Recent achievements on ASPIICS, an externally occulted coronagraph for PROBA-3

Renotte, Étienne; Buckley, Steve; Cernica, I.; Denis, François; Desselle, Richard; Vos, Lieve De; Fineschi, Silvano; Fleury-Frenette, Karl; Galano, Damien; Galy, Camille; Gillis, Jean-Marie; Graas, Estelle; Graczyk, Rafał; Horodyská, P.; Kranitis, N.; Kurowski, Michal; Ladno, Michal; Liébecq, Sylvie; Loreggia, D.; Mechmech, I.; Melich, Radek; Mollet, Dominique; Mosdorf, M.; Mroczkowski, Mateusz; O’Neill, Kevin; Patočka, Karel; Paschalis, A.; Peřestý, R.; Radzik, Bartlomiej; Rataj, M.; Salvador, Lucas; Servaye, Jean-Sébastien; Stockman, Yvan; Thizy, Cédric; Walczak, Tomasz; Zarzycka, Alicja; Zhukov, A. N.

doi:10.1117/12.2232695

Cited by 6 publications

(4 citation statements)

References 2 publications

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“…The coronagraph will cover the range of radial distances between ∼1.1 and 3 solar radii, thus providing continuous observational conditions very close to those during a total solar eclipse, but without the eects of Earth's atmosphere. AS-PIICS will provide novel solar observations capabilities to achieve two major science objectives in the area of solar physics [27,11]:…”

Section: Instrument Control Unitmentioning

confidence: 99%

From Graphs to the Science Computer of a Space Telescope

Graczyk,

Bujwan,

Darmetko

et al. 2022

Application and Theory of Petri Nets and Concurrency

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Space system engineering has to follow a rigorous design process to manage performance/risk trade-os at each development stage and possibly across several functional and organizational domains. The process is further complicated by the co-development of multiple solutions, each contributing dierently to the goal and with dierent tradeos. Moreover, the design process is iterative, involving both changing requirements and specications along the dierent ways that lead to the set goal of the mission. The above requires rigorous modeling that, in addition, must be easily extendible and maintainable across organizational units. On the example of the PROBA-3 science computer (instrument control unit, CCB DPU), we show how Petri Nets can serve as such a simple-to-maintain, holistic model, combining nite-state characterizations with dynamic system behavior caused by hardware-software interactions, to express the component-state dependent end-to-end performance characteristics of the system. The paper elaborates on how the proposed Petri-Net-modeling scheme allows for system architecture optimization that result in safely reduced technical margins and in turn substantial savings in components costs. We show that performance metrics, obtained from simulation, correlate well with the real performance characteristics of the ight model of PROBA-3's science computer.

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Section: Instrument Control Unitmentioning

confidence: 99%

From Graphs to the Science Computer of a Space Telescope

Graczyk,

Bujwan,

Darmetko

et al. 2022

Application and Theory of Petri Nets and Concurrency

Self Cite

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“…They were able to simulate the External occulter diffraction and provide us with the diffraction profile at the entrance aperture of ASPIICS. For more information on the EO diffraction simulation and its verification, see [7] (Diffraction calculation) and [8] (Diffraction simulation verification by a scaled-model). Figure 27 below shows the complete diffraction irradiance for one radius on the pupil plane.…”

Section: In-fov Straylight Source: External Occulter Diffractionmentioning

confidence: 99%

Straylight analysis on ASPIICS, PROBA-3 coronagraph

Galy

Thizy

Stockman

et al. 2019

International Conference on Space Optics — ICSO 2018

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PROBA-3 is a mission devoted to the in-orbit demonstration (IOD) of precise formation flying (F²) techniques and technologies for future ESA missions. The mission includes two spacecraft. One of them will act as an external occulter for scientific observations of the solar corona from the other spacecraft, which will hold the ASPIICS coronagraph instrument, under CSL responsibility.The ASPIICS instrument on PROBA-3 looks at the solar corona through a refractive telescope, able to select 3 different spectral bands: Fe XIV line @ 530.4nm, He I D3 line @587.7nm, and the white-light spectral band [540;570nm]. The external occulter being located at ~ 150 meters from the instrument entrance, will allow ASPIICS to observe the corona really close to the solar limb, probably closer than any internally or externally occulted coronagraph ever observed. This paper will present the straylight model and analyses carried out by CSL. A first specificity of the analysis is that the scene on the useful Field of View (FOV) is the solar corona which has a brightness dynamic range as high as 10³ between the close corona, close to 1 solar radius (Rsun), and the "distant" corona around 3RSun. The specifications are very stringent for this type of instrument. A consensus was found and will be presented regarding the expected straylight within the FOV. It will also be shown that to achieve realistic estimations it is required to take into account the exact location of the created straylight as well as the entrance field.The second specificity that had to be analyzed is that the diffraction from the solar disk by the external occulter enters the instrument un-obstructed until the internal occulter, and with a brightness 100 times higher than the close corona (~1RSun) brightness. The simulation of this diffraction as well as its propagation inside the ASPIICS telescope creating additional straylight, had to be carefully established in order to give realistic results of its impact on the performances while being actually possible to compute.

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“…The D 3 line will be observed routinely by the large coronagraph on Proba-3, the Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun (ASPIICS; see, e.g., Renotte et al 2016). ASPIICS will provide polarimetry in a narrow band centered on the D 3 line, together with one on the green Fe XIV line.…”

Section: Introductionmentioning

confidence: 99%

Helium Line Emissivities in the Solar Corona

Zanna

Storey

Badnell

et al. 2020

ApJ

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We present new collisional-radiative models (CRMs) for helium in the quiescent solar corona and predict the emissivities of the He and He + lines to be observed by DKIST, Solar Orbiter, and Proba-3. We discuss in detail the rates we selected for these models, highlighting several shortcomings we have found in previous work. As no previous complete and self-consistent coronal CRM for helium existed, we have benchmarked our largest model at a density of 10 6 cm −3 and temperature of 20,000 K against recent CRMs developed for photoionized nebulae. We then present results for the outer solar corona, using new dielectronic recombination rates we have calculated, which increase the abundance of neutral helium by about a factor of 2. We also find that all optical triplet He I lines, and in particular the well-known He I 10830 and 5876 Å lines, are strongly affected by both photoexcitation and photoionization from the disk radiation and that extensive CRMs are required to obtain correct estimates. Close to the Sun, at an electron density of 10 8 cm −3 and temperature of 1 MK, we predict the emissivity of He I 10830 Å to be comparable to that of the strong Fe XIII coronal line at 10798 Å. However, we expect the He I emissivity to sharply fall in the outer corona, with respect to Fe XIII. We confirm that the He + Lyα at 304 Å is also significantly affected by photoexcitation and is expected to be detectable as a strong coronal line up to several solar radii.

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Recent achievements on ASPIICS, an externally occulted coronagraph for PROBA-3

Cited by 6 publications

References 2 publications

From Graphs to the Science Computer of a Space Telescope

From Graphs to the Science Computer of a Space Telescope

Straylight analysis on ASPIICS, PROBA-3 coronagraph

Helium Line Emissivities in the Solar Corona

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