Relevant bibliographies by topics / PROBA-3 space mission

Academic literature on the topic 'PROBA-3 space mission'

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Published: 10 March 2023

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Journal articles on the topic "PROBA-3 space mission"

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Vivès, S., P. Lamy, S. Koutchmy, and J. Arnaud. "ASPIICS, a giant externally occulted coronagraph for the PROBA-3 formation flying mission." Advances in Space Research 43, no. 6 (March 2009): 1007–12. http://dx.doi.org/10.1016/j.asr.2008.10.026.

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Shestov, S. V., A. N. Zhukov, B. Inhester, L. Dolla, and M. Mierla. "Expected performances of the PROBA-3/ASPIICS solar coronagraph: Simulated data." Astronomy & Astrophysics 652 (July 30, 2021): A4. http://dx.doi.org/10.1051/0004-6361/202140467.

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Context. The Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun (ASPIICS) is a novel externally occulted solar coronagraph that will be launched on board the Project for On-Board Autonomy (PROBA-3) mission in 2023. The external occulter will be placed on the first satellite ∼150 m ahead of the second satellite, which will carry an optical instrument. During 6 hours per orbit, the satellites will fly in a precise formation and will constitute a giant externally occulted coronagraph. The large distance between the external occulter and the primary objective will allow observations of the white-light solar corona starting from extremely low heights of ∼1.1 R⊙. Aims. Developing and testing of algorithms for the scientific image processing requires understanding of all the optics-related and detector-related effects of the coronagraph, development of appropriate physical and numerical models, and preparation of simulated images that include all these effects. At the same time, an analysis of the simulated data gives valuable information about the performance of the instrument, the suitable observation regime, and the amount of telemetry. Methods. We used available physical models of the instrument and implemented them as a software to generate simulated data. We analyzed intermediate and complete simulated images to obtain a better understanding of the performance of ASPIICS, in particular, to predict its photometric sensitivity, effect of noise, suitable exposure times, etc. Results. The proposed models and algorithms are used not only to create the simulated data, but also to form the basis for the scientific processing algorithms to be applied during on-ground ASPIICS data processing. We discuss the possible effect of noise and the uncertainty of the calibration factors on the accuracy of final data, and propose suitable exposure times.
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Shestov, S. V., A. N. Zhukov, and D. B. Seaton. "Modeling and removal of optical ghosts in the PROBA-3/ASPIICS externally occulted solar coronagraph." Astronomy & Astrophysics 622 (February 2019): A101. http://dx.doi.org/10.1051/0004-6361/201834584.

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Context. ASPIICS is a novel externally occulted solar coronagraph, which will be launched onboard the PROBA-3 mission of the European Space Agency. The external occulter will be placed on the first satellite ∼150 m ahead of the second satellite that will carry an optical instrument. For 6 h per orbit, the satellites will fly in a precise formation, constituting a giant externally occulted coronagraph. The large distance between the external occulter and the primary objective will allow observations of the white-light solar corona starting from extremely low heights ∼1.1 R⊙. Aims. We aim to analyze the possible influence of optical ghost images formed inside the telescope and to develop an algorithm for their removal. Methods. We implement the optical layout of ASPIICS in Zemax and study the ghost behavior in sequential and nonsequential regimes. We identify sources of the ghost contributions and analyze their geometrical behavior. Finally we develop a mathematical model and software to calculate ghost images for any given input image. Results. We show that ghost light can be important in the outer part of the field of view, where the coronal signal is weak, since the energy of bright inner corona is redistributed to the outer corona. However, the model allows for the ghost contribution to be removed. Due to the large distance between the external occulter and the primary objective, the primary objective does not produce a significant ghost. The use of the Lyot spot in ASPIICS is not necessary.
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Aime, C. "Fresnel diffraction of multiple disks on axis." Astronomy & Astrophysics 637 (May 2020): A16. http://dx.doi.org/10.1051/0004-6361/201937208.

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Aims. We seek to study the Fresnel diffraction of external occulters that differ from a single mask in a plane. Such occulters have been used in previous space missions and are planned for the future ESA Proba 3 ASPIICS coronagraph. Methods. We studied the shading efficiency of double on-axis disks and generalized results to a 3D occulter. We used standard Fourier optics in an analytical approach. We show that the Fresnel diffraction of two and three disks on axis can be expressed using a Babinet-like approach. Results are obtained in the form of convolution integrals that can be written as Bessel-Hankel integrals; these are difficult to compute numerically for large Fresnel numbers found in solar coronagraphy. Results. We show that the shading efficiency of two disks is well characterized by the intensity of the residual Arago spot, a quantity that is easier to compute and therefore allows an interesting parametric study. Very simple conditions are derived for optimal sizes and positions of two disks to produce the darkest structure around the Arago spot. These conditions are inspired from empirical experiments performed in the sixties. A differential equation is established to give the optimal envelope for a multiple-disk occulter. The solution takes the form of a simple law, the approximation of which is a conical occulter, a shape already used in the SOHO Mission. Conclusions. In addition to quantifying expected results, the present study highlights unfortunate configurations of disks and spurious diffractions that may increase the stray light. Particular attention is paid to the possible issues of the future occulter spacecraft of ASPIICS.
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Shestov, S. V., and A. N. Zhukov. "Influence of misalignments on the performance of externally occulted solar coronagraphs." Astronomy & Astrophysics 612 (April 2018): A82. http://dx.doi.org/10.1051/0004-6361/201732386.

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Context. The ASPIICS instrument is a novel externally occulted coronagraph that will be launched on board the PROBA-3 mission of the European Space Agency. The external occulter will be placed on one satellite ~150 m ahead of the second satellite that will carry an optical instrument. During 6 h out of 19.38 h of orbit, the satellites will fly in a precise (accuracy around a few millimeters) formation, constituting a giant externally occulted coronagraph. The large distance between the external occulter and the primary objective will allow observations of the white-light solar corona starting from extremely low heights ~ 1.1R⊙. Aims. We intend to analyze influence of shifts of the satellites and misalignments of optical elements on the ASPIICS performance in terms of diffracted light. Based on the quantitative influence of misalignments on diffracted light, we provide a recipe for choosing the size of the internal occulter (IO) to achieve a trade-off between the minimal height of observations and sustainability to possible misalignments. Methods. We considered different types of misalignments and analyzed their influence from optical and computational points of view. We implemented a numerical model of the diffracted light and its propagation through the optical system and computed intensities of diffracted light throughout the instrument. Our numerical approach is based on a model from the literature that considered the axisymmetrical case. Here we extend the model to include nonsymmetrical cases and possible misalignments. Results. The numerical computations fully confirm the main properties of the diffracted light that we obtained from semi-analytical consideration. We obtain that relative influences of various misalignments are significantly different. We show that the internal occulter with RIO = 1.694 mm = 1.1R⊙ is large enough to compensate possible misalignments expected to occur in PROBA-3/ASPIICS. Besides that we show that apodizing the edge of the internal occulter leads to additional suppression of the diffracted light. Conclusions. We conclude that the most important misalignment is the tilt of the telescope with respect to the line connecting the center of the external occulter and the entrance aperture. Special care should be taken to co-align the external occulter and the coronagraph, which means co-aligning the diffraction fringe from the external occulter and the internal occulter. We suggest that the best orientation strategy is to point the coronagraph to the center of the external occulter.
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Rougeot, R., R. Flamary, D. Mary, and C. Aime. "Influence of surface roughness on diffraction in the externally occulted Lyot solar coronagraph." Astronomy & Astrophysics 626 (June 2019): A1. http://dx.doi.org/10.1051/0004-6361/201834634.

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Context. The solar coronagraph ASPIICS will fly on the future ESA formation flying mission Proba-3. The instrument combines an external occulter of diameter 1.42 m and a Lyot solar coronagraph of 5 cm diameter, located downstream at a distance of 144 m. Aims. The theoretical performance of the externally occulted Lyot coronagraph has been computed by assuming perfect optics. In this paper, we improve related modelling by introducing roughness scattering effects from the telescope. We have computed the diffraction at the detector, that we compare to the ideal case without perturbation to estimate the performance degradation. We have also investigated the influence of sizing the internal occulter and the Lyot stop, and we performed a sensitivity analysis on the roughness. Methods. We have built on a recently published numerical model of diffraction propagation. The micro-structures of the telescope are built by filtering a white noise with a power spectral density following an isotropic ABC function, suggested by Harvey scatter theory. The parameters were tuned to fit experimental data measured on ASPIICS lenses. The computed wave front error was included in the Fresnel wave propagation of the coronagraph. A circular integration over the solar disk was performed to reconstruct the complete diffraction intensity. Results. The level of micro-roughness is 1.92 nm root-mean-square. Compared to the ideal case, in the plane of the internal occulter, the diffraction peak intensity is reduced by ≃0.001%. However, the intensity outside the peak increases by 12% on average, up to 20% at 3 R⊙, where the mask does not filter out the diffraction. At detector level, the diffraction peak remains ≃10−6 at 1.1 R⊙, similar to the ideal case, but the diffraction tail at large solar radius is much higher, up to one order of magnitude. Sizing the internal occulter and the Lyot stop does not improve the rejection, as opposed to the ideal case. Conclusions. Besides these results, this paper provides a methodology to implement roughness scattering in the wave propagation model for the solar coronagraph.
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Rougeot, R., and C. Aime. "Theoretical performance of serrated external occulters for solar coronagraphy." Astronomy & Astrophysics 612 (April 2018): A80. http://dx.doi.org/10.1051/0004-6361/201732512.

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Context. This study is made in the context of the future solar coronagraph ASPIICS of the ESA formation-flying mission Proba-3. Aims. In the context of solar coronagraphy, we provide a comparative study of the theoretical performance of serrated (or toothed) external occulters by varying the number and size of the teeth, which we compare to the sharp-edged and apodized disks. The tooth height is small (a few centimeters), to avoid hindering the observation of the solar corona near the limb. We first analyze the diffraction pattern produced by such occulters. In a second step, we compute the umbra profile by integration over the Sun. Methods. We explored a few methods to compute the diffraction pattern. Two of them were implemented. The first is based on 2D fast Fourier transformation (FFT) routines and a multiplication by the Fresnel filter of the form exp(−iπλzu2). Simple rules were derived and discussed to set the sampling conditions. The Maggi–Rubinowicz representation is then proposed as an alternative method, and is proven to be very efficient for this study. Results. Serrated occulters tend to create a two-level intensity pattern, the inner being the darker, which perfectly matches a previously reported geometrical prediction. The diffraction in this central region is lower by two to four orders of magnitude when compared to the sharp-edged disk. The achieved umbra level at the center ranges from 10−4 to below 10−7, depending on the geometry of the teeth. Conclusions. Our study shows that serrated occulters can achieve a high rejection and can almost reach the performance of the apodized disk when very many teeth are used. We prove that shaped occulters must be preferred to simple disks in solar and stellar coronagraphy.
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Aime, C., C. Theys, R. Rougeot, and H. Lantéri. "Principle of Fredholm image reconstruction in the vignetting zone of an externally occulted solar coronagraph." Astronomy & Astrophysics 622 (February 2019): A212. http://dx.doi.org/10.1051/0004-6361/201833843.

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Aims. This study is carried out in the context of data processing of the solar coronagraph ASPIICS of the future formation-flying mission Proba-3, which is expected to provide images of the corona very close to the limb. There will be a transition zone of the order of 100 arcsec close to the limb, where the telescope aperture suffers a strong vignetting by the external occulter (a disc of 1.42 m at 144 m). The instrument response in this region will vary rapidly both in shape and in integrated intensity, the latter being particular to the external occultation. The aim of this paper is to propose a technique to recover as much as possible of the image of the corona very close to the limb in the vignetting zone. Methods. The object image relationship in this zone is not defined by the usual convolution but by the more general Fredholm integral of the first kind. Theoretical aspects of the problem are detailed in the context of a matrix formalism for the inversion of the Fredholm integral, formalism that we maintain up to the end of the numerical simulations, which is specific to the present work. The iterative Richardson-Lucy algorithm, specially written for the non-constant integrated intensity of the responses is used here for reconstruction. A study of the effect of noise on a photodetected image is made. Results. An important part of the work consisted in calculating the elements of the transfer matrix between the object and the image for a simulation on a small region of size 100 × 100 arcsec sampled over 128 × 128 pixels. This is obtained propagating the light through the system using a previously published approach. On a toy object, the reconstruction is excellent down to about 60 arcsec from the limb, corresponding to a vignetting of 50%. The drawback is that the recovery of a N × N object requires the handling of a N2 × N2 matrix, i.e. a 16384 × 16384 transfer matrix here. However, taking into account radial symmetries of the experiment, we propose the use of a transformation from Cartesian to polar coordinates which allows to apply the same procedure all around the sun as for a small region.
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Meftah, Mustapha, Fabrice Boust, Philippe Keckhut, Alain Sarkissian, Thomas Boutéraon, Slimane Bekki, Luc Damé, et al. "INSPIRE-SAT 7, a Second CubeSat to Measure the Earth’s Energy Budget and to Probe the Ionosphere." Remote Sensing 14, no. 1 (January 1, 2022): 186. http://dx.doi.org/10.3390/rs14010186.

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INSPIRE-SAT 7 is a French 2-Unit CubeSat (11.5 × 11.5 × 22.7 cm) primarily designed for Earth and Sun observation. INSPIRE-SAT 7 is one of the missions of the International Satellite Program in Research and Education (INSPIRE). Twice the size of a 4 × 4 Rubik’s Cube and weighing about 3 kg, INSPIRE-SAT 7 will be deployed in Low Earth Orbit (LEO) in 2023 to join its sister satellite, UVSQ-SAT. INSPIRE-SAT 7 represents one of the in-orbit demonstrators needed to test how two Earth observation CubeSats in orbit can be utilized to set up a satellite constellation. This new scientific and technological pathfinder CubeSat mission (INSPIRE-SAT 7) uses a multitude of miniaturized sensors on all sides of the CubeSat to measure the Earth’s energy budget components at the top-of-the-atmosphere for climate change studies. INSPIRE-SAT 7 contains also a High-Frequency (HF) payload that will receive HF signals from a ground-based HF transmitter to probe the ionosphere for space weather studies. Finally, this CubeSat is equipped with several technological demonstrators (total solar irradiance sensors, UV sensors to measure solar spectral irradiance, a new Light Fidelity (Li-Fi) wireless communication system, a new versatile telecommunication system suitable for CubeSat). After introducing the objectives of the INSPIRE-SAT 7 mission, we present the satellite definition and the mission concept of operations. We also briefly show the observations made by the UVSQ-SAT CubeSat, and assess how two CubeSats in orbit could improve the information content of their Earth’s energy budget measurements. We conclude by reporting on the potential of future missions enabled by CubeSat constellations.
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Patterson, Richard J., Steven R. Majewski, Catherine L. Slesnick, Jaehyon Rhee, Jeffrey D. Crane, Allyson A. Polak, Arunav Kundu, et al. "The Grid Giant Star Survey for the Space Interferometry Mission." International Astronomical Union Colloquium 183 (2001): 65–74. http://dx.doi.org/10.1017/s0252921100078623.

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AbstractNASA’s Space Interferometry Mission (SIM), scheduled for launch in 2009, will determine the positions of thousands of stars as faint as V = 20 to a precision better than 4 microarcseconds (µas). A key part of the mission is the Astrometric Grid, which is a reference frame of several thousand stars with V ≤ 13 against which all relative measurements will be calibrated. To serve as a reliable inertial reference frame, the Grid must be astrometrically stable against photocenter jitter (from planets, binary companions, flaring or spotting) at the ~ 4µas level. Sub–solar metallicity giant stars, by virtue of their intrinsic luminosity, can probe the Galaxy to greater distances than almost any other stellar type at the same apparent magnitude. Thus, distant (> 3 kpc) giants with V < 13 will have proportionately smaller astrometric jitter compared to other potential Astrometric Grid star candidates. The Grid Giant Star Survey is a patchwork all-sky survey to find sub–solar metallicity K giants for the Grid, and to provide a unique database for studies of Galactic stellar populations. We describe here the survey characteristics and give examples of results to date.
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Dissertations / Theses on the topic "PROBA-3 space mission"

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Vladimiro, Noce. "PROBA-3: coronografia spaziale in formation flight." Doctoral thesis, 2021. http://hdl.handle.net/2158/1232411.

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Disegno e sviluppo del sottosistema metrologico SPS (Shadow Position Sensor) a bordo della missione ESA PROBA-3 il cui scopo è la dimostrazione delle capacità di volo in formazione di due satelliti che costituiranno, inoltre, un coronografo gigante nello spazio. Design and devopment of the SPS (Shadow Position Sensor) metrology subsystem on board the ESA PROBA-3 mission, whose aim is to demonstrate formation-flying capabilites and to deploy in space a large virtual instrument devoted to Sun corona observations.
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Conference papers on the topic "PROBA-3 space mission"

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Galano, Damien, Steve Buckley, Ileana Cernica, Vladimír Dániel, François Denis, Lieve de Vos, Silvano Fineschi, et al. "Development of ASPIICS: a coronagraph based on Proba-3 formation flying mission." In Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, edited by Howard A. MacEwen, Makenzie Lystrup, Giovanni G. Fazio, Natalie Batalha, Edward C. Tong, and Nicholas Siegler. SPIE, 2018. http://dx.doi.org/10.1117/12.2312493.

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Capobianco, Gerardo, F. Amadori, Silvano Fineschi, Alessandro Bemporad, Marta Casti, Davide Loreggia, Vladimiro Noce, et al. "Formation flying performances simulator for the shadow position sensors of the ESA PROBA-3 mission." In International Conference on Space Optics — ICSO 2021, edited by Zoran Sodnik, Bruno Cugny, and Nikos Karafolas. SPIE, 2021. http://dx.doi.org/10.1117/12.2600310.

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Lamy, P. L., S. Vivès, W. Curdt, J. Davila, J. M. Defise, Silvano Fineschi, S. Kuzin, et al. "ASPIICS: a giant, white light and emission line coronagraph for the ESA proba-3 formation flight mission." In International Conference on Space Optics 2010, edited by Naoto Kadowaki. SPIE, 2017. http://dx.doi.org/10.1117/12.2309188.

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Noce, Vladimiro, Mauro Focardi, Steve Buckley, François Denis, Alessandro Bemporad, Silvano Fineschi, Maurizio Pancrazzi, et al. "An improved version of the Shadow Position Sensor readout electronics on-board the ESA PROBA-3 Mission." In UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XX, edited by Oswald H. Siegmund. SPIE, 2017. http://dx.doi.org/10.1117/12.2273694.

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"Feasibility of the PROBA 3 Formation Flying Demonstration Mission as a Pair of Microsats in GTO." In 55th International Astronautical Congress of the International Astronautical Federation, the International Academy of Astronautics, and the International Institute of Space Law. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2004. http://dx.doi.org/10.2514/6.iac-04-u.1.04.

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Messaros, Robert, Marius-Catalin Dumitru, and Milan Novacek. "The Proba-3 G-EMCS approach to a highly integrated multi spacecraft Mission Operations and EGSE System featuring SLE and POCKET support." In 15th International Conference on Space Operations. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2018. http://dx.doi.org/10.2514/6.2018-2393.

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Perez, Rovin, and Slaveya Abadzhieva. "Design challenges, and outcomes of building a satellite the size of a soda can." In Symposium on Space Educational Activities (SSAE). Universitat Politècnica de Catalunya, 2022. http://dx.doi.org/10.5821/conference-9788419184405.070.

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A Mach contest is part of an annual event, organized by UKLSL, which combines both CanSat and rocket competitions. The first Mach event in 2021 was focused on the design of “Simple and Advance CanSats”, and culminated on a 3-day activity at Machrihanish Airbase in Scotland. It involved setup, pre-flight checks, and system adjustments. This paper focuses on the design challenges, and outcomes from building a satellite the size of a soda can by reviewing the event, the mission designed for the competition, and students’ feedback on what could have been improved to prepare the next team competing in Mach-22 which would involve developing a Rocket design and launching an “Advance CanSat”. The competition allowed undergraduate students at The University of Nottingham to experience a practical learning style by solving real engineering problems and practicing professional development skills through design review presentations and providing a flight readiness review to the launch providers of the competition. The proposed mission statement was part of the “PEAK” category, which involved atmospheric studies, where it acts as a simulation model for measuring the atmosphere on different planets and as a deployable probe from rovers to measure varying atmospheric levels. The competition exposed students to perform AITV (Assembly, Integration, Testing, Verification) processes to their CanSat and constructed procedures to test and validate the recovery system. Results from the first Mach event prove a solid starting point for future CanSat competition and space activities within our university. In the future, there are aspirations to grow a student space society and get students involved in extra-curricular STEM (Science, Technology, Engineering, Math) projects, and allow them to apply the theory and concepts learned in their academics
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