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1.
The paper presents the results obtained from the UV-spectrometer of the Solar Spectrum Experiment during the Spacelab 1 mission in December 1983. The irradiance data concern 492 passbands, which are located between 200 and 358 nm at almost equidistant wavelengths separated by about 0.3 nm. The passbands have a well-defined, bell-shaped profile with a full width at half maximum of about 1.3 nm. The data, which have an error budget between 4 and 5%, agree closely with the spectral distributions observed by Heath (1980) and Mentall et al. (1981) and confirm that the solar irradiance and the fluxes of Sun-like stars show about the same spectral distribution down to at least 240 nm. 相似文献
2.
Gérard Thuillier Michel Hersé Paul C. Simon Dietrich Labs Holger Mandel Didier Gillotay Thomas Foujols 《Solar physics》1998,177(1-2):41-61
The SOLSPEC instrument has been built to carry out solar spectral irradiance measurements from 200 to 3000 nm. It consists of three spectrometers designed to measure the solar spectral irradiance in ultraviolet, visible, and infrared domains. It flew with the ATLAS I mission in March 1992. This paper is dedicated to the visible part of the solar spectrum. Comparisons with recent data are shown and differences below 450 nm are discussed. 相似文献
3.
G. Thuillier G. Schmidtke C. Erhardt B. Nikutowski A. I. Shapiro C. Bolduc J. Lean N. Krivova P. Charbonneau G. Cessateur M. Haberreiter S. Melo V. Delouille B. Mampaey K. L. Yeo W. Schmutz 《Solar physics》2014,289(12):4433-4452
Onboard the International Space Station (ISS), two instruments are observing the solar spectral irradiance (SSI) at wavelengths from 16 to 2900 nm. Although the ISS platform orientation generally precludes pointing at the Sun more than 10?–?14 days per month, in November/December 2012 a continuous period of measurements was obtained by implementing an ISS ‘bridging’ maneuver. This enabled observations to be made of the solar spectral irradiance (SSI) during a complete solar rotation. We present these measurements, which quantify the impact of active regions on SSI, and compare them with data simultaneously gathered from other platforms, and with models of spectral irradiance variability. Our analysis demonstrates that the instruments onboard the ISS have the capability to measure SSI variations consistent with other instruments in space. A comparison among all available SSI measurements during November–December 2012 in absolute units with reconstructions using solar proxies and observed solar activity features is presented and discussed in terms of accuracy. 相似文献
4.
S. Turck-Chièze P. Lamy C. Carr P. H. Carton A. Chevalier I. Dandouras J. M. Defise S. Dewitte T. Dudok de Wit J. P. Halain S. Hasan J. F. Hochedez T. Horbury P. Levacher M. Meissonier N. Murphy P. Rochus A. Ruzmaikin W. Schmutz G. Thuillier S. Vivès 《Experimental Astronomy》2009,23(3):1017-1055
The DynaMICCS mission is designed to probe and understand the dynamics of crucial regions of the Sun that determine solar
variability, including the previously unexplored inner core, the radiative/convective zone interface layers, the photosphere/chromosphere
layers and the low corona. The mission delivers data and knowledge that no other known mission provides for understanding
space weather and space climate and for advancing stellar physics (internal dynamics) and fundamental physics (neutrino properties,
atomic physics, gravitational moments...). The science objectives are achieved using Doppler and magnetic measurements of
the solar surface, helioseismic and coronographic measurements, solar irradiance at different wavelengths and in-situ measurements
of plasma/energetic particles/magnetic fields. The DynaMICCS payload uses an original concept studied by Thalès Alenia Space
in the framework of the CNES call for formation flying missions: an external occultation of the solar light is obtained by
putting an occulter spacecraft 150 m (or more) in front of a second spacecraft. The occulter spacecraft, a LEO platform of
the mini sat class, e.g. PROTEUS, type carries the helioseismic and irradiance instruments and the formation flying technologies.
The latter spacecraft of the same type carries a visible and infrared coronagraph for a unique observation of the solar corona
and instrumentation for the study of the solar wind and imagers. This mission must guarantee long (one 11-year solar cycle)
and continuous observations (duty cycle > 94%) of signals that can be very weak (the gravity mode detection supposes the measurement
of velocity smaller than 1 mm/s). This assumes no interruption in observation and very stable thermal conditions. The preferred
orbit therefore is the L1 orbit, which fits these requirements very well and is also an attractive environment for the spacecraft
due to its low radiation and low perturbation (solar pressure) environment. This mission is secured by instrumental R and
D activities during the present and coming years. Some prototypes of different instruments are already built (GOLFNG, SDM)
and the performances will be checked before launch on the ground or in space through planned missions of CNES and PROBA ESA
missions (PICARD, LYRA, maybe ASPIICS). 相似文献
5.
Thuillier Gérard Hersé Michel Simon Paul C. Labs Dietrich Mandel Holger Gillotay Didier 《Solar physics》1997,171(2):283-302
The SOLSPEC instrument has been built to carry out solar spectral irradiance measurements from space. It consists of three spectrometers designed to measure the solar spectral irradiance from 180 to 3000 nm. It flew for the first time in December 1983 with the SpaceLab 1 mission (SL1) and later with the ATLAS missions after significant improvement of the instrument optics and calibration procedures. For the ATLAS 1 mission in March 1992, the thermal conditions encountered during the measurements were better than those of SL1, leading to better data quality. Furthermore, other Sun spectrometers, two on the same platform and two others on board the Upper Atmosphere Research Satellite, have also carried out UV absolute spectral measurements at the same time. These opportunities allowed comparisons of solar irradiance determinations. The UV part of the measurements made during that mission is presented here as well as its calibration and accuracy analysis. 相似文献
6.
G. Thuillier J. Claudel D. Djafer M. Haberreiter N. Mein S. M. L. Melo W. Schmutz A. Shapiro C. I. Short S. Sofia 《Solar physics》2011,268(1):125-149
In this paper we compare observed, empirical, and modelled solar limb profiles and discuss their potential use to derive physical
properties of the solar atmosphere. The PHOENIX, SolMod3D, and COSI radiative transfer codes as well as VAL-C models are used
to calculate the solar limb shape under different assumptions. The main properties of each model are shown. The predicted
limb shape as a function of wavelength for different features on the solar disk, such as quiet Sun, sunspots, and faculae,
is investigated. These models provide overall consistent limb shapes with some discrepancies that are discussed here in terms
of differences in solar atmosphere models, opacities, and the algorithms used to derive the solar limb profile. Our analysis
confirms that the most common property of all models is limb shapes that are much steeper than what is observed, or predicted
by the available empirical models. Furthermore, we have investigated the role of the Fraunhofer lines within the spectral
domain used for the solar limb measurements. Our results show that the presence of the Fraunhofer lines significantly displaces
the limb inflection point from its position estimated assuming only the photospheric continuum. The PICARD satellite, launched
on 15 June 2010, will provide measurements of the limb shape at several wavelengths. This work shows that the precision of
these measurements allows for discrimination among the available models. 相似文献
7.
This instrument, at the present time in development, will fly on board Spacelab I in May 1983. Other flights are foreseen during the following missions. This instrument is composed by three double monochromators covering the range 170 to 3200 nm. The spectrometers have band-passes of 1 nm up to 900 nm and 20 nm from 850 to 3200 nm with an accuracy 10–2 nm. Calibration lamps are included in the instrument to monitor any change of its sensitivity and wavelength scale.Proceedings of the 14th ESLAB Symposium on Physics of Solar Variations, 16–19 September 1980, Scheveningen, The Netherlands.Institut d'Aéronomie Spatiale de Belgique, 3, avenue Circulaire-B1180 Bruxelles, Belgique.Landessternwarte-Koenigstuhl, D6900 Heidelberg, F.R.G.Hamburger Sternwarte, Gojenbergsweg, D2050 Hamburg 80, F.R.G. 相似文献
8.
G. Thuillier D. Bolsée G. Schmidtke T. Foujols B. Nikutowski A. I. Shapiro R. Brunner M. Weber C. Erhardt M. Hersé D. Gillotay W. Peetermans W. Decuyper N. Pereira M. Haberreiter H. Mandel W. Schmutz 《Solar physics》2014,289(6):1931-1958
On 7 February 2008, the SOLAR payload was placed onboard the International Space Station. It is composed of three instruments, two spectrometers and a radiometer. The two spectrometers allow us to cover the 16?–?2900 nm spectral range. In this article, we first briefly present the instrumentation, its calibration and its performance in orbit. Second, the solar spectrum measured during the transition between Solar Cycles 23 to 24 at the time of the minimum is shown and compared with other data sets. Its accuracy is estimated as a function of wavelength and the solar atmosphere brightness-temperature is calculated and compared with those derived from two theoretical models. 相似文献
9.
Thuillier G. Hersé M. Labs D. Foujols T. Peetermans W. Gillotay D. Simon P.C. Mandel H. 《Solar physics》2003,214(1):1-22
The SOLar SPECtrum (SOLSPEC) and the SOlar SPectrum (SOSP) spectrometers are two twin instruments built to carry out solar spectral irradiance measurements. They are made of three spectrometers dedicated to observations in the ultraviolet, visible and infrared domains. SOLSPEC flew with the ATmospheric Laboratory for Applications and Science (ATLAS) while SOSP flew on the EUropean Retrieval CArrier (EURECA) missions. ATLAS 1 and 2 data being already published, this paper is mostly dedicated to the ATLAS 3 and EURECA data in the IR domain. Comparisons between the ATLAS data sets and the Upper Atmosphere Research Satellite (UARS) results are made. EURECA IR data are shown and compared with previous results. Our best UV, visible and IR spectra are finally merged into a single absolute solar irradiance spectrum covering the 200 to 2400 nm domain. 相似文献
10.
To determine the apparent diameter of the Sun, it is first necessary to measure the shape of the intensity profile of the
solar limb with an imaging optical system (hereafter denoted as a solar-limb profile). The inflection point of the limb profile
is usually used as a reference for calculating the diameter. Because this point may be difficult to determine in the presence
of noise, it is necessary to define an appropriate filtering process that eliminates noise while preserving the position of
the inflection point. In this paper we study two filtering techniques, one based on the compact wavelet transform and the
other on the finite Fourier transform definition, that meet these requirements. The application of these two techniques to
data gathered by the Solar Disk Sextant experiment shows that the solar radius increased from 1992 to 1996 by about 197 mas.
However, a previous analysis of the same data and our present analysis provide a difference in the measured radii of about
92 mas. We show that this difference is entirely traced to the filtering process. 相似文献