ASPIICS: an externally occulted coronagraph for PROBA-3: Design evolution

Renotte, Étienne; Baston, Elena Carmen; Бемпорад, А.; Capobianco, Gerardo; Cernica, I.; Darakchiev, Radoslav; Denis, François; Desselle, Richard; Vos, Lieve De; Fineschi, Silvano; Focardi, M.; Górski, Tomasz; Graczyk, Rafał; Halain, Jean-Philippe; Hermans, Aline; Jackson, Carl; Kintziger, Christian; Kosiec, J.; Kranitis, N.; Landini, F.; Lédl, Vít; Massone, G.; Mazzoli, Alexandra; Melich, Radek; Mollet, Dominique; Mosdorf, M.; Nicolini, G.; Nicula, B.; Orleański, P.; Palau, Marie-Catherine; Pancrazzi, M.; Paschalis, A.; Peřestý, R.; Plesseria, Jean-Yves; Rataj, M.; Romoli, M.; Thizy, Cédric; Thome, Michel; Tsinganos, K.; Wodnicki, Ryszard; Walczak, Tomasz; Zhukov, A. N.

doi:10.1117/12.2056784

Cited by 16 publications

(7 citation statements)

References 2 publications

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“…The application of the algorithm is not only limited to CMEs, but also to analyse the dynamics of streamers, blobs, current sheets/rays, etc... in this FOV, and long-term coronal studies (Lamy et al, 2020a,b). The recently launched Multi Element Telescope for Imaging and Spectroscopy (METIS) onboard Solar Orbiter (Müller et al, 2020), and future space-based missions including the Visible Emission Line Coronagraph (VELC: Raghavendra Prasad et al, 2017;Banerjee, Patel, and Pant, 2017) onboard Aditya-L1 (Seetha and Megala, 2017), and the Association of Spacecraft for Polarimetric and the Imaging Investigation of the Corona of the Sun (ASPIICS: Renotte et al, 2014) of the Project for Onboard Autonomy-3 (PROBA-3) will also observe the inner corona. The application of SiRGraF on their data will be helpful to bring out processes occurring in the inner corona thereby improving our understanding of the same.…”

Section: Discussionmentioning

confidence: 99%

A Simple Radial Gradient Filter for Batch-Processing of Coronagraph Images

Patel,

Majumdar,

Pant

et al. 2022

Preprint

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Images of the extended solar corona, as observed by white-light coronagraphs as observed by different white-light coronagraphs include the K-and F-corona and suffer from a radial variation in intensity. These images require separation of the two coronal components with some additional image-processing to reduce the intensity gradient and analyse the structures and processes occurring at different heights in the solar corona within the full field of view. Over the past few decades, coronagraphs have been producing enormous amounts of data, which will be continued with the launch of new telescopes. To process these bulk coronagraph images with steep radial-intensity gradients, we have developed an algorithm: Simple Radial Gradient Filter (SiRGraF). This algorithm is based on subtracting a minimum background (F-corona) created using long duration images and then dividing the resultant by a uniform intensity gradient image to enhance the K-corona. We demonstrate the utility of this algorithm to bring out the short time-scale transient structures of the corona. SiRGraF could be used to reveal and analyse such structures. It is not suitable for quantitative estimations based on intensity. We have successfully tested the algorithm on images of the Large Angle Spectroscopic COronagraph (LASCO)-C2 onboard the Solar and Heliospheric Observatory (SOHO), and COR-2A onboard the Solar TErrestrial D. Banerjee

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Section: Discussionmentioning

confidence: 99%

A Simple Radial Gradient Filter for Batch-Processing of Coronagraph Images

Patel,

Majumdar,

Pant

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…It is worth noting that future solar missions, such as ADITYA-L1 (Seetha and Megala, 2017), PROBA-3 (Renotte et al, 2014), Solar orbiter (Müller et al, 2013), etc., will coronagraphs observing the inner corona and full disk UV imagers. This algorithm can be applied to these datasets, and will help add to improve our knowledge of CME evolution following and during their eruption.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Automated Detection of Accelerating Solar Eruptions Using Parabolic Hough Transform

et al. 2021

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“…This height is below the existing space-based white-light coronagraphs used for analysis. It is worth mentioning that future space-based missions, including Aditya-L1 (Seetha and Megala, 2017;Raghavendra Prasad et al, 2017), PROBA-3 (Renotte et al, 2014), and Solar Orbiter (Müller et al, 2013), are equipped with coronagraphs capable of observing the inner corona, a region with limited observations from existing space-based instruments. These instruments will be helpful in studies similar to this work to identify the white-light counterparts of the radio imaging of the shock origin, thereby improving understanding of such phenomenon.…”

Section: Discussionmentioning

confidence: 99%

Imaging and Spectral Observations of a Type-II Radio Burst Revealing the Section of the CME-Driven Shock That Accelerates Electrons

et al. 2021

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We report on a multi-wavelength analysis of the 26 January 2014 solar eruption involving a coronal mass ejection (CME) and a Type-II radio burst, performed by combining data from various space and ground-based instruments. An increasing standoff distance with height shows the presence of a strong shock, which further manifests itself in the continuation of the metric Type-II burst into the decameter-hectometric (DH) domain. A plot of speed versus position angle (PA) shows different points on the CME leading edge traveled with different speeds. From the starting frequency of the Type-II burst and white-light data, we find that the shock signature producing the Type-II burst might be coming from the flanks of the CME. Measuring the speeds of the CME flanks, we find the southern flank to be at a higher speed than the northern flank; further the radio contours from Type-II imaging data showed that the burst source was coming from the southern flank of the CME. From the standoff distance at the CME nose, we find that the local Alfven speed is close to the white-light shock speed, thus causing the Mach number to be small there. Also, the presence of a streamer near the southern flank appears to have provided additional favorable conditions for the generation of shock-associated radio emission. These results provide conclusive evidence that the Type-II emission could originate from the flanks of the CME, which in our study is from the southern flank of the CME.

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ASPIICS: an externally occulted coronagraph for PROBA-3: Design evolution

Cited by 16 publications

References 2 publications

A Simple Radial Gradient Filter for Batch-Processing of Coronagraph Images

A Simple Radial Gradient Filter for Batch-Processing of Coronagraph Images

Automated Detection of Accelerating Solar Eruptions Using Parabolic Hough Transform

Imaging and Spectral Observations of a Type-II Radio Burst Revealing the Section of the CME-Driven Shock That Accelerates Electrons

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