Solar extreme ultraviolet irradiance observations from GOES: design characteristics and initial performance

Viereck, R. A.; Hanser, Fred; Wise, J. O.; Guha, S.; Jones, Andrew; McMullin, D. R.; Plunket, Simon; Strickland, D. J.; Evans, Scott

doi:10.1117/12.734886

Cited by 30 publications

(18 citation statements)

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“…For the reasons mentioned above, these sensors, as well as other previous solar irradiance sensors, have met with limited success, particularly in the 40-90 nm spectral region. 2,3, 4 There are several spaceborne instruments that now perform solar imaging in narrow spectral bands at 17.1 nm, 19.5 nm, and 30.4 nm, using on-axis telescopes with spectrally-selective coatings on their mirrors, including the Extreme ultraviolet Imaging Telescope (EIT) on SOHO and the Extreme Ultra-Violet Imager (EUVI) on STEREO. The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO), scheduled for launch in late 2009, will perform solar imaging in narrow spectral bands at 17.1 nm, 19.3 nm, and 30.4 nm.…”

Section: Measurement Requirements and Previous Sensorsmentioning

confidence: 99%

Zone plate EUV solar irradiance monitor

et al. 2009

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Measuring the solar extreme ultraviolet (EUV) irradiance is a high priority for space weather and upper atmospheric research. We have designed and fabricated a sensor to measure the total solar irradiance in the extremely variable 17.1-19.5 nm spectral band that contains numerous Fe emission lines and we are developing another similar sensor for the 30.4 nm He II spectral line. Each of these sensors uses a 4 mm diameter zone plate (ZP) to focus the in-band solar radiation onto a small pinhole in front of a detector. The focal length of a ZP is inversely proportional to wavelength, and the pinhole's diameter is sufficient to admit the in-band radiation from the full solar disk and inner corona. A 2 mm diameter central occulting disk minimizes the undiffracted (0-order) and out-of-band radiation that reaches the pinhole. Two thin Al film filters, one in front of the ZP and one deposited on the detector, are virtually opaque to wavelengths longer than EUV and prevent the detector from responding to most of the solar spectrum. A ZP has a number of advantages over a diffraction grating. Because it focuses in-band radiation, a ZP allows the detector to be smaller than the aperture, reducing both the dark current and the out-of-band response. The circular symmetry of the ZP eliminates both the polarization sensitivity and the shift in the spectral band with field angle that are intrinsic to a linear grating. The optical assembly is contained in a very small volume. We are planning to fly the Fe-band sensor as a secondary payload on NRL's VERIS sounding rocket solar measurement mission in the near future and are investigating the feasibility of flying both sensors on a future CubeSat mission.

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Section: Measurement Requirements and Previous Sensorsmentioning

confidence: 99%

Zone plate EUV solar irradiance monitor

et al. 2009

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“…The Geostationary Operational Environmental Satellite (GOES-13) carries a multi-channel Extreme Ultraviolet Sensor (EUVS) whose solar measurements within this spectral region are new to the GOES program (Viereck et al, 2007). The observed intervals (identified below) actually fall within both the X-ray ultraviolet (XUV) region from 0.1 to 10 nm and the extreme ultraviolet (EUV) region from 10 to 121 nm.…”

Section: Introductionmentioning

confidence: 99%

Early Observations by the GOES-13 Solar Extreme Ultraviolet Sensor (EUVS)

et al. 2010

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NOAA's GOES-13 satellite, launched in May 2006, includes a new solar sensor, called EUVS (Extreme UltraViolet Sensor), that measures energy fluxes in five broad-band spectral channels that span the region from 1 to 130 nm. Here, we report on measurements made during the mission's six-month post-launch test (PLT) period which provided nearly continuous observations from August through November 2006 and the recording of an X9 flare that occurred on 5 December 2006. In this paper, we present a calibration model for the GOES EUVS that incorporates the effects of pointing offsets, cross-disk radiance variability (radiance refers to partial-disk emission), and changes to assumed spectral shapes. Appendices are included that report on the sensitivity to these effects. The main body of the paper gives a description of the model and data recorded during the PLT period. Comparisons are made with time-coincident measurements from TIMED/SEE (Version 10.02), SOHO/SEM, and SORCE/ SOLSTICE for the time period August-November. Comparisons are made with SORCE/XPS for the 5 December flare. In general, there is agreement among the data sets within expected measurement uncertainties. There will be a series of EUVSs extending into the next generation of GOES (starting with GOES-13). The initial performance of GOES-13 EUVS, including 5-channel measurements approximately every 11 s on a nearly continuous basis, suggests that the EUVS series will play a key role over the next many years in monitoring solar EUV variability.

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“…The GOES/EUVS observations are expected to be operational during the SDO mission and to continue on past the SDO mission using a series of GOES satellites. The GOES/EUVS will only observe a few key EUV emissions (Viereck et al, 2007;Eparvier et al, 2009), so the EVE-established relationships of these GOES EUV bands to all other EUV wavelengths will be an important component for the future EUV irradiance-modeling effort.…”

Section: Solar Irradiance Modelsmentioning

confidence: 99%

“…The extracted emission lines are total irradiances over the lines including the background. There are several broadbands including EVE's photometer measurements and several wavelength bands extracted from the MEGS spectra that simulate bands from other instruments, such as AIA, SOHO/Solar EUV Monitor (SEM) (Judge et al, 1998), and GOES/EUV Sensor (EUVS) (Viereck et al, 2007). For these other instrument bands, their normalized responsivity profiles are convolved with the MEGS spectrum so that the EVE equivalent bands can be more directly compared for calibration and validation purposes.…”

Section: Eve Levelmentioning

confidence: 99%

Extreme Ultraviolet Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO): Overview of Science Objectives, Instrument Design, Data Products, and Model Developments

Woods

Eparvier

Hock

et al. 2010

The Solar Dynamics Observatory

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The highly variable solar extreme ultraviolet (EUV) radiation is the major energy input to the Earth's upper atmosphere, strongly impacting the geospace environment, affecting satellite operations, communications, and navigation. The Extreme ultraviolet Variability Experiment (EVE) onboard the NASA Solar Dynamics Observatory (SDO) will measure the solar EUV irradiance from 0.1 to 105 nm with unprecedented spectral resolution (0.1 nm), temporal cadence (ten seconds), and accuracy (20%). EVE includes several irradiance instruments: The Multiple EUV Grating Spectrographs (MEGS)-A is a grazingincidence spectrograph that measures the solar EUV irradiance in the 5 to 37 nm range with 0.1-nm resolution, and the MEGS-B is a normal-incidence, dual-pass spectrograph that measures the solar EUV irradiance in the 35 to 105 nm range with 0.1-nm resolution. To provide MEGS in-flight calibration, the EUV SpectroPhotometer (ESP) measures the solar EUV irradiance in broadbands between 0.1 and 39 nm, and a MEGS-Photometer measures the Sun's bright hydrogen emission at 121.6 nm. The EVE data products include a near real-time space-weather product (Level 0C), which provides the solar EUV irradiance in specific bands and also spectra in 0.1-nm intervals with a cadence of one minute and with a time delay of less than 15 minutes. The EVE higher-level products are Level 2 with the solar EUV irradiance at higher time cadence (0.25 seconds for photometers and ten seconds for spectrographs) and Level 3 with averages of the solar irradiance over a day and over each one-hour period. The EVE team also plans to advance existing models of solar EUV irradiance and to operationally use the EVE measurements in models of Earth's ionosphere and thermosphere. Improved understanding of the evolution of solar flares and extending the various models to incorporate solar flare events are high priorities for the EVE team.

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Solar extreme ultraviolet irradiance observations from GOES: design characteristics and initial performance

Cited by 30 publications

References 0 publications

Zone plate EUV solar irradiance monitor

Zone plate EUV solar irradiance monitor

Early Observations by the GOES-13 Solar Extreme Ultraviolet Sensor (EUVS)

Extreme Ultraviolet Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO): Overview of Science Objectives, Instrument Design, Data Products, and Model Developments

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