The LYRA Instrument Onboard PROBA2: Description and In-Flight Performance

Dominique, Marie; Hochedez, J.‐F.; Schmutz, W.; Dammasch, I. E.; Шапиро, А. И.; Kretzschmar, M.; Zhukov, A. N.; Gillotay, D.; Stockman, Yvan; BenMoussa, A.

doi:10.1007/s11207-013-0252-5

Cited by 66 publications

(72 citation statements)

References 22 publications

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“…The passbands of the filters and their accompanying widths were chosen to maximise their scientific value. The 210 nm channel, measuring the Herzberg continuum, has the same spectral window as that on PROBA2/LYRA (Hochedez et al 2006;Dominique et al 2013). However, while LYRA uses experimental diamond detectors (BenMoussa et al 2009), PREMOS utilises classical silicon detectors for all channels.…”

Section: Premos Instrument Descriptionmentioning

confidence: 99%

“…The first is to rely on redundant systems in which rarely exposed spectral channels are used to periodically correct the degradation of the operational channel. This method is used for most of the radiometers such as SoHO/VIRGO, PICARD/PREMOS, and PROBA2/LYRA (Hochedez et al 2006;Dominique et al 2013). The second option is to use reference data, such as periodic rocket launches of a clone instrument, or stable external sources, such as selected stars (in the case of the SOLSTICE I and II instruments) or calibrated lamps (in the case of the SOLSPEC instrument).…”

Section: Introductionmentioning

confidence: 99%

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Solar irradiance observations with PREMOS filter radiometers on the PICARD mission: In-flight performance and data release

Cessateur

Schmutz

Wehrli

et al. 2016

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Context. The PREcision Monitoring Sensor (PREMOS) is a solar radiometer on board the French PICARD mission that was launched in June 2010 and decommissioned in April 2014. Aims. The PREMOS radiometer obtains solar irradiance measurements in specific spectral windows in the UV, visible, and nearinfrared. In this paper, the PREMOS data and calibration methods are presented. Methods. Using back-up channels, the degradation can theoretically be assessed to correct operational channels. However, a strong degradation within all PREMOS channels requires the application of additional methods, namely using back-up channels and assessing the degradation via a proxy-based model. Results. The corrected Level 3 PREMOS data are then used in different contexts in order to be validated. First, the signature of the p-mode are retrieved from the PREMOS data. The Venus transit allows us to empirically determine the intrinsic noise level within the PREMOS high cadence data for the visible and near-infrared channels. We then compare the PREMOS data directly to other data sets, namely from the SOLar-STellar Irradiance Comparison Experiment (SOLSTICE) and the Solar Irradiance Monitor (SIM) instruments on board the SOlar Radiation and Climate Experiment (SORCE) spacecraft. Regarding the UV channels, we found an excellent correlation over the lifetime of the PREMOS mission. The ratio between SORCE and PREMOS observations is always less than 1%. Regarding the SSI measurements in the visible and near-infrared, a comparison of short-term variations (i.e. 27-day modulation) shows a rather good correlation by taking into consideration the intrinsic noise within both SIM and PREMOS observations.

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Section: Premos Instrument Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Solar irradiance observations with PREMOS filter radiometers on the PICARD mission: In-flight performance and data release

Cessateur

Schmutz

Wehrli

et al. 2016

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“…Our analysis is based on data from The Atmospheric Imaging Assembly (AIA; Boerner et al 2012) instrument on board the Solar Dynamics Observatory (SDO), the Large Yield Radiometer (LYRA; Dominique et al 2013), and The Sun Watcher with Active Pixel System detector and image Processing (SWAP) telescope Halain et al 2013), both on board PROBA2. Level 1 data are used for both the AIA and the SWAP imagers.…”

Section: Observationsmentioning

confidence: 99%

“…Additional calibration rocket flights will allow us to update the AIA instrument spectral calibration curve (Boerner et al 2012). Level 3 data is used for the PROBA2 radiometer which is fully radiometrically calibrated; the data is then averaged over one minute (Dominique et al 2013).…”

Section: Observationsmentioning

confidence: 99%

“…It must be noted, however, that since the beginning of the mission, channel 3 has experienced a stronger degradation than channel 4, which has resulted in a progressive rejection of the longer wavelengths of the channel, making it more similar to channel 4 from the spectral point of view (Kretzschmar et al 2012). Dominique et al (2013) describes additional details of the effects of the degradation on the individual channels of the LYRA instrument and discusses the algorithm used to correct for the instrument degradation. The characterization of the degradation of in-orbit EUV filters and detectors is of great interest for any data analysis, especially when applying comparative analysis.…”

Section: Observationsmentioning

confidence: 99%

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Segmentation of coronal features to understand the solar EUV and UV irradiance variability

Kumara

Kariyappa

Zender

et al. 2013

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Context. The study of solar irradiance variability is of great importance in heliophysics, the Earth's climate, and space weather applications. These studies require careful identifying, tracking and monitoring of active regions (ARs), coronal holes (CHs), and the quiet Sun (QS). Aims. We studied the variability of solar irradiance for a period of two years (January 2011-December 2012) using the Large Yield Radiometer (LYRA), the Sun Watcher using APS and image Processing (SWAP) on board PROBA2, and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). Methods. We used the spatial possibilistic clustering algorithm (SPoCA) to identify and segment coronal features from the EUV observations of AIA. The AIA segmentation maps were then applied on SWAP images, and parameters such as the intensity, fractional area, and contribution of ARs/CHs/QS features were computed and compared with the full-disk integrated intensity and LYRA irradiance measurements. Results. We report the results obtained from SDO/AIA and PROBA2/SWAP images taken from January 2011 to December 2012 and compare the resulting integrated full-disk intensity with PROBA2/LYRA irradiance. We determine the contributions of the segmented features to EUV and UV irradiance variations. The variations of the parameters resulting from the segmentation, namely the area, integrated intensity, and relative contribution to the solar irradiance, are compared with LYRA irradiance. We find that the active regions have a great impact on the irradiance fluctuations. In the EUV passbands considered in this study, the QS is the greatest contributor to the solar irradiance, with up to 63% of total intensity values. Active regions, on the other hand, contribute to about 10%, and off-limb structures to about 24%. We also find that the area of the features is highly variable suggesting that their area has to be taken into account in irradiance models, in addition to their intensity variations. Conclusions. We successfully show that the feature extraction allows us to use EUV telescopes to measure irradiance fluctuations and to quantify the contribution of each part to the EUV spectral solar irradiance observed with a calibrated radiometer. This study also shows that SPoCA is viable, and that the segmentation of images can be a useful tool. We also provide the measurement correlation between SWAP and AIA during this analysis.

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Interplanetary coronal mass ejection observed at STEREO‐A, Mars, comet 67P/Churyumov‐Gerasimenko, Saturn, and New Horizons en route to Pluto: Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

et al. 2017

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We discuss observations of the journey throughout the Solar System of a large interplanetary coronal mass ejection (ICME) that was ejected at the Sun on 14 October 2014. The ICME hit Mars on 17 October, as observed by the Mars Express, Mars Atmosphere and Volatile EvolutioN Mission (MAVEN), Mars Odyssey, and Mars Science Laboratory (MSL) missions, 44 h before the encounter of the planet with the Siding‐Spring comet, for which the space weather context is provided. It reached comet 67P/Churyumov‐Gerasimenko, which was perfectly aligned with the Sun and Mars at 3.1 AU, as observed by Rosetta on 22 October. The ICME was also detected by STEREO‐A on 16 October at 1 AU, and by Cassini in the solar wind around Saturn on the 12 November at 9.9 AU. Fortuitously, the New Horizons spacecraft was also aligned with the direction of the ICME at 31.6 AU. We investigate whether this ICME has a nonambiguous signature at New Horizons. A potential detection of this ICME by Voyager 2 at 110–111 AU is also discussed. The multispacecraft observations allow the derivation of certain properties of the ICME, such as its large angular extension of at least 116°, its speed as a function of distance, and its magnetic field structure at four locations from 1 to 10 AU. Observations of the speed data allow two different solar wind propagation models to be validated. Finally, we compare the Forbush decreases (transient decreases followed by gradual recoveries in the galactic cosmic ray intensity) due to the passage of this ICME at Mars, comet 67P, and Saturn.

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The LYRA Instrument Onboard PROBA2: Description and In-Flight Performance

Cited by 66 publications

References 22 publications

Solar irradiance observations with PREMOS filter radiometers on the PICARD mission: In-flight performance and data release

Solar irradiance observations with PREMOS filter radiometers on the PICARD mission: In-flight performance and data release

Segmentation of coronal features to understand the solar EUV and UV irradiance variability

Interplanetary coronal mass ejection observed at STEREO‐A, Mars, comet 67P/Churyumov‐Gerasimenko, Saturn, and New Horizons en route to Pluto: Comparison of its Forbush decreases at 1.4, 3.1, and 9.9 AU

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