The Solar Ultraviolet Spectral Irradiance Monitor (SUSIM) experiment on board the Upper Atmosphere Research Satellite (UARS)

Brueckner, G. E.; Edlow, Kenneth; Floyd, L.; Lean, J.; Vanhoosier, M. E.

doi:10.1029/93jd00410

Cited by 181 publications

(85 citation statements)

References 22 publications

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“…The differences between data sets arise from many factors such as instrument resolution and analysis techniques, however; it appears that as long as the analysis of each of the data sets is consistent, then individual data sets will correlate very well with the other data sets [Hall and Anderson, 1988;de Toma et al, 1997;Cebula and DeLand, 1998;White et al, 1998]. This property of the Mg II core-to-wing ratio has been used to create long time series from multiple satellites [e.g., DeLand and Cebula, 1993;Donnelly et al, 1994;Viereck and Puga, 1999].…”

Section: Calculating the Mg II Core-to-wing Ratiomentioning

confidence: 99%

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A composite Mg II index spanning from 1978 to 2003

Viereck¹,

et al. 2004

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[1] The Mg II core-to-wing ratio is a measure of solar chromospheric variability. The Mg II Index, formed by combining various Mg II core-to-wing data sets, has been used in EUV, UV, and total solar irradiance models. It is one of the longest records of solar variability reaching back nearly 25 years. We present a single, continuous time series of the Mg II core-to-wing ratio extending from November 1978 to the present. The Mg II core-to-wing ratio is a measurement that is well suited to the creating of a single time series despite the fact that the seven different instruments measuring the solar flux near 280 nm have different spectral resolutions and sample rates. The Upper Atmosphere Research Satellite (UARS) Solar Ultraviolet Spectral Irradiance Monitor (SUSIM), UARS Solar Stellar Irradiance Comparison Experiment (SOLSTICE), ERS-2/Global Ozone Monitoring Experiment (GOME) and five NOAA solar backscatter ultraviolet data sets were used. Initially, the best data sets were selected to create a time series spanning from 1978 to the present. Then the gaps in the record were filled with data from various other Mg II data sets. Where no alternate data were available, a cubic spline function was used to bridge the missing data. In some cases the data gaps were too long for reasonable spline fits (more than 5 days), and for these gaps the F10.7 cm flux data were scaled to fill the gaps. Thus a continuous, uninterrupted time series of the Mg II core-to-wing ratio was created. The final Mg II time series is compared with other solar activity indices, such as the F10.7, He I 1083, and Sunspot number, to look for trends in the Mg II data.

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Section: Calculating the Mg II Core-to-wing Ratiomentioning

confidence: 99%

“…[33] NASA launched the UARS satellite in September 1991 with SUSIM [Brueckner et al, 1993;Floyd et al, 1998] and SOLSTICE Woods et al, 1993] instruments on board. The SUSIM instrument typically operates with 1.1 nm resolution (similar to the SBUV instruments).…”

Section: A12 Uars Susim and Solstice Datamentioning

confidence: 99%

A composite Mg II index spanning from 1978 to 2003

Viereck¹,

et al. 2004

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“…Would the solar cycle variability be a simple amplification of the rotational variability shown in the figure? If so, twocomponent models with a quiet Sun and active region component may suffice to describe the solar cycle (Lean 1987). A more complicated relation between intermediate and longterm variability requires additional terms, for example an active network component, to fully describe the solar variations.…”

Section: Discussionmentioning

confidence: 99%

“…We continue to crosscalibrate the SOLSTICE data with the data from the UARS SUSIM instrument (Brueckner et al 1993) and the ATLAS SSBUV and SUSIM instruments. Our current validation efforts indicate that SOLSTICE absolute accuracy is ±2% for wavelengths longward of 200 nm and ±5% for shorter wavelengths.…”

Section: Solar Observationsmentioning

confidence: 99%

Irradiance Observations from the UARS/SOLSTICE Experiment

Rottman¹,

Woods²,

White³

et al. 1994

International Astronomical Union Colloquium

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The Solar/Stellar Irradiance Comparison Experiment (SOLSTICE) is one of the two ultraviolet spectrometers on the Upper Atmosphere Research Satellite (UARS) measuring the full disk solar irradiance. This spectrometer covers the spectral range of 119 to 421 nm and typically makes ten full spectral scans per day. The instrument was designed to monitor changes in the solar radiation with a relative accuracy of better than 1%. To achieve this goal the spectrometer makes repeated observations of a number of bright blue stars; stars that individually should vary by only small fractions of a percent over time periods of thousands of years. The calibration stars are observed with the same optics and detectors used for the solar observations and any drift in the instrument response is directly determined by changes in the ensemble average flux from these calibration stars. The instrument performance and calibration are described and solar data from the first year of the UARS mission are presented. These UARS data show significant solar activity during late 1991 and early 1992 and then clearly mark a decrease as we move off the maximum of solar cycle 22. We are optimistic that an extended UARS mission, perhaps as long as ten years, is now possible.

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“…Another strategy is to develop robust instruments containing built-in relative calibration units with redundant optical elements. Ultraviolet SSI measurements from space had important contributions from instruments such as the Solar Backscatter UltraViolet (SBUV) radiometer flown on weather satellites (Markert 1975); the Solar Ultraviolet Spectral Irradiance Monitor (SUSIM; Brueckner et al 1993); and the SOLar STellar Irradiance Comparison Experiment (SOLSTICE; Rottman et al 2001) experiments on board the Upper Atmosphere Research Satellite (UARS), which made SSI measurements from Lyman α (Ly-α) to 400 nm during solar cycle 22. Since 2003 measurements have been made by the new SOLSTICE instrument and the Solar Irradiance Monitor (SIM) on board the Solar Radiation A&A 600, A21 (2017) and Climate Experiment (SORCE) platform (Rottman 2005), and also by the SCanning Imaging Absorption spectroMeter for Atmospheric CHartographY (SCIAMACHY) instrument (Skupin et al 2005).…”

Section: Introductionmentioning

confidence: 99%

SOLAR/SOLSPEC mission on ISS: In-flight performance for SSI measurements in the UV

Bolsée

Pereira

Gillotay

et al. 2017

A&A

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Context. The SOLar SPECtrum (SOLSPEC) experiment is part of the Solar Monitoring Observatory (SOLAR) payload, and has been externally mounted on the Columbus module of the International Space Station (ISS) since 2008. SOLAR/SOLSPEC combines three absolutely calibrated double monochromators with concave gratings for measuring the solar spectral irradiance (SSI) from 166 nm to 3088 nm. This physical quantity is a key input for studies of climatology, planetary atmospheres, and solar physics. Aims. A general description of the instrument is given, including in-flight operations and performance of the ultraviolet (UV) channel from 175 nm to 340 nm. Methods. We developed a range of processing and correction methods, which are described in detail. For example, methods for correcting thermal behavior effects, instrument linearity, and especially the accuracy of the wavelength and absolute radiometric scales have been validated by modeling the standard uncertainties. Results. The deliverable is a quiet Sun UV reference solar spectrum as measured by SOLAR/SOLSPEC during the minimum of solar activity prior to cycle 24. Comparisons with other instruments measuring SSI are also presented.

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The Solar Ultraviolet Spectral Irradiance Monitor (SUSIM) experiment on board the Upper Atmosphere Research Satellite (UARS)

Cited by 181 publications

References 22 publications

A composite Mg II index spanning from 1978 to 2003

A composite Mg II index spanning from 1978 to 2003

Irradiance Observations from the UARS/SOLSTICE Experiment

SOLAR/SOLSPEC mission on ISS: In-flight performance for SSI measurements in the UV

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