SWAP onboard PROBA 2, a new EUV imager for solar monitoring

Berghmans, D.; Hochedez, J.‐F.; Defise, J. M.; Lecat, Jean-Hervé; Nicula, B.; Slemzin, V. A.; Lawrence, G.; Katsyiannis, A. C.; Linden, R. Van der; Zhukov, A. N.; Clette, F.; Rochus, Pierre; Mazy, Emmanuel; Thibert, Tanguy; Nicolosi, P.; Pelizzo, M. G.; Schühle, U.

doi:10.1016/j.asr.2005.03.070

Cited by 83 publications

(59 citation statements)

References 6 publications

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“…This will allow the CME to emerge early enough into the coronagraph field of view when the wave is still strong. PROBA-II/SWAP (Berghmans et al, 2006) off-point EUV images which can follow the early EUV CME at much larger heights than any current EUV imager, up to 1 R above the solar limb, can also help into the wave-CME comparisons. 6.…”

Section: Future Areas Of Workmentioning

confidence: 99%

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

2012

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A major, albeit serendipitous, discovery of the SOlar and Heliospheric Observatory mission was the observation by the Extreme Ultraviolet Telescope (EIT) of large-scale Extreme Ultraviolet (EUV) intensity fronts propagating over a significant fraction of the Sun's surface. These so-called EIT or EUV waves are associated with eruptive phenomena and have been studied intensely. However, their wave nature has been challenged by non-wave (or pseudo-wave) interpretations and the subject remains under debate. A string of recent solar missions has provided a wealth of detailed EUV observations of these waves bringing us closer to resolving their nature. With this review, we gather the current state-of-art knowledge in the field and synthesize it into a picture of an EUV wave driven by the lateral expansion of the CME. This picture can account for both wave and pseudo-wave interpretations of the observations, thus resolving the controversy over the nature of EUV waves to a large degree but not completely. We close with a discussion of several remaining open questions in the field of EUV waves research.

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Section: Future Areas Of Workmentioning

confidence: 99%

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

2012

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“…11a. The SWAP telescope is a compact EUV imager onboard the PROBA2 (PRoject for Onboard Autonomy) micro-satellite, which provides coronal images at a temperature of ∼0.8 MK (Berghmans et al 2006;Halain et al 2010). The CME frontal loop shown by blue curve is clearly observed, which agrees well with the AIA 171 Å images of the low corona (Fig.…”

Section: Cmementioning

confidence: 99%

Multiwavelength observation of a large-scale flux rope eruption above a kinked small filament

Kumar

Cho

2014

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We analyzed multiwavelength observations of a western limb flare (C3.9) that occurred in AR NOAA 111465 on 30 April 2012. The high-resolution images recorded by SDO/AIA 304, 1600 Å and Hinode/SOT Hα show the activation of a small filament (rising speed ∼ 40 km s −1 ) associated with a kink instability and the onset of a C-class flare near the southern leg of the filament. The first magnetic reconnection occurred at one of the footpoints of the filament and caused the breaking of its southern leg. The filament shows unwinding motion of the northern leg and apex in counterclockwise direction and failed to erupt. A flux-rope structure (visible only in hot channels, i.e., AIA 131 and 94 Å and Hinode/SXT) appeared along the neutral line during the second magnetic reconnection that occurred above the kinked filament. The formation of the RHESSI hard X-ray source (12−25 keV) above the kinked filament and the simultaneous appearance of the hot 131 Å loops associated with photospheric brightenings (AIA 1700 Å) indicates the particle acceleration along these loops from the top of the filament. In addition, extreme ultraviolet disturbances or waves observed above the filament in 171 Å also show a close association with magnetic reconnection. The flux rope rises slowly (∼100 km s −1 ), which produces a very large twisted structure possibly through reconnection with the surrounding sheared magnetic fields within ∼15−20 min, and showed an impulsive acceleration reaching a height of about 80-100 Mm. AIA 171 and SWAP 174 Å images reveal a cool compression front (or coronal mass ejection frontal loop) surrounding the hot flux rope structure.

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“…In addition to its view from two vantage points, the EUVI will provide a substantial improvement in image resolution and image cadence over SOHO-EIT. In 2007, SWAP (Berghmans et al, 2005b) will bring advances thanks to its 1 min cadence, autonomous CME-tracking ability and concomitancy with EUVI. Its passband is centred on 17.5 nm.…”

Section: Cool Corona Imagesmentioning

confidence: 99%

Solar weather monitoring

et al. 2005

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Abstract. Space Weather nowcasting and forecasting require solar observations because geoeffective disturbances can arise from three types of solar phenomena: coronal mass ejections (CMEs), flares and coronal holes. For each, we discuss their definition and review their precursors in terms of remote sensing and in-situ observations. The objectives of Space Weather require some specific instrumental features, which we list using the experience gained from the daily operations of the Solar Influences Data analysis Centre (SIDC) at the Royal Observatory of Belgium. Nowcasting requires real-time monitoring to assess quickly and reliably the severity of any potentially geoeffective solar event. Both research and forecasting could incorporate more observations in order to feed case studies and data assimilation respectively. Numerical models will result in better predictions of geomagnetic storms and solar energetic particle (SEP) events. We review the data types available to monitor solar activity and interplanetary conditions. They come from space missions and ground observatories and range from sequences of dopplergrams, magnetograms, white-light, chromospheric, coronal, coronagraphic and radio images, to irradiance and in-situ time-series. Their role is summarized together with indications about current and future solar monitoring instruments.

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SWAP onboard PROBA 2, a new EUV imager for solar monitoring

Cited by 83 publications

References 6 publications

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

Multiwavelength observation of a large-scale flux rope eruption above a kinked small filament

Solar weather monitoring

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