GeV/nucleon sulphur ions interacting in copper and CR39 targets. No evidence for fractionally charged fragments was found requiring a minimum track length of 7 mm in CR39 detectors placed after a 14 mm copper target. The combined upper limit for the production probability of fractionally charged fragments relative to ordinary ones is at the level of 1.2–2.3 × 10–4 (90% C.L.). The charge resolution of the CR39 detectors for an average of 10 measurements of the same track is σ = 0.05e at Z = 6. 相似文献
8.
Rajmal Jain Hemant Dave A. B. Shah N. M. Vadher Vishal M. Shah G. P. Ubale K. S. B. Manian Chirag M. Solanki K. J. Shah Sumit Kumar S. L. Kayasth V. D. Patel Jayshree J. Trivedi M. R. Deshpande 《Solar physics》2005,227(1):89-122
The first space-borne solar astronomy experiment of India, namely Solar X-ray Spectrometer (SOXS), was successfully launched on 08 May 2003 on board geostationary satellite GSAT-2 of India. The SOXS is composed of two independent payloads, viz. SOXS Low-Energy Detector (SLD) Payload and SOXS High-Energy Detector (SHD) Payload. The SOXS aims to study the full-disk integrated X-ray emission in the energy range from 4 keV to 10 MeV. In this paper we present the first report on the SLD instrumentation and its in-orbit performance. The SLD payload was designed and developed at the Physical Research Laboratory in collaboration with various centers of Indian Space Research Organisation (ISRO). The basic scientific aim of the SLD payload is to study solar flares in the energy range from 4 to 60 keV with high spectral and temporal resolution. To meet these requirements, the SLD payload employs state-of-the-art solid state detectors, the first time for a solar astronomy experiment, viz. Si PIN (4 –25 keV), and cadmium–zinc–telluride (4 –60 keV). With their superb high-energy resolution characteristics, SLD can observe iron and iron–nickel complex lines that are visible only during solar flares. In view of its 3.4 FOV, the detector package is mounted on a Sun Aspect System, for the first time, to get uninterrupted observations in a geostationary orbit. The SLD payload configuration, its in-flight operation, and the response of the detectors are presented. We also present the first observations of solar flares made by the SLD payload and briefly describe their temporal and spectral mode results. 相似文献
9.
The Naval Research Laboratory flew solar X-ray ionization chamber detectors on a series of Solar Radiation (SOLRAD) satellites from 1960 through 1979. The flare responses of the SOLRAD 11 detectors are compared with those of the similar NOAA SMS/GOES detectors during two periods of common observations. The nominal GOES fluxes exceed those of SOLRAD 11 by a factor of 1.5–2 in the 0.5–4 Å band, but fall below those of SOLRAD by a factor of 2–4 in the 1–8 Å band. Significant passband differences account for these relationships between the detector responses. Since the X-ray detectors are standardized among the various SOLRAD satellites, and all detectors are closely matched among the various SMS/GOES satellites, these conversion factors allow the SOLRAD flare observations to serve as proxies for GOES X-ray observations prior to the GOES era. We summarize the detector characteristics and data sources of the 0.5–3 Å and 1–8 Å detectors for the SOLRAD series. 相似文献
10.
WSO／UV(世界空间紫外天文台)以及监测太阳活动的特殊探测器(Solar Sentinel)都需要在日-地(月)系的平动点附近运行，且相对日-地(月)系要求其几何位置几乎保持不变，因此有必要阐明平动点的动力学特征及其附近的运动状况。基于这一点，对限制性三体模型下，日-地(月)系中平动点附近扰动运动的稳定性作了详尽的分析，尤其讨论了共线平动点具有不稳定动力学特征时，如何使WSO／UV这类空间探测器保持在其附近的情况；同时阐明了轨道保持不变的条件和相应的轨控措施。 相似文献
11.
R. P. Lin D. W. Curtis J. H. Primbsch P. R. Harvey W. K. Levedahl D. M. Smith R. M. Pelling F. Duttweiler K. Hurley 《Solar physics》1982,113(1-2):333-345
We describe a balloon payload designed to study the processes of energy release, particle acceleration, and heating of the active corona, in hard X-ray microflares and normal flares. An array of liquid nitrogen-cooled germanium detectors together with large area phoswich scintillation detectors provide the highest sensitivity (500 cm2) and energy resolution (0.7 keV) ever achieved for solar hard X-ray (15–600 keV) measurements. These detectors were flown in February 1987 from Australia on a long duration RAdiation COntrolled balloON (RACOON) flight (LDBF) which provided 12 days of observations before cutdown in Brazil. The payload includes solar cells for power, pointing and navigation sensors, a microprocessor controlled data system with VCR tape storage, and transmitters for GOES and ARGOS spacecraft. This successful flight illustrates the potential of LDBF's for solar flare studies.Also Physics Department.Presently at Space Sciences Laboratory, University of California, Berkeley CA 94720. 相似文献
12.
M. E. VanHoosier J.-D. F. Bartoe G. E. Brueckner D. K. Prinz J. W. Cook 《Solar physics》1981,74(2):521-530
There exists a growing need to improve the accuracy of measurement of the absolute solar flux within the wavelength range 120–400 nm. Although full-disk solar fluxes and variations thereof in the 120–400 nm region are required to model the solar atmosphere, current increased interest in the measurements arises from their importance in modeling the terrestrial atmosphere. We describe the Solar Ultraviolet Spectral Irradiance Monitor (SUSIM) experiment under development at the Naval Research Laboratory (NRL) for flight aboard the Space Shuttle and the Upper Atmospheric Research Satellite (UARS). SUSIM will monitor the solar flux in the 120–400 nm region with high precision, using an in-flight calibration system to reduce absolute error to < 10%, and error relative to the 400 nm continuum to < 1%.Proceedings of the 14th ESLAB Symposium on Physics of Solar Variations, 16–19 September 1980, Scheveningen, The Netherlands. 相似文献
13.
C. U. Keller 《Solar physics》1996,164(1-2):243-252
Recent instrumental developments in imaging polarimetry allow array detectors to reach a polarimetric sensitivity of 1 × 10–4 of the intensity. New instrumental effects appear at these levels of sensitivity and generate spurious polarization signals with amplitudes of up to 5 × 10–4. Here I discuss these effects and present methods to avoid them. Polarized spectra with an rms noise of 6 × 10–6 may then be obtained. Furthermore a method is brought to the reader's attention that allows polarization measurements at the 1 × 10–4 level with regular array detectors, e.g. in the near-infrared. 相似文献
14.
J. A. D. L. Blommaert L. Metcalfe B. Altieri A. Biviano K. Okumura R. Siebenmorgen S. Guest S. Ott 《Experimental Astronomy》2000,10(2-3):241-254
An overview is given of the absolute flux calibration of the ISOCAMdetectors. The flux calibration is based on observations of standard stars selected from the Ground Based Preparatory Programme, for which Kurucz stellar models are available. No dependencies of the responsivity on different configurations of thecamera were found. No trend of changing responsivity is found throughout the mission for the SW and LW detectors. There exists a decreasing responsivity of about 5% for LW during the orbit. 相似文献
15.
16.
One of the main limitations to the sensitivity of the infrared camera ISOCAM on-board the Infrared Space Observatory (ISO)
comes from responsivity variations and glitches caused by the impacts of charged particles in photo-detectors. Glitch rate
measurements, glitch properties and removal methods have already been addressed during the first ISO detector workshop(Madrid,
1998) and published in a special issue of Experimental Astronomy. It appeared that glitch rate and most of glitch properties
could be reproduced by Monte-Carlo simulations. This is very interesting in order to predict before launch the effect of charged
particles in photo-detectors operated in space. This paper presents results of Monte-Carlo simulations of radiation effects
on ISOCAM detectors. Glitch rates, spatial and energetic properties of glitches have been computed and are compared with measured
values.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
17.
EDELWEISS Collaboration P. Di Stefano L. Berg B. Chambon M. Chapellier J. Chaumont G. Chardin P. Charvin M. De Jsus D. Drain L. Dumoulin P. Forget P. Garoche J. Gascon C. Goldbach D. L'Hte J. Mallet J. Mangin S. Marnieros L. Miramonti L. Mosca X-F. Navick G. Nollez P. Pari S. Pcourt E. Simon L. Stab J-P. Torre R. Tourbot D. Yvon 《Astroparticle Physics》2001,14(4):1425
The discrimination capabilities of a 70 g heat and ionization Ge bolometer are studied. This first prototype has been used by the EDELWEISS dark matter experiment, installed in the Laboratoire Souterrain de Modane, for direct detection of WIMPs. Gamma and neutron calibrations demonstrate that this type of detector is able to reject more than 99.6% of the background while retaining 95% of the signal, provided that the background events distribution is not biased towards the surface of the Ge crystal. However, the 1.17 kg day of data taken in a relatively important radioactive environment show an extra population slightly overlapping the signal. This background is likely due to interactions of low energy photons or electrons near the surface of the crystal, and is somewhat reduced by applying a higher charge-collecting inverse bias voltage (−6 V instead of −2 V) to the Ge diode. Despite this contamination, more than 98% of the background can be rejected while retaining 50% of the signal. This yields a conservative upper limit of 0.7 event day−1 kg−1 keVrecoil−1 at 90% confidence level in the 15–45 keV recoil energy interval; the present sensitivity appears to be limited by the fast ambient neutrons. Upgrades in progress on the installation are summarized. 相似文献
18.
A. Abergel M. A. Miville-Deschênes F. X. Désert M. Pérault H. Aussel M. Sauvage 《Experimental Astronomy》2000,10(2-3):353-368
The detector of the long wavelength channel of the ISOCAMcamera on-board the Infrared Space Observatory is a Galliumdoped Silicon photo-conductor hybridized by Indium bump. Itpresents systematic memory effects of the response which canbias the photometry by a factor of typically 40%. The main features of the response after flux variations are discussed. A simple empirical model actually used to correct systematically the data with a photometric accuracy of 5–10% is detailed. 相似文献
19.
{We investigate the conversion of the 0.5–4 and 1–8 Å soft X-ray flux measurements made by detectors on the Geostationary Operational Environmental Satellites (GOES) into temperature and emission measures of coronal plasma using modern spectral models and modern understanding of coronal abundances. In particular, the original analysis by Thomas, Starr and Crannell (1985) is updated to take into account the realization that coronal abundances may be quite different from photospheric abundances. An important result of this analysis is that the derived temperatures and emission measures depend strongly on the assumed abundances even at high temperatures where continuum rather than spectral lines dominates the Sun’s X-ray spectrum. This occurs because the higher coronal abundances mean that most of the continuum is due to free–bound emission processes, not free–free emission, and thus is abundance-dependent. We find significant differences between modern calculations of the temperature response of the flux measurements and the versions currently in use: for a typical flare, emission measures may be up to a factor of 4 smaller than the current software suggests. Derived temperatures are similar for both photospheric and coronal abundances for cool flares (e.g., 15 MK), but for hot flares (e.g., 35 MK) coronal abundances can lead to significantly (~25%) lower temperatures being derived. 相似文献
20.
M. Yoshimori K. Okudaira Y. Hirasima T. Igarashi M. Akasaka Y. Takai K. Morimoto T. Watanabe K. Ohki J. Nishimura T. Yamagami Y. Ogawara I. Kondo 《Solar physics》1991,136(1):69-88
The SOLAR-A spacecraft has spectroscopic capabilities in a wide energy band from soft X-rays to gamma-rays. The Wide Band Spectrometer (WBS), consisting of three kinds of spectrometers, soft X-ray spectrometer (SXS), hard X-ray spectrometer (HXS) and gamma-ray spectrometer (GRS), is installed on SOLAR-A to investigate plasma heating, high-energy particle acceleration, and interaction processes. SXS has two proportional counters and each counter provides 128-channel pulse height data in the 2–30 keV range every 2 s and 2-channel pulse count data every 0.25 s. HXS has a NaI scintillation detector and provides 32-channel pulse height data in the 20–400 keV range every 1 s and 2-channel pulse count data every 0.125 s. GRS has two identical BGO scintillation detectors and each detector provides 128-channel pulse height data in the 0.2–10 MeV range every 4 s and 4-channel pulse count data (0.2–0.7, 0.7–4, 4–7, and 7–10 MeV) every 0.25–0.5 s. In addition, each of the BGO scintillation detectors provides 16-channel pulse height data in the 8–100 MeV range every 4 s and 2-channel pulse count data (8–30 and 30–100 MeV) every 0.5 s. The SXS observations enable one to study the thermal evolution of flare plasma by obtaining time series of electron temperatures and emission measures of hot plasma; the HXS observations enable one to study the electron acceleration and heating mechanisms by obtaining time series of the electron spectrum; and the GRS observations enable one to study the high-energy electron and ion acceleration and interaction processes by obtaining time series of electron and ion spectra.After the launch the name of SOLAR-A has been changed to YOHKOH. 相似文献