Solar cycle minimum measurements of the solar extreme ultraviolet spectral irradiance on 14 April 2008

Chamberlin, Phillip C.; Woods, Thomas N.; Crotser, David A.; Eparvier, F. G.; Hock, R. A.; Woodraska, D.

doi:10.1029/2008gl037145

Cited by 57 publications

(51 citation statements)

References 15 publications

(17 reference statements)

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“…These results are very similar to those presented by Chamberlin et al (2009). This latest irradiance result with the prototype EVE includes the post-flight calibrations, which provided improvements especially for the higher-order corrections.…”

Section: Megs a And Bsupporting

confidence: 79%

“…No significant degradation was found between the pre-and post-flight calibrations. The main difference between this spectrum and that reported by Chamberlin et al (2009) …”

Section: Megs a And Bcontrasting

confidence: 39%

“…While the focus of this paper is on the calibration of the EVE instruments to be flown on SDO, final calibration results for the prototype EVE instrument flown on a NASA sounding rocket in 2008 are included for comparison. Some early calibration results for MEGS are presented by Chamberlin et al ( , 2009). …”

Section: Megs a And B Calibrationmentioning

confidence: 99%

See 2 more Smart Citations

Extreme Ultraviolet Variability Experiment (EVE) Multiple EUV Grating Spectrographs (MEGS): Radiometric Calibrations and Results

Hock

Chamberlin

Woods

et al. 2010

The Solar Dynamics Observatory

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The NASA Solar Dynamics Observatory (SDO), scheduled for launch in early 2010, incorporates a suite of instruments including the Extreme Ultraviolet Variability Experiment (EVE). EVE has multiple instruments including the Multiple Extreme ultraviolet Grating Spectrographs (MEGS) A, B, and P instruments, the Solar Aspect Monitor (SAM), and the Extreme ultraviolet SpectroPhotometer (ESP). The radiometric calibration of EVE, necessary to convert the instrument counts to physical units, was performed at the National Institute of Standards and Technology (NIST) Synchrotron Ultraviolet Radiation Facility (SURF III) located in Gaithersburg, Maryland. This paper presents the results and derived accuracy of this radiometric calibration for the MEGS A, B, P, and SAM instruments, while the calibration of the ESP instrument is addressed by Didkovsky et al. (Solar Phys., 2010, doi:10.1007. In addition, solar measurements that were taken on 14 April 2008, during the NASA 36.240 sounding-rocket flight, are shown for the prototype EVE instruments.

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Section: Megs a And Bsupporting

confidence: 79%

“…No significant degradation was found between the pre-and post-flight calibrations. The main difference between this spectrum and that reported by Chamberlin et al (2009) …”

Section: Megs a And Bcontrasting

confidence: 39%

See 1 more Smart Citation

Extreme Ultraviolet Variability Experiment (EVE) Multiple EUV Grating Spectrographs (MEGS): Radiometric Calibrations and Results

Hock

Chamberlin

Woods

et al. 2010

The Solar Dynamics Observatory

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“…Fig. 4 shows the synthetic spectrum calculated with the SRPM system in spherical symmetry compared to the observed spectrum measured with the EVE rocket instrument during a calibration flight on April 14, 2008 (Chamberlin et al 2009). For details on the spectral synthesis see Haberreiter & Fontenla (2009).…”

Section: Ssi Variations In the Euvmentioning

confidence: 99%

Mechanisms for total and spectral solar irradiance variations

Haberreiter

2009

Proc. IAU

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Abstract. The total and spectral irradiance varies over short time scales, i.e. from days to months, and longer time scales from years to decades, centuries, and beyond. In this talk we review the current understanding of irradiance changes from days to decades. We present the current status of observations and discuss proposed reconstruction approaches to understand these variations. The main question that ultimately needs to be answered is what are the physical processes that could explain the enhanced heating of the photosphere, chromosphere, transition region, and corona, leading to a change in the solar radiative output at various wavelengths. As semi-empirical models allow us to reproduce the solar spectrum over a broad wavelength range, they offer a powerful tool to determine the energy necessary to heat certain layers and at the same time balance the radiative losses.

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“…The wavelength coverage of all instruments is shown in Figure 3, along with the solar-cycle minimum spectrum obtained with the prototype EVE onboard a sounding rocket flight on 14 April 2008 (Chamberlin et al, 2009). Eparvier et al (2004), Crotser et al (2004Crotser et al ( , 2007, , Didkovsky et al (2007Didkovsky et al ( , 2010, and Hock et al (2010) provide details of the optical designs for the EVE instruments, but a brief overview of the instruments is included here.…”

Section: Eve Instrumentationmentioning

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 cycle minimum measurements of the solar extreme ultraviolet spectral irradiance on 14 April 2008

Cited by 57 publications

References 15 publications

Extreme Ultraviolet Variability Experiment (EVE) Multiple EUV Grating Spectrographs (MEGS): Radiometric Calibrations and Results

Extreme Ultraviolet Variability Experiment (EVE) Multiple EUV Grating Spectrographs (MEGS): Radiometric Calibrations and Results

Mechanisms for total and spectral solar irradiance variations

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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