The solar package on ISS: SOL-ACES

Wienhold, F. G.; Anders, J.; Galuska, B.; Klocke, U.; Knothe, M.; Riedel, Wolfgang; Schmidtke, G.; Singler, R.; Ulmer, U.; Wolf, H.

doi:10.1016/s1464-1917(00)00060-x

Cited by 6 publications

(7 citation statements)

References 4 publications

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“…The SDO EVE will measure the solar radiation from 0.1 to 105 nm with 0.1-nm spectral resolution at wavelengths longer than 5 nm. In addition, the ESA Solar Auto-Calibrating EUV Spectrometers (SOL-ACES) (Wienhold et al, 2000) is planning to make new solar EUV irradiance measurements in 2008 -2010 from the International Space Station. The SOL-ACES will measure the solar radiation from 17 to 220 nm with a spectral resolution from 0.3 to 2 nm with four grazing incidence planar grating spectrometers.…”

Section: Discussionmentioning

confidence: 99%

XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models

et al. 2008

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Solar soft X-ray (XUV) radiation is highly variable on all time scales and strongly affects Earth's ionosphere and upper atmosphere; consequently, the solar XUV irradiance is important for atmospheric studies and for space weather applications. Although there have been several recent measurements of the solar XUV irradiance, detailed understanding of the solar XUV irradiance, especially its variability during flares, has been hampered by the broad bands measured in the XUV range. In particular, the simple conversion of the XUV photometer signal into irradiance, in which a static solar spectrum is assumed, overestimates the flare variations by more than a factor of two as compared to the atmospheric response to the flares. To address this deficiency in the simple conversion, an improved algorithm using CHIANTI spectral models has been developed to process the XUV Photometer System (XPS) measurements with its broadband photometers. Model spectra representative of quiet Sun, active region, and flares are combined to match the signals from the XPS and produce spectra from 0.1 to 40 nm in 0.1-nm intervals for the XPS Level 4 data product. The two XPS instruments are aboard NASA's Solar Radiation and Climate Experiment (SORCE) and Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) satellites. In addition, the XPS responsivities have been updated for the latest XPS data processing version. The new XPS results are consistent with daily variations from the previous simple conversion technique used for XPS and are also consistent with spectral measurements made at wavelengths longer than 27 nm. Most importantly, the XPS flare variations are reduced by factors of 2 -4 at wavelengths shorter than 14 nm and are more consistent, for the first time, with atmospheric response to solar flares. Along with the details of the new XPS algorithm, several comparisons to dayglow and photoelectron measurements and model results are also presented to help verify the accuracy of the new XUV irradiance spectra.

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Section: Discussionmentioning

confidence: 99%

XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models

et al. 2008

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“…The Solar Patrol mission is planned to fly in 2005–2006 aboard the Russian part of the International Space Station (ISS) [ Avahyan and Kuvaldin , 2000], and it consists of three instruments to measure the solar XUV and EUV irradiance from 0.14 to 153 nm. The SOL‐ACES is planning to fly in 2005–2006 as part of the ESA part of the ISS [ Wienhold et al , 2000], and it will measure the solar irradiance from 17 to 220 nm using grating spectrometers. The SDO EVE will measure the solar EUV irradiance from 0.1 to 105 nm with 0.1 nm spectral resolution longward of 5 nm and is expected to be launched in 2008.…”

Section: Summary and Future Workmentioning

confidence: 99%

Solar EUV Experiment (SEE): Mission overview and first results

et al. 2005

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[1] The Solar EUV Experiment (SEE) is one of four scientific instruments on the NASA Thermosphere Ionosphere Mesosphere Energetics Dynamics (TIMED) spacecraft, which has been simultaneously observing the Sun and Earth's upper atmosphere since January 2002. The SEE instrument measures the irradiance of the highly variable, solar extreme ultraviolet (EUV) radiation, one of the major energy sources for the upper atmosphere. The primary SEE data product is the solar spectral irradiances from 0.1 to 194 nm in 1 nm intervals that are fundamental for the TIMED mission's investigation of the energetics in the tenuous, but highly variable, layers of the Earth's atmosphere above 60 km. The TIMED mission began normal operations on 22 January 2002, a time when the Sun displayed maximum levels of activity for solar cycle 23, and has provided daily measurements as solar activity has declined to moderate levels. Solar irradiance variability observed by SEE during the 2 years of the TIMED prime mission includes a variety of moderate and large flares over periods of seconds to hours and dozens of solar rotational cycles over a typical period of 27 days. The SEE flare measurements provide important, new results because of the simultaneous spectral coverage from 0.1 to 194 nm, albeit limited temporal coverage due to its 3% duty cycle. In addition, the SEE measurements reveal important, new results concerning phase shifts of 2-7 days in the intermediate-term variations between different UV wavelengths that appear to be related to their different center-to-limb variations. The new solar EUV irradiance time series from SEE are also important in filling the ''EUV Hole,'' which is the gap in irradiance measurements in the EUV spectrum since the 1980s. The solar irradiances measured by SEE (Version 7, released July 2004) are compared with other measurements and predictions from models of the solar EUV irradiance. While the measurement comparisons show reasonable agreement, there are significant differences between SEE and some of the models in the EUV range. The data processing algorithms and calibrations are also discussed.

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“…In recent years there has been a sharp increase in the interest in and need for monitoring of solar activity and its effects in phenomena on Earth. These problems are under investigation also in the frame of the international TIGER (Thermospheric/Ionospheric GEospheric Research) Program [15][16][17][18]. Although the first impact of space weather on the distortion of telegraph communication was recorded in 1860, there is now increasing interest in the societal impact of the solar and geomagnetic activities.…”

Section: The Creation Of the Space Solar Patrol Apparatusmentioning

confidence: 99%

Space Solar Patrol data and changes in weather and climate, including global warming

Avakyan¹,

Baranova²,

Леонов³

et al. 2010

Meas. Sci. Technol.

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In this paper, the results obtained during the execution of several ISTC projects are presented. The general aim of these projects has been the study of global changes in the environment, connected with solar activity. A brief description of the optical apparatus of the Space Solar Patrol (SSP) developed and built in the framework of the ISTC projects 385, 385.2, 1523 and 2500 is given. The SSP is intended for permanent monitoring of spectra and absolute fluxes of soft x-ray and extreme ultraviolet (x-ray/EUV) radiation from the full disk of the Sun which ionizes the upper atmosphere of the Earth. Permanent solar monitoring in the main part of the ionizing radiation spectra 0.8-115 (119) nm does not exist. The apparatus of the SSP was developed in the years 1996-2005 with multiyear experience of developing such apparatus in S I Vavilov State Optical Institute. The basis of this apparatus is the use of unique detectors of ionizing radiation-open secondary electron multipliers, which are 'solar blind' to near UV, visible and IR radiation from the Sun, and new methodology of these solar spectroradiometric absolute measurements. The prospects are discussed of using the SSP data for the investigation and forecast of the influence of solar variability on the weather and climate including global warming and also on the biosphere including human beings (proposal 3878).

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The solar package on ISS: SOL-ACES

Cited by 6 publications

References 4 publications

XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models

XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models

Solar EUV Experiment (SEE): Mission overview and first results

Space Solar Patrol data and changes in weather and climate, including global warming

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