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Your search keyword '"Bemporad, A."' showing total 96 results
Start Over Author "Bemporad, A." Publisher edp sciences
96 results on '"Bemporad, A."'

1. Study of solar brightness profiles in the 18–26 GHz frequency range with INAF radio telescopes

Author

Marongiu, M., primary, Pellizzoni, A., additional, Righini, S., additional, Mulas, S., additional, Nesti, R., additional, Burtovoi, A., additional, Romoli, M., additional, Serra, G., additional, Valente, G., additional, Egron, E., additional, Murtas, G., additional, Iacolina, M. N., additional, Melis, A., additional, Guglielmino, S. L., additional, Loru, S., additional, Zucca, P., additional, Zanichelli, A., additional, Bachetti, M., additional, Bemporad, A., additional, Buffa, F., additional, Concu, R., additional, Deiana, G. L., additional, Karakotia, C., additional, Ladu, A., additional, Maccaferri, A., additional, Marongiu, P., additional, Messerotti, M., additional, Navarrini, A., additional, Orfei, A., additional, Ortu, P., additional, Pili, M., additional, Pisanu, T., additional, Pupillo, G., additional, Romano, P., additional, Saba, A., additional, Schirru, L., additional, Tiburzi, C., additional, Abbo, L., additional, Frassati, F., additional, Giarrusso, M., additional, Jerse, G., additional, Landini, F., additional, Pancrazzi, M., additional, Russano, G., additional, Sasso, C., additional, and Susino, R., additional

Published
2024
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2. Eruptive events with exceptionally bright emission in H I Ly-α observed by the Metis coronagraph

Author

Russano, G., primary, Andretta, V., additional, De Leo, Y., additional, Teriaca, L., additional, Uslenghi, M., additional, Giordano, S., additional, Telloni, D., additional, Heinzel, P., additional, Jejčič, S., additional, Abbo, L., additional, Bemporad, A., additional, Burtovoi, A., additional, Capuano, G. E., additional, Frassati, F., additional, Guglielmino, S. L., additional, Jerse, G., additional, Landini, F., additional, Liberatore, A., additional, Nicolini, G., additional, Pancrazzi, M., additional, Romano, P., additional, Sasso, C., additional, Susino, R., additional, Zangrilli, L., additional, Da Deppo, V., additional, Fineschi, S., additional, Grimani, C., additional, Moses, J. D., additional, Naletto, G., additional, Romoli, M., additional, Spadaro, D., additional, and Stangalini, M., additional

Published
2024
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4. In-flight radiometric calibration of the Metis Visible Light channel using stars and comparison with STEREO-A/COR2 data

Author

De Leo, Y., primary, Burtovoi, A., additional, Teriaca, L., additional, Romoli, M., additional, Chioetto, P., additional, Andretta, V., additional, Uslenghi, M., additional, Landini, F., additional, Susino, R., additional, Pancrazzi, M., additional, Frassati, F., additional, Giarrusso, M., additional, Giordano, S., additional, Zangrilli, L., additional, Spadaro, D., additional, Abbo, L., additional, Bemporad, A., additional, Capobianco, G., additional, Capuano, G. E., additional, Casini, C., additional, Casti, M., additional, Corso, A. J., additional, Da Deppo, V., additional, Fabi, M., additional, Fineschi, S., additional, Frassetto, F., additional, Grimani, C., additional, Guglielmino, S. L., additional, Heinzel, P., additional, Jerse, G., additional, Liberatore, A., additional, Magli, E., additional, Massone, G., additional, Messerotti, M., additional, Moses, J. D., additional, Naletto, G., additional, Nicolini, G., additional, Pelizzo, M. G., additional, Romano, P., additional, Russano, G., additional, Sasso, C., additional, Schühle, U., additional, Straus, T., additional, Slemer, A., additional, Stangalini, M., additional, Telloni, D., additional, Volpicelli, C. A., additional, and Zuppella, P., additional

Published
2023
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5. A high-latitude coronal mass ejection observed by a constellation of coronagraphs: Solar Orbiter/Metis, STEREO-A/COR2, and SOHO/LASCO

Author

Zimbardo, G., primary, Ying, B., additional, Nisticò, G., additional, Feng, L., additional, Rodríguez-García, L., additional, Panasenco, O., additional, Andretta, V., additional, Banerjee, D., additional, Bemporad, A., additional, De Leo, Y., additional, Franci, L., additional, Frassati, F., additional, Habbal, S., additional, Long, D., additional, Magdalenic, J., additional, Mancuso, S., additional, Naletto, G., additional, Perri, S., additional, Romoli, M., additional, Spadaro, D., additional, Stangalini, M., additional, Strachan, L., additional, Susino, R., additional, Vainio, R., additional, Velli, M., additional, Cohen, C. M. S., additional, Giacalone, J., additional, Shen, M., additional, Telloni, D., additional, Abbo, L., additional, Burtovoi, A., additional, Jerse, G., additional, Landini, F., additional, Nicolini, G., additional, Pancrazzi, M., additional, Russano, G., additional, Sasso, C., additional, and Uslenghi, M., additional

Published
2023
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6. Reconstruction of the Parker spiral with the Reverse In situ data and MHD APproach – RIMAP

Author

Biondo Ruggero, Bemporad Alessandro, Mignone Andrea, and Reale Fabio

Subjects
solar wind, coronal mass ejections, space weather, modeling, heliosphere, interplanetary medium, Meteorology. Climatology, QC851-999
Abstract

The reconstruction of plasma parameters in the interplanetary medium is very important to understand the interplanetary propagation of solar eruptions and for Space Weather application purposes. Because only a few spacecraft are measuring in situ these parameters, reconstructions are currently performed by running complex numerical Magneto-hydrodynamic (MHD) simulations starting from remote sensing observations of the Sun. Current models apply full 3D MHD simulations of the corona or extrapolations of photospheric magnetic fields combined with semi-empirical relationships to derive the plasma parameters on a sphere centered on the Sun (inner boundary). The plasma is then propagated in the interplanetary medium up to the Earth’s orbit and beyond. Nevertheless, this approach requires significant theoretical and computational efforts, and the results are only in partial agreement with the in situ observations. In this paper we describe a new approach to this problem called RIMAP – Reverse In situ data and MHD APproach. The plasma parameters in the inner boundary at 0.1 AU are derived directly from the in situ measurements acquired at 1 AU, by applying a back reconstruction technique to remap them into the inner heliosphere. This remapping is done by using the Weber and Davies solar wind theoretical model to reconstruct the wind flowlines. The plasma is then re-propagated outward from 0.1 AU by running a MHD numerical simulation based on the PLUTO code. The interplanetary spiral reconstructions obtained with RIMAP are not only in a much better agreement with the in situ observations, but are also including many more small-scale longitudinal features in the plasma parameters that are not reproduced with the approaches developed so far.

Published
2021
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8. Connecting Solar Orbiter remote-sensing observations and Parker Solar Probe in situ measurements with a numerical MHD reconstruction of the Parker spiral

Author

Biondo, Ruggero, primary, Bemporad, Alessandro, additional, Pagano, Paolo, additional, Telloni, Daniele, additional, Reale, Fabio, additional, Romoli, Marco, additional, Andretta, Vincenzo, additional, Antonucci, Ester, additional, Da Deppo, Vania, additional, De Leo, Yara, additional, Fineschi, Silvano, additional, Heinzel, Petr, additional, Moses, Daniel, additional, Naletto, Giampiero, additional, Nicolini, Gianalfredo, additional, Spadaro, Daniele, additional, Stangalini, Marco, additional, Teriaca, Luca, additional, Landini, Federico, additional, Sasso, Clementina, additional, Susino, Roberto, additional, Jerse, Giovanna, additional, Uslenghi, Michela, additional, and Pancrazzi, Maurizio, additional

Published
2022
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9. Current state and perspectives of Space Weather science in Italy

Author

Plainaki Christina, Antonucci Marco, Bemporad Alessandro, Berrilli Francesco, Bertucci Bruna, Castronuovo Marco, De Michelis Paola, Giardino Marco, Iuppa Roberto, Laurenza Monica, Marcucci Federica, Messerotti Mauro, Narici Livio, Negri Barbara, Nozzoli Francesco, Orsini Stefano, Romano Vincenzo, Cavallini Enrico, Polenta Gianluca, and Ippolito Alessandro

Subjects
heliosphere, instrumentation, missions, strategy, data management, Meteorology. Climatology, QC851-999
Abstract

Italian teams have been involved many times in Space Weather observational campaigns from space and from the ground, contributing in the advancing of our knowledge on the properties and evolution of the related phenomena. Numerous Space Weather forecasting and now-casting modeling efforts have resulted in a remarkable add-on to the overall progress in the field, at both national and international level. The Italian Space Agency has participated several times in space missions with science objectives related to Space Weather; indeed, an important field for the Italian scientific and industrial communities interested in Heliophysics and Space Weather, is the development of new instrumentation for future space missions. In this paper, we present a brief state-of-the-art in Space Weather science in Italy and we discuss some ideas on a long-term plan for the support of future scientific research in the related disciplines. In the context of the current roadmap, the Italian Space Agency aims to assess the possibility to develop a national scientific Space Weather data centre to encourage synergies between different science teams with interest in the field and to motivate innovation and new mission concept development. Alongside with the proposed recommendations, we also discuss how the Italian expertise could complement international efforts in a wider international Space Weather context.

Published
2020
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10. Coronal mass ejection followed by a prominence eruption and a plasma blob as observed by Solar Orbiter

Author

Bemporad, A., primary, Andretta, V., additional, Susino, R., additional, Mancuso, S., additional, Spadaro, D., additional, Mierla, M., additional, Berghmans, D., additional, D’Huys, E., additional, Zhukov, A. N., additional, Talpeanu, D.-C., additional, Colaninno, R., additional, Hess, P., additional, Koza, J., additional, Jejčič, S., additional, Heinzel, P., additional, Antonucci, E., additional, Da Deppo, V., additional, Fineschi, S., additional, Frassati, F., additional, Jerse, G., additional, Landini, F., additional, Naletto, G., additional, Nicolini, G., additional, Pancrazzi, M., additional, Romoli, M., additional, Sasso, C., additional, Slemer, A., additional, Stangalini, M., additional, and Teriaca, L., additional

Published
2022
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11. Reconstruction of the Parker spiral with the Reverse in situ data and MHD APproach - RIMAP

Author

R. Biondo, Alessandro Bemporad, Andrea Mignone, Fabio Reale, Biondo R., Bemporad A., Mignone A., and Reale F.

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Space weather, Solar wind, Interplanetary medium, lcsh:QC851-999, 01 natural sciences, Heliosphere, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Modeling, Coronal mass ejections, Computational physics, Space and Planetary Science, Physics::Space Physics, lcsh:Meteorology. Climatology, Heliospheric current sheet, Astrophysics::Earth and Planetary Astrophysics, Magnetohydrodynamics, Interplanetary spaceflight
Abstract

The reconstruction of plasma parameters in the interplanetary medium is very important to understand the interplanetary propagation of solar eruptions and for Space Weather application purposes. Because only a few spacecraft are measuring in situ these parameters, reconstructions are currently performed by running complex numerical Magneto-hydrodynamic (MHD) simulations starting from remote sensing observations of the Sun. Current models apply full 3D MHD simulations of the corona or extrapolations of photospheric magnetic fields combined with semi-empirical relationships to derive the plasma parameters on a sphere centered on the Sun (inner boundary). The plasma is then propagated in the interplanetary medium up to the Earth’s orbit and beyond. Nevertheless, this approach requires significant theoretical and computational efforts, and the results are only in partial agreement with the in situ observations. In this paper we describe a new approach to this problem called RIMAP – Reverse In situ data and MHD APproach. The plasma parameters in the inner boundary at 0.1 AU are derived directly from the in situ measurements acquired at 1 AU, by applying a back reconstruction technique to remap them into the inner heliosphere. This remapping is done by using the Weber and Davies solar wind theoretical model to reconstruct the wind flowlines. The plasma is then re-propagated outward from 0.1 AU by running a MHD numerical simulation based on the PLUTO code. The interplanetary spiral reconstructions obtained with RIMAP are not only in a much better agreement with the in situ observations, but are also including many more small-scale longitudinal features in the plasma parameters that are not reproduced with the approaches developed so far.

Published
2021

12. Cosmic-ray flux predictions and observations for and with Metis on board Solar Orbiter

Author

Grimani, C., primary, Andretta, V., additional, Chioetto, P., additional, Da Deppo, V., additional, Fabi, M., additional, Gissot, S., additional, Naletto, G., additional, Persici, A., additional, Plainaki, C., additional, Romoli, M., additional, Sabbatini, F., additional, Spadaro, D., additional, Stangalini, M., additional, Telloni, D., additional, Uslenghi, M., additional, Antonucci, E., additional, Bemporad, A., additional, Capobianco, G., additional, Capuano, G., additional, Casti, M., additional, De Leo, Y., additional, Fineschi, S., additional, Frassati, F., additional, Frassetto, F., additional, Heinzel, P., additional, Jerse, G., additional, Landini, F., additional, Liberatore, A., additional, Magli, E., additional, Messerotti, M., additional, Moses, D., additional, Nicolini, G., additional, Pancrazzi, M., additional, Pelizzo, M. G., additional, Romano, P., additional, Sasso, C., additional, Schühle, U., additional, Slemer, A., additional, Straus, T., additional, Susino, R., additional, Teriaca, L., additional, Volpicelli, C. A., additional, Freiherr von Forstner, J. L., additional, and Zuppella, P., additional

Published
2021
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13. First light observations of the solar wind in the outer corona with the Metis coronagraph

Author

Romoli, M., primary, Antonucci, E., additional, Andretta, V., additional, Capuano, G. E., additional, Da Deppo, V., additional, De Leo, Y., additional, Downs, C., additional, Fineschi, S., additional, Heinzel, P., additional, Landini, F., additional, Liberatore, A., additional, Naletto, G., additional, Nicolini, G., additional, Pancrazzi, M., additional, Sasso, C., additional, Spadaro, D., additional, Susino, R., additional, Telloni, D., additional, Teriaca, L., additional, Uslenghi, M., additional, Wang, Y.-M., additional, Bemporad, A., additional, Capobianco, G., additional, Casti, M., additional, Fabi, M., additional, Frassati, F., additional, Frassetto, F., additional, Giordano, S., additional, Grimani, C., additional, Jerse, G., additional, Magli, E., additional, Massone, G., additional, Messerotti, M., additional, Moses, D., additional, Pelizzo, M.-G., additional, Romano, P., additional, Schühle, U., additional, Slemer, A., additional, Stangalini, M., additional, Straus, T., additional, Volpicelli, C. A., additional, Zangrilli, L., additional, Zuppella, P., additional, Abbo, L., additional, Auchère, F., additional, Aznar Cuadrado, R., additional, Berlicki, A., additional, Bruno, R., additional, Ciaravella, A., additional, D’Amicis, R., additional, Lamy, P., additional, Lanzafame, A., additional, Malvezzi, A. M., additional, Nicolosi, P., additional, Nisticò, G., additional, Peter, H., additional, Plainaki, C., additional, Poletto, L., additional, Reale, F., additional, Solanki, S. K., additional, Strachan, L., additional, Tondello, G., additional, Tsinganos, K., additional, Velli, M., additional, Ventura, R., additional, Vial, J.-C., additional, Woch, J., additional, and Zimbardo, G., additional

Published
2021
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14. The first coronal mass ejection observed in both visible-light and UV H I Ly-αchannels of the Metis coronagraph on board Solar Orbiter

Author

Andretta, V., primary, Bemporad, A., additional, De Leo, Y., additional, Jerse, G., additional, Landini, F., additional, Mierla, M., additional, Naletto, G., additional, Romoli, M., additional, Sasso, C., additional, Slemer, A., additional, Spadaro, D., additional, Susino, R., additional, Talpeanu, D.-C., additional, Telloni, D., additional, Teriaca, L., additional, Uslenghi, M., additional, Antonucci, E., additional, Auchère, F., additional, Berghmans, D., additional, Berlicki, A., additional, Capobianco, G., additional, Capuano, G. E., additional, Casini, C., additional, Casti, M., additional, Chioetto, P., additional, Da Deppo, V., additional, Fabi, M., additional, Fineschi, S., additional, Frassati, F., additional, Frassetto, F., additional, Giordano, S., additional, Grimani, C., additional, Heinzel, P., additional, Liberatore, A., additional, Magli, E., additional, Massone, G., additional, Messerotti, M., additional, Moses, D., additional, Nicolini, G., additional, Pancrazzi, M., additional, Pelizzo, M.-G., additional, Romano, P., additional, Schühle, U., additional, Stangalini, M., additional, Straus, Th., additional, Volpicelli, C. A., additional, Zangrilli, L., additional, Zuppella, P., additional, Abbo, L., additional, Aznar Cuadrado, R., additional, Bruno, R., additional, Ciaravella, A., additional, D’Amicis, R., additional, Lamy, P., additional, Lanzafame, A., additional, Malvezzi, A. M., additional, Nicolosi, P., additional, Nisticò, G., additional, Peter, H., additional, Plainaki, C., additional, Poletto, L., additional, Reale, F., additional, Solanki, S. K., additional, Strachan, L., additional, Tondello, G., additional, Tsinganos, K., additional, Velli, M., additional, Ventura, R., additional, Vial, J.-C., additional, Woch, J., additional, and Zimbardo, G., additional

Published
2021
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17. Effects of the chromospheric Lyα line profile shape on the determination of the solar wind H I outflow velocity using the Doppler dimming technique

Author

Capuano, G. E., primary, Dolei, S., additional, Spadaro, D., additional, Guglielmino, S. L., additional, Romano, P., additional, Ventura, R., additional, Andretta, V., additional, Bemporad, A., additional, Sasso, C., additional, Susino, R., additional, Da Deppo, V., additional, Frassetto, F., additional, Giordano, S. M., additional, Landini, F., additional, Nicolini, G., additional, Pancrazzi, M., additional, Romoli, M., additional, and Zangrilli, L., additional

Published
2021
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18. SWIFF: Space weather integrated forecasting framework

Author

Frederiksen Jacob Trier, Nordlund Åke, Restante Anna Lisa, Olshevsky Vyacheslav, Faganello Matteo, Pegoraro Francesco, Califano Francesco, Henri Pierre, Trávníček Pavel M., Šebek Ondřej, Poedts Stefaan, Markidis Stefano, Keppens Rony, Pierrard Viviane, Lapenta Giovanni, Mackay Duncan H., Parnell Clare E., Bemporad Alessandro, Susino Roberto, and Borremans Kris

Subjects
space weather, modelling, high performance computing, Meteorology. Climatology, QC851-999
Abstract

SWIFF is a project funded by the Seventh Framework Programme of the European Commission to study the mathematical-physics models that form the basis for space weather forecasting. The phenomena of space weather span a tremendous scale of densities and temperature with scales ranging 10 orders of magnitude in space and time. Additionally even in local regions there are concurrent processes developing at the electron, ion and global scales strongly interacting with each other. The fundamental challenge in modelling space weather is the need to address multiple physics and multiple scales. Here we present our approach to take existing expertise in fluid and kinetic models to produce an integrated mathematical approach and software infrastructure that allows fluid and kinetic processes to be modelled together. SWIFF aims also at using this new infrastructure to model specific coupled processes at the Solar Corona, in the interplanetary space and in the interaction at the Earth magnetosphere.

Published
2013
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20. Coordination within the remote sensing payload on the Solar Orbiter mission

Author

O. C. St. Cyr, D. Orozco Suárez, Ester Antonucci, Sunil Sidher, Marina Battaglia, Phillip C. Chamberlin, V. Andretta, David Long, Johann Hirzberger, A. Giunta, Silvano Fineschi, N. Bach, Simon Plunkett, C. Watson, B. Mampaey, S. Fahmy, I. Tanco, S. Caminade, Andrei Zhukov, Andreas Lagg, David Berghmans, Joachim Woch, David R. Williams, G. J. Hurford, M. Haberreiter, T. Grundy, Shane A. Maloney, Donald M. Hassler, S. Parenti, J. J. Cerullo, Eric Buchlin, Sami K. Solanki, Federico Landini, A. Pacros, J. Carlyle, A. De Groof, Angelos Vourlidas, V. Martinez-Pillet, J. Lefort, Alexis P. Rouillard, Cis Verbeeck, S. Lodiot, Mats Carlsson, Gianalfredo Nicolini, T. Straus, M. Kolleck, L. Etesi, D. R. McMullin, L. Sanchez, R. A. Howard, J. C. del Toro Iniesta, Daniel Müller, Joseph M. Davila, F. Marliani, Robin C. Colaninno, F. Auchère, Lucia Kleint, A. Philippon, Andrzej Fludra, Luca Teriaca, Louise K. Harra, Udo Schühle, Marco Romoli, William T. Thompson, Holly Gilbert, Maurizio Pancrazzi, Alessandro Bemporad, P. Rochus, Säm Krucker, N. Rich, I. Zouganelis, Hardi Peter, Daniele Spadaro, Thomas Wiegelmann, Science and Technology Facilities Council (UK), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Umeå University, Department of Chemistry, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], GSFC Laboratory for Solar and Space Physics, NASA Goddard Space Flight Center (GSFC), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Royal Observatory of Belgium [Brussels] (ROB), Trinity College Dublin, Space Systems Research Corporation (SSRC), European Space Research and Technology Centre (ESTEC), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidad de Cantabria [Santander], INAF - Osservatorio Astrofisico di Catania (OACT), University of Kansas [Kansas City], Johns Hopkins University (JHU), Solar-Terrestrial Centre of Excellence [Brussels] (STCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung (MPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Solar System Research (MPS), and European Space Agency (European Space Agency) (ESA)

Subjects
Sun: general, 010504 meteorology & atmospheric sciences, Context (language use), Instrumentation: spectrographs, Instrumentation: polarimeters, 01 natural sciences, law.invention, instruments [Space vehicles], Orbiter, law, 0103 physical sciences, general [Sun], Space vehicles: instruments, spectrographs [Instrumentation], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Physics, Earth's orbit, Data processing, polarimeters [Instrumentation], Spacecraft, instruments, instrumentation: polarimeters, instrumentation: spectrographs, telescopes [space vehicles], business.industry, Payload, Suite, Bandwidth (signal processing), Astronomy and Astrophysics, Space and Planetary Science, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Telescopes
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.-- Full list of authors: Auchère, F.; Andretta, V.; Antonucci, E.; Bach, N.; Battaglia, M.; Bemporad, A.; Berghmans, D.; Buchlin, E.; Caminade, S.; Carlsson, M.; Carlyle, J.; Cerullo, J. J.; Chamberlin, P. C.; Colaninno, R. C.; Davila, J. M.; De Groof, A.; Etesi, L.; Fahmy, S.; Fineschi, S.; Fludra, A.; Gilbert, H. R.; Giunta, A.; Grundy, T.; Haberreiter, M.; Harra, L. K.; Hassler, D. M.; Hirzberger, J.; Howard, R. A.; Hurford, G.; Kleint, L.; Kolleck, M.; Krucker, S.; Lagg, A.; Landini, F.; Long, D. M.; Lefort, J.; Lodiot, S.; Mampaey, B.; Maloney, S.; Marliani, F.; Martinez-Pillet, V.; McMullin, D. R.; Müller, D.; Nicolini, G.; Orozco Suarez, D.; Pacros, A.; Pancrazzi, M.; Parenti, S.; Peter, H.; Philippon, A.; Plunkett, S.; Rich, N.; Rochus, P.; Rouillard, A.; Romoli, M.; Sanchez, L.; Schühle, U.; Sidher, S.; Solanki, S. K.; Spadaro, D.; St Cyr, O. C.; Straus, T.; Tanco, I.; Teriaca, L.; Thompson, W. T.; del Toro Iniesta, J. C.; Verbeeck, C.; Vourlidas, A.; Watson, C.; Wiegelmann, T.; Williams, D.; Woch, J.; Zhukov, A. N.; Zouganelis, I., Context. To meet the scientific objectives of the mission, the Solar Orbiter spacecraft carries a suite of in-situ (IS) and remote sensing (RS) instruments designed for joint operations with inter-instrument communication capabilities. Indeed, previous missions have shown that the Sun (imaged by the RS instruments) and the heliosphere (mainly sampled by the IS instruments) should be considered as an integrated system rather than separate entities. Many of the advances expected from Solar Orbiter rely on this synergistic approach between IS and RS measurements. Aims. Many aspects of hardware development, integration, testing, and operations are common to two or more RS instruments. In this paper, we describe the coordination effort initiated from the early mission phases by the Remote Sensing Working Group. We review the scientific goals and challenges, and give an overview of the technical solutions devised to successfully operate these instruments together. Methods. A major constraint for the RS instruments is the limited telemetry (TM) bandwidth of the Solar Orbiter deep-space mission compared to missions in Earth orbit. Hence, many of the strategies developed to maximise the scientific return from these instruments revolve around the optimisation of TM usage, relying for example on onboard autonomy for data processing, compression, and selection for downlink. The planning process itself has been optimised to alleviate the dynamic nature of the targets, and an inter-instrument communication scheme has been implemented which can be used to autonomously alter the observing modes. We also outline the plans for in-flight cross-calibration, which will be essential to the joint data reduction and analysis. Results. The RS instrument package on Solar Orbiter will carry out comprehensive measurements from the solar interior to the inner heliosphere. Thanks to the close coordination between the instrument teams and the European Space Agency, several challenges specific to the RS suite were identified and addressed in a timely manner. © 2020 F. Auchère et al., A. V. is supported by NRL grant N00173-16-1-G029. D. M. L. is grateful to the Science Technology and Facilities Council for the award of an Ernest Rutherford Fellowship (ST/R003246/1).

Published
2020
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21. The Solar Orbiter Science Activity Plan

Author

Zouganelis, I., primary, De Groof, A., additional, Walsh, A. P., additional, Williams, D. R., additional, Müller, D., additional, St Cyr, O. C., additional, Auchère, F., additional, Berghmans, D., additional, Fludra, A., additional, Horbury, T. S., additional, Howard, R. A., additional, Krucker, S., additional, Maksimovic, M., additional, Owen, C. J., additional, Rodríguez-Pacheco, J., additional, Romoli, M., additional, Solanki, S. K., additional, Watson, C., additional, Sanchez, L., additional, Lefort, J., additional, Osuna, P., additional, Gilbert, H. R., additional, Nieves-Chinchilla, T., additional, Abbo, L., additional, Alexandrova, O., additional, Anastasiadis, A., additional, Andretta, V., additional, Antonucci, E., additional, Appourchaux, T., additional, Aran, A., additional, Arge, C. N., additional, Aulanier, G., additional, Baker, D., additional, Bale, S. D., additional, Battaglia, M., additional, Bellot Rubio, L., additional, Bemporad, A., additional, Berthomier, M., additional, Bocchialini, K., additional, Bonnin, X., additional, Brun, A. S., additional, Bruno, R., additional, Buchlin, E., additional, Büchner, J., additional, Bucik, R., additional, Carcaboso, F., additional, Carr, R., additional, Carrasco-Blázquez, I., additional, Cecconi, B., additional, Cernuda Cangas, I., additional, Chen, C. H. K., additional, Chitta, L. P., additional, Chust, T., additional, Dalmasse, K., additional, D’Amicis, R., additional, Da Deppo, V., additional, De Marco, R., additional, Dolei, S., additional, Dolla, L., additional, Dudok de Wit, T., additional, van Driel-Gesztelyi, L., additional, Eastwood, J. P., additional, Espinosa Lara, F., additional, Etesi, L., additional, Fedorov, A., additional, Félix-Redondo, F., additional, Fineschi, S., additional, Fleck, B., additional, Fontaine, D., additional, Fox, N. J., additional, Gandorfer, A., additional, Génot, V., additional, Georgoulis, M. K., additional, Gissot, S., additional, Giunta, A., additional, Gizon, L., additional, Gómez-Herrero, R., additional, Gontikakis, C., additional, Graham, G., additional, Green, L., additional, Grundy, T., additional, Haberreiter, M., additional, Harra, L. K., additional, Hassler, D. M., additional, Hirzberger, J., additional, Ho, G. C., additional, Hurford, G., additional, Innes, D., additional, Issautier, K., additional, James, A. W., additional, Janitzek, N., additional, Janvier, M., additional, Jeffrey, N., additional, Jenkins, J., additional, Khotyaintsev, Y., additional, Klein, K.-L., additional, Kontar, E. P., additional, Kontogiannis, I., additional, Krafft, C., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Labrosse, N., additional, Lagg, A., additional, Landini, F., additional, Lavraud, B., additional, Leon, I., additional, Lepri, S. T., additional, Lewis, G. R., additional, Liewer, P., additional, Linker, J., additional, Livi, S., additional, Long, D. M., additional, Louarn, P., additional, Malandraki, O., additional, Maloney, S., additional, Martinez-Pillet, V., additional, Martinovic, M., additional, Masson, A., additional, Matthews, S., additional, Matteini, L., additional, Meyer-Vernet, N., additional, Moraitis, K., additional, Morton, R. J., additional, Musset, S., additional, Nicolaou, G., additional, Nindos, A., additional, O’Brien, H., additional, Orozco Suarez, D., additional, Owens, M., additional, Pancrazzi, M., additional, Papaioannou, A., additional, Parenti, S., additional, Pariat, E., additional, Patsourakos, S., additional, Perrone, D., additional, Peter, H., additional, Pinto, R. F., additional, Plainaki, C., additional, Plettemeier, D., additional, Plunkett, S. P., additional, Raines, J. M., additional, Raouafi, N., additional, Reid, H., additional, Retino, A., additional, Rezeau, L., additional, Rochus, P., additional, Rodriguez, L., additional, Rodriguez-Garcia, L., additional, Roth, M., additional, Rouillard, A. P., additional, Sahraoui, F., additional, Sasso, C., additional, Schou, J., additional, Schühle, U., additional, Sorriso-Valvo, L., additional, Soucek, J., additional, Spadaro, D., additional, Stangalini, M., additional, Stansby, D., additional, Steller, M., additional, Strugarek, A., additional, Štverák, Š., additional, Susino, R., additional, Telloni, D., additional, Terasa, C., additional, Teriaca, L., additional, Toledo-Redondo, S., additional, del Toro Iniesta, J. C., additional, Tsiropoula, G., additional, Tsounis, A., additional, Tziotziou, K., additional, Valentini, F., additional, Vaivads, A., additional, Vecchio, A., additional, Velli, M., additional, Verbeeck, C., additional, Verdini, A., additional, Verscharen, D., additional, Vilmer, N., additional, Vourlidas, A., additional, Wicks, R., additional, Wimmer-Schweingruber, R. F., additional, Wiegelmann, T., additional, Young, P. R., additional, and Zhukov, A. N., additional

Published
2020
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22. Models and data analysis tools for the Solar Orbiter mission

Author

Rouillard, A. P., primary, Pinto, R. F., additional, Vourlidas, A., additional, De Groof, A., additional, Thompson, W. T., additional, Bemporad, A., additional, Dolei, S., additional, Indurain, M., additional, Buchlin, E., additional, Sasso, C., additional, Spadaro, D., additional, Dalmasse, K., additional, Hirzberger, J., additional, Zouganelis, I., additional, Strugarek, A., additional, Brun, A. S., additional, Alexandre, M., additional, Berghmans, D., additional, Raouafi, N. E., additional, Wiegelmann, T., additional, Pagano, P., additional, Arge, C. N., additional, Nieves-Chinchilla, T., additional, Lavarra, M., additional, Poirier, N., additional, Amari, T., additional, Aran, A., additional, Andretta, V., additional, Antonucci, E., additional, Anastasiadis, A., additional, Auchère, F., additional, Bellot Rubio, L., additional, Nicula, B., additional, Bonnin, X., additional, Bouchemit, M., additional, Budnik, E., additional, Caminade, S., additional, Cecconi, B., additional, Carlyle, J., additional, Cernuda, I., additional, Davila, J. M., additional, Etesi, L., additional, Espinosa Lara, F., additional, Fedorov, A., additional, Fineschi, S., additional, Fludra, A., additional, Génot, V., additional, Georgoulis, M. K., additional, Gilbert, H. R., additional, Giunta, A., additional, Gomez-Herrero, R., additional, Guest, S., additional, Haberreiter, M., additional, Hassler, D., additional, Henney, C. J., additional, Howard, R. A., additional, Horbury, T. S., additional, Janvier, M., additional, Jones, S. I., additional, Kozarev, K., additional, Kraaikamp, E., additional, Kouloumvakos, A., additional, Krucker, S., additional, Lagg, A., additional, Linker, J., additional, Lavraud, B., additional, Louarn, P., additional, Maksimovic, M., additional, Maloney, S., additional, Mann, G., additional, Masson, A., additional, Müller, D., additional, Önel, H., additional, Osuna, P., additional, Orozco Suarez, D., additional, Owen, C. J., additional, Papaioannou, A., additional, Pérez-Suárez, D., additional, Rodriguez-Pacheco, J., additional, Parenti, S., additional, Pariat, E., additional, Peter, H., additional, Plunkett, S., additional, Pomoell, J., additional, Raines, J. M., additional, Riethmüller, T. L., additional, Rich, N., additional, Rodriguez, L., additional, Romoli, M., additional, Sanchez, L., additional, Solanki, S. K., additional, St Cyr, O. C., additional, Straus, T., additional, Susino, R., additional, Teriaca, L., additional, del Toro Iniesta, J. C., additional, Ventura, R., additional, Verbeeck, C., additional, Vilmer, N., additional, Warmuth, A., additional, Walsh, A. P., additional, Watson, C., additional, Williams, D., additional, Wu, Y., additional, and Zhukov, A. N., additional

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2020
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23. Metis: the Solar Orbiter visible light and ultraviolet coronal imager

Author

Antonucci, Ester, primary, Romoli, Marco, additional, Andretta, Vincenzo, additional, Fineschi, Silvano, additional, Heinzel, Petr, additional, Moses, J. Daniel, additional, Naletto, Giampiero, additional, Nicolini, Gianalfredo, additional, Spadaro, Daniele, additional, Teriaca, Luca, additional, Berlicki, Arkadiusz, additional, Capobianco, Gerardo, additional, Crescenzio, Giuseppe, additional, Da Deppo, Vania, additional, Focardi, Mauro, additional, Frassetto, Fabio, additional, Heerlein, Klaus, additional, Landini, Federico, additional, Magli, Enrico, additional, Marco Malvezzi, Andrea, additional, Massone, Giuseppe, additional, Melich, Radek, additional, Nicolosi, Piergiorgio, additional, Noci, Giancarlo, additional, Pancrazzi, Maurizio, additional, Pelizzo, Maria G., additional, Poletto, Luca, additional, Sasso, Clementina, additional, Schühle, Udo, additional, Solanki, Sami K., additional, Strachan, Leonard, additional, Susino, Roberto, additional, Tondello, Giuseppe, additional, Uslenghi, Michela, additional, Woch, Joachim, additional, Abbo, Lucia, additional, Bemporad, Alessandro, additional, Casti, Marta, additional, Dolei, Sergio, additional, Grimani, Catia, additional, Messerotti, Mauro, additional, Ricci, Marco, additional, Straus, Thomas, additional, Telloni, Daniele, additional, Zuppella, Paola, additional, Auchère, Frederic, additional, Bruno, Roberto, additional, Ciaravella, Angela, additional, Corso, Alain J., additional, Alvarez Copano, Miguel, additional, Aznar Cuadrado, Regina, additional, D’Amicis, Raffaella, additional, Enge, Reiner, additional, Gravina, Alessio, additional, Jejčič, Sonja, additional, Lamy, Philippe, additional, Lanzafame, Alessandro, additional, Meierdierks, Thimo, additional, Papagiannaki, Ioanna, additional, Peter, Hardi, additional, Fernandez Rico, German, additional, Giday Sertsu, Mewael, additional, Staub, Jan, additional, Tsinganos, Kanaris, additional, Velli, Marco, additional, Ventura, Rita, additional, Verroi, Enrico, additional, Vial, Jean-Claude, additional, Vives, Sebastien, additional, Volpicelli, Antonio, additional, Werner, Stephan, additional, Zerr, Andreas, additional, Negri, Barbara, additional, Castronuovo, Marco, additional, Gabrielli, Alessandro, additional, Bertacin, Roberto, additional, Carpentiero, Rita, additional, Natalucci, Silvia, additional, Marliani, Filippo, additional, Cesa, Marco, additional, Laget, Philippe, additional, Morea, Danilo, additional, Pieraccini, Stefano, additional, Radaelli, Paolo, additional, Sandri, Paolo, additional, Sarra, Paolo, additional, Cesare, Stefano, additional, Del Forno, Felice, additional, Massa, Ernesto, additional, Montabone, Mauro, additional, Mottini, Sergio, additional, Quattropani, Daniele, additional, Schillaci, Tiziano, additional, Boccardo, Roberto, additional, Brando, Rosario, additional, Pandi, Arianna, additional, Baietto, Cristian, additional, Bertone, Riccardo, additional, Alvarez-Herrero, Alberto, additional, García Parejo, Pilar, additional, Cebollero, María, additional, Amoruso, Mauro, additional, and Centonze, Vito, additional

Published
2020
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24. Coordination within the remote sensing payload on the Solar Orbiter mission

Author

Auchère, F., primary, Andretta, V., additional, Antonucci, E., additional, Bach, N., additional, Battaglia, M., additional, Bemporad, A., additional, Berghmans, D., additional, Buchlin, E., additional, Caminade, S., additional, Carlsson, M., additional, Carlyle, J., additional, Cerullo, J. J., additional, Chamberlin, P. C., additional, Colaninno, R. C., additional, Davila, J. M., additional, De Groof, A., additional, Etesi, L., additional, Fahmy, S., additional, Fineschi, S., additional, Fludra, A., additional, Gilbert, H. R., additional, Giunta, A., additional, Grundy, T., additional, Haberreiter, M., additional, Harra, L. K., additional, Hassler, D. M., additional, Hirzberger, J., additional, Howard, R. A., additional, Hurford, G., additional, Kleint, L., additional, Kolleck, M., additional, Krucker, S., additional, Lagg, A., additional, Landini, F., additional, Long, D. M., additional, Lefort, J., additional, Lodiot, S., additional, Mampaey, B., additional, Maloney, S., additional, Marliani, F., additional, Martinez-Pillet, V., additional, McMullin, D. R., additional, Müller, D., additional, Nicolini, G., additional, Orozco Suarez, D., additional, Pacros, A., additional, Pancrazzi, M., additional, Parenti, S., additional, Peter, H., additional, Philippon, A., additional, Plunkett, S., additional, Rich, N., additional, Rochus, P., additional, Rouillard, A., additional, Romoli, M., additional, Sanchez, L., additional, Schühle, U., additional, Sidher, S., additional, Solanki, S. K., additional, Spadaro, D., additional, St Cyr, O. C., additional, Straus, T., additional, Tanco, I., additional, Teriaca, L., additional, Thompson, W. T., additional, del Toro Iniesta, J. C., additional, Verbeeck, C., additional, Vourlidas, A., additional, Watson, C., additional, Wiegelmann, T., additional, Williams, D., additional, Woch, J., additional, Zhukov, A. N., additional, and Zouganelis, I., additional

Published
2020
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25. Hydrogen non-equilibrium ionisation effects in coronal mass ejections

Author

Alessandro Bemporad, Paolo Pagano, Duncan H. Mackay, Science & Technology Facilities Council, European Research Council, University of St Andrews. Applied Mathematics, Pagano P., Bemporad A., and Mackay D.H.

Subjects
Magnetohydrodynamics (MHD), 010504 meteorology & atmospheric sciences, Hydrogen, Sun: coronal mass ejections (CMEs), FOS: Physical sciences, chemistry.chemical_element, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, coronal mass ejections (CMEs) [un], Ionization, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, data analysis [Methods], Sun: magnetic fields, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QC, QB, 0105 earth and related environmental sciences, Physics, UV radiation [Sun], Sun: corona, Astronomy and Astrophysics, 3rd-DAS, Plasma, Magnetic flux, Solar wind, QC Physics, Astrophysics - Solar and Stellar Astrophysics, chemistry, Space and Planetary Science, Physics::Space Physics, Plasma diagnostics, Magnetohydrodynamics
Abstract

This research has received funding from the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1 and the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 647214). D.H.M. would like to thank both the UK STFC and the ERC (Synergy grant: WHOLE SUN, grant Agreement No. 810218) for financial support. D.H.M. and P.P. would like to thank STFC for IAA funding under grant number SMC1-XAS012. This work used the DiRAC@Durham facility man-aged by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk. The equipment was funded by BEIS capital funding via STFC capital grants ST/P002293/1, ST/R002371/1 and ST/S002502/1,Durham University and STFC operations grant ST/R000832/1. DiRAC is part of the National e-Infrastructure. We acknowledge the use of the open source (gitorious.org/amrvac) MPI-AMRVAC software, relying on coding efforts from C. Xia, O.Porth, R. Keppens. CHIANTI is a collaborative project involving George Mason University, the University of Michigan(USA), University of Cambridge (UK) and NASA Goddard Space Flight Center (USA). Context. A new generation of coronagraphs used to study solar wind and coronal mass ejections (CMEs) are being developed and launched. These coronagraphs will heavily rely on multi-channel observations where visible light (VL) and UV-EUV (ultraviolet-extreme ultraviolet) observations provide new plasma diagnostics. One of these instruments, Metis on board ESA-Solar Orbiter, will simultaneously observe VL and the UV Lyman-α line. The number of neutral hydrogen atoms (a small fraction of coronal protons) is a key parameter for deriving plasma properties, such as the temperature from the observed Lyman-α line intensity. However, these measurements are significantly affected if non-equilibrium ionisation effects occur, which can be relevant during CMEs. Aims. The aim of this work is to determine if non-equilibrium ionisation effects are relevant in CMEs and, in particular, when and in which regions of the CME plasma ionisation equilibrium can be assumed for data analysis. Methods. We used a magneto-hydrodynamic (MHD) simulation of a magnetic flux rope ejection to generate a CME. From this, we then reconstructed the ionisation state of hydrogen atoms in the CME by evaluating both the advection of neutral and ionised hydrogen atoms and the ionisation and recombination rates in the MHD simulation. Results. We find that the equilibrium ionisation assumption mostly holds in the core of the CME, which is represented by a magnetic flux rope. In contrast, non-equilibrium ionisation effects are significant at the CME front, where we find about 100 times more neutral hydrogen atoms than prescribed by ionisation equilibrium conditions. We find this to be the case even if this neutral hydrogen excess might be difficult to identify due to projection effects. Conclusions. This work provides key information for the development of a new generation of diagnostic techniques that aim to combine visible light and Lyman-α line emissions. The results show that non-equilibrium ionisation effects need to be considered when we analyse CME fronts. Incorrectly assuming equilibrium ionisation in these regions would lead to a systematic underestimate of plasma temperatures. Postprint

Published
2020
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27. Combining white light and UV Lyman-α coronagraphic images to determine the solar wind speed

Author

L. Zangrilli, F. Frassati, Alessandro Bemporad, and Silvio Giordano

Subjects
Solar minimum, Physics, FOS: Physical sciences, Inverse transform sampling, Astronomy and Astrophysics, Context (language use), Inversion (meteorology), Astrophysics, Corona, Computational physics, Solar wind, Wavelength, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Magnetohydrodynamics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

This work focuses on the combination of White Light (WL) and UV (Ly-alpha) coronagraphic images to demonstrate the capability to measure the solar wind speed in the inner corona directly with the ratio between these two images (a technique called "quick inversion method"), thus avoiding to account for the line-of-sight (LOS) integration effects in the inversion of data. After a derivation of the theoretical basis and illustration of the main hypotheses in the "quick inversion method", the data inversion technique is tested first with 1D radial analytic profiles, and then with 3D numerical MHD simulations, in order to show the effects of variabilities related with different phases of solar activity cycle and complex LOS distribution of plasma parameters. The same technique is also applied to average WL and UV images obtained from real data acquired by SOHO UVCS and LASCO instruments around the minimum and maximum of the solar activity cycle. Comparisons between input and output velocities show overall a good agreement, demonstrating that this method that allows to infer the solar wind speed with WL-UV image ratio can be complementary to more complex techniques requiring the full LOS integration. The analysis described here also allowed us to quantify the possible errors in the outflow speed, and to identify the coronal regions where the "quick inversion method" performs at the best. The "quick inversion" applied to real UVCS and LASCO data allowed also to reconstruct the typical bimodal distribution of fast and slow wind at solar minimum, and to derive a more complex picture around solar maximum. The application of the technique shown here will be very important for the future analyses of data acquired with multichannel WL and UV (Ly-alpha) coronagraphs, such as Metis on-board Solar Orbiter, LST on-board ASO-S, and any other future WL and UV Ly-alpha multi-channel coronagraph., 14 pages, 8 figures, accepted for Astronomy & Astrophysics

Published
2021
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28. Effects of the chromospheric Lyα line profile shape on the determination of the solar wind H I outflow velocity using the Doppler dimming technique

Author

P. Romano, Rita Ventura, G. E. Capuano, V. Da Deppo, L. Zangrilli, Salvo L. Guglielmino, F. Frassetto, Alessandro Bemporad, G. Nicolini, Roberto Susino, V. Andretta, S. Dolei, Maurizio Pancrazzi, Daniele Spadaro, Marco Romoli, Silvio Giordano, Clementina Sasso, and Federico Landini

Subjects
Physics, Range (particle radiation), media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics, Radiation, Asymmetry, symbols.namesake, Solar wind, Acceleration, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physics::Space Physics, symbols, Astrophysics::Solar and Stellar Astrophysics, Outflow, Astrophysics::Earth and Planetary Astrophysics, Doppler effect, Line (formation), media_common
Abstract

The determination of solar wind outflow velocity is fundamental in order to probe the mechanisms of wind acceleration in the corona. We aim to study, via the Doppler dimming technique, the effects that the chromospheric Ly{\alpha} line profile shape causes on the determination of the outflow speed of coronal HI atoms. The Doppler dimming technique takes into account the decrease of coronal Ly{\alpha} radiation in regions where HI atoms flow out in the solar wind. Starting from UV observations (UVCS/SOHO) of the coronal Ly{\alpha} line and simultaneous measurements of pB (LASCO/SOHO and Mk3/MLSO), we studied the effect of the pumping chromospheric Ly{\alpha} line profile through measurements from SOHO/SUMER, UVSP/SMM and LPSP/OSO-8, taken from representative on-disk regions and as a function of time during the solar activity cycle. In particular, we considered the effect of four chromospheric line parameters: line width, depth of the central reversal, asymmetry and distance of the peaks. We find that the range of variability of these parameters is of about 50% for the width, 69% for the depth of the central reversal, 35% for the asymmetry, and 50% for the distance of the peaks. Then, we find that the variability of the pumping Ly{\alpha} profile affects the estimates of the coronal HI velocity by about 9-12%. Therefore, this uncertainty is smaller than other physical quantities uncertainties, and a constant in time and unique shape of the Ly{\alpha} profile over the solar disk can be adopted in order to estimate the solar wind outflow velocity., Comment: 12 pages, 10 figures, 1 table, it will appear in "Astronomy & Astrophysics", accepted for "ESPM-16" and "SWICo 2021", the uploaded abstract is abridged

Published
2021
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29. Radio evidence for a shock wave reflected by a coronal hole

Author

Silvio Giordano, Alessandro Bemporad, Salvatore Mancuso, Carla Taricco, Daniele Telloni, Federica Frassati, and D. Barghini

Subjects
Shock wave, 010504 meteorology & atmospheric sciences, Sun: coronal mass ejections (CMEs), Astrophysics::High Energy Astrophysical Phenomena, Extreme ultraviolet lithography, Sun: radio radiation, shock waves, Sun: activity, Sun: corona, Sun: coronal mass ejections (CMEs), Sun: magnetic fields, FOS: Physical sciences, Coronal hole, Astrophysics, 01 natural sciences, Sun: activity, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sun: magnetic fields, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Sun: radio radiation, Sun: corona, Astronomy and Astrophysics, shock waves, Corona, Shock (mechanics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Extreme ultraviolet, Physics::Space Physics, Reflection (physics)
Abstract

We report the first unambiguous observational evidence in the radio range of the reflection of a coronal shock wave at the boundary of a coronal hole. The event occurred above an active region located at the northwest limb of the Sun and was characterized by an eruptive prominence and an extreme-ultraviolet (EUV) wave steepening into a shock. The EUV observations acquired by the Atmospheric Imaging Assembly (AIA) instrument on board the Solar Dynamics Observatory(SDO) and the Extreme Ultraviolet Imager (EUVI) instrument on board the Solar TErrestrial RElations Observatory(STEREO-A) were used to track the development of the EUV front in the inner corona. Metric type II radio emission, a distinguishing feature of shock waves propagating in the inner corona, was simultaneously recorded by ground-based radio spectrometers. The radio dynamic spectra displayed an unusual reversal of the type II emission lanes, together with type III-like herringbone emission, indicating shock-accelerated electron beams. Combined analysis of imaging data from the two space-based EUV instruments and the Nancay Radioheliograph (NRH) evidences that the reverse-drifting typeiiemission was produced at the intersection of the shock front, reflected at a coronal hole boundary, with an intervening low-Alfv\'en-speed region characterized by an open field configuration. We also provide an outstanding data-driven reconstruction of the spatiotemporal evolution in the inner corona of the shock-accelerated electron beams produced by the reflected shock., Comment: Accepted by Astronomy & Astrophysics, 6 pages, 7 figures

Published
2021
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30. Effect of the non-uniform solar chromospheric Lyα radiation on determining the coronal H I outflow velocity

Author

Dolei, S., primary, Spadaro, D., additional, Ventura, R., additional, Bemporad, A., additional, Andretta, V., additional, Sasso, C., additional, Susino, R., additional, Antonucci, E., additional, Da Deppo, V., additional, Fineschi, S., additional, Frassetto, F., additional, Landini, F., additional, Naletto, G., additional, Nicolini, G., additional, Pancrazzi, M., additional, and Romoli, M., additional

Published
2019
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31. Comparing extrapolations of the coronal magnetic field structure at 2.5R⊙with multi-viewpoint coronagraphic observations

Author

Sasso, C., primary, Pinto, R. F., additional, Andretta, V., additional, Howard, R. A., additional, Vourlidas, A., additional, Bemporad, A., additional, Dolei, S., additional, Spadaro, D., additional, Susino, R., additional, Antonucci, E., additional, Abbo, L., additional, Da Deppo, V., additional, Fineschi, S., additional, Frassetto, F., additional, Landini, F., additional, Naletto, G., additional, Nicolini, G., additional, Nicolosi, P., additional, Pancrazzi, M., additional, Romoli, M., additional, Telloni, D., additional, and Ventura, R., additional

Published
2019
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33. Mapping the solar wind HI outflow velocity in the inner heliosphere by coronagraphic ultraviolet and visible-light observations

Author

Gianalfredo Nicolini, Daniele Telloni, Roberto Susino, Ester Antonucci, Clementina Sasso, Rita Ventura, Vincenzo Andretta, S. Dolei, Silvano Fineschi, Lucia Abbo, Giampiero Naletto, F. Frassetto, Maurizio Pancrazzi, Daniele Spadaro, Piergiorgio Nicolosi, Marco Romoli, Mauro Focardi, V. Da Deppo, Federico Landini, Alessandro Bemporad, Silvio Giordano, and ITA

Subjects
Brightness, 010504 meteorology & atmospheric sciences, Solar wind, Astrophysics, 01 natural sciences, law.invention, Orbiter, law, Sun: corona, Sun: UV radiation, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), Physics, Corona, Physics::Space Physics, Solar rotation, Outflow, Astrophysics::Earth and Planetary Astrophysics, Heliosphere
Abstract

We investigated the capability of mapping the solar wind outflow velocity of neutral hydrogen atoms by using synergistic visible-light and ultraviolet observations. We used polarised brightness images acquired by the LASCO/SOHO and Mk3/MLSO coronagraphs, and synoptic Lyα line observations of the UVCS/SOHO spectrometer to obtain daily maps of solar wind H I outflow velocity between 1.5 and 4.0 R⊙ on the SOHO plane of the sky during a complete solar rotation (from 1997 June 1 to 1997 June 28). The 28-days data sequence allows us to construct coronal off-limb Carrington maps of the resulting velocities at different heliocentric distances to investigate the space and time evolution of the outflowing solar plasma. In addition, we performed a parameter space exploration in order to study the dependence of the derived outflow velocities on the physical quantities characterising the Lyα emitting process in the corona. Our results are important in anticipation of the future science with the Metis instrument, selected to be part of the Solar Orbiter scientific payload. It was conceived to carry out near-sun coronagraphy, performing for the first time simultaneous imaging in polarised visible-light and ultraviolet H I Lyα line, so providing an unprecedented view of the solar wind acceleration region in the inner corona.

Published
2018

34. Measuring the electron temperatures of coronal mass ejections with future space-based multi-channel coronagraphs: a numerical test

Author

Silvio Giordano, Paolo Pagano, Alessandro Bemporad, Bemporad A., Pagano P., Giordano S., European Research Council, University of St Andrews. Applied Mathematics, ITA, and GBR

Subjects
010504 meteorology & atmospheric sciences, Sun: coronal mass ejections (CMEs), Plasma parameters, T-NDAS, Context (language use), Astrophysics, 01 natural sciences, symbols.namesake, Methods: data analysis, 0103 physical sciences, Radiative transfer, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, data analysis [Methods], 010303 astronomy & astrophysics, QC, QB, 0105 earth and related environmental sciences, Physics, UV radiation [Sun], numerical [Methods], Methods: numerical, Astronomy and Astrophysics, Plasma, Sun: UV radiation, Polarization (waves), coronal mass ejections (CMEs) [Sun], Computational physics, QC Physics, Plasmas, Space and Planetary Science, Physics::Space Physics, symbols, Magnetohydrodynamics, Doppler effect
Abstract

Context. The determination from coronagraphic observations of physical parameters of the plasma embedded in coronal mass ejections (CMEs) is of crucial importance for our understanding of the origin and evolution of these phenomena. Aims. The aim of this work is to perform the first ever numerical simulations of a CME as it will be observed by future two-channel (visible light VL and UV Ly-α) coronagraphs, such as the Metis instrument on-board ESA-Solar Orbiter mission, or any other future coronagraphs with the same spectral band-passes. These simulations are then used to test and optimize the plasma diagnostic techniques to be applied to future observations of CMEs. Methods. The CME diagnostic techniques are tested here by analyzing synthetic coronagraphic observations. First, a numerical three-dimensional (3D) magnetohydrodynamic (MHD) simulation of a CME is performed, and the plasma parameters in the simulation are used to generate synthetic visible light (VL) and ultraviolet (UV) coronagraphic two-dimensional (2D) images of the eruption (i.e., integrated along the line-of-sight). Second, synthetic data are analyzed with different assumptions (as will be done with real data), to infer the kinematic properties of the CME (such as the extension along the line-of-sight of the emitting region, the expansion speed, and the CME propagation direction), as well as physical parameters of the CME plasma (the plasma electron density and temperature). A comparison between input parameters from the simulation and output parameters from the synthetic data analysis is then performed. Results. The inversion of VL polarized data allows to successfully determine the CME speed and 3D propagation direction (with the polarization ratio technique), as well as to derive information on the extension along the line-of-sight of the emitting plasma, a crucial parameter needed to convert the plasma electron column densities into number densities. These parameters are used to analyze UV Ly-α images and to estimate the CME plasma temperature, also taking into account Doppler dimming effect. Output plasma temperatures are in general underestimated, both in the CME body and core regions. By neglecting the UV Ly-α radiative excitation of H atoms, reliable temperatures can be more easily derived in the CME core (within ∼60%). On the other hand, we show that a determination of temperatures (within ∼20−30%) in the CME body requires 2D maps of CME radial speeds and Doppler dimming coefficients to be derived.

Published
2018
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35. Effect of the non-uniform solar chromospheric Lyα radiation on determining the coronal H I outflow velocity

Author

Daniele Spadaro, Ester Antonucci, F. Frassetto, Giampiero Naletto, Maurizio Pancrazzi, Gianalfredo Nicolini, Vincenzo Andretta, Federico Landini, Rita Ventura, V. Da Deppo, Clementina Sasso, Alessandro Bemporad, S. Dolei, Roberto Susino, Silvano Fineschi, Marco Romoli, and ITA

Subjects
Solar minimum, Brightness, 010504 meteorology & atmospheric sciences, Solar wind, Astrophysics, Radiation, 01 natural sciences, symbols.namesake, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), Physics, Sun: corona, Astronomy and Astrophysics, Sun: UV radiation, Corona, Space and Planetary Science, Physics::Space Physics, symbols, Outflow, Astrophysics::Earth and Planetary Astrophysics, Doppler effect
Abstract

We derived maps of the solar wind outflow velocity of coronal neutral hydrogen atoms at solar minimum in the altitude range 1.5–4.0 R⊙. We applied the Doppler dimming technique to coronagraphic observations in the UV H I Lyα line at 121.6 nm. The technique exploits the intensity reduction in the coronal line with increasing velocities of the outflowing plasma to determine the solar wind velocity by iterative modelling. The Lyα line intensity is sensitive to the wind outflow velocity and also depends on the physical properties of coronal particles and underlying chromospheric emission. Measurements of irradiance by the chromospheric Lyα radiation in the corona are required for a rigorous application of the Doppler dimming technique, but they are not provided by past and current instrumentations. A correlation function between the H I 121.6 nm and He II 30.4 nm line intensities was used to construct Carrington rotation maps of the non-uniform solar chromospheric Lyα radiation and thus to compute the Lyα line irradiance throughout the outer corona. Approximations concerning the temperature of the scattering H I atoms and exciting solar disc radiation were also adopted to significantly reduce the computational time and obtain a faster procedure for a quick-look data analysis of future coronagraphic observations. The effect of the chromospheric Lyα brightness distribution on the resulting H I outflow velocities was quantified. In particular, we found that the usual uniform-disc approximation systematically leads to an overestimated velocity in the polar and mid-latitude coronal regions up to a maximum of about 50−60 km s−1 closer to the Sun. This difference decreases at higher altitudes, where an increasingly larger chromospheric portion, including both brighter and darker disc features, contributes to illuminate the solar corona, and the non-uniform radiation condition progressively approaches the uniform-disc approximation.

Published
2019
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39. Mapping the solar wind HI outflow velocity in the inner heliosphere by coronagraphic ultraviolet and visible-light observations

Author

Dolei, S., primary, Susino, R., additional, Sasso, C., additional, Bemporad, A., additional, Andretta, V., additional, Spadaro, D., additional, Ventura, R., additional, Antonucci, E., additional, Abbo, L., additional, Da Deppo, V., additional, Fineschi, S., additional, Focardi, M., additional, Frassetto, F., additional, Giordano, S., additional, Landini, F., additional, Naletto, G., additional, Nicolini, G., additional, Nicolosi, P., additional, Pancrazzi, M., additional, Romoli, M., additional, and Telloni, D., additional

Published
2018
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40. Depth profiling and morphological characterization of AlN thin films deposited on Si substrates using a reactive sputter magnetron

Author

Alberto Somoza, Sebastiano Mariazzi, Roberto S. Brusa, Jorge Feugeas, J. Bürgi, Mattia Piccoli, Carlos Eugenio Macchi, Javier García Molleja, Edoardo Bemporad, Macchi, C, Burgi, J, Garcıa Molleja, J, Mariazzi, S, Piccoli, Mattia, Bemporad, Edoardo, Feugeas, J, Sennen Brusa, R, and Somoza, A.

Subjects
Materials science, Silicon, business.industry, Ciencias Físicas, Positron annihilation, Analytical chemistry, Reactive sputter magnetron, chemistry.chemical_element, Substrate (electronics), Nitride, Condensed Matter Physics, Electronic, Optical and Magnetic Materials, Positron annihilation spectroscopy, chemistry, Sputtering, Cavity magnetron, Optoelectronics, Thin film, Spectroscopy, business, Instrumentation, Aluminum nitride, CIENCIAS NATURALES Y EXACTAS, Films, Física de los Materiales Condensados
Abstract

It is well-known that the characteristics of aluminum nitride thin films mainly depend on their morphologies, the quality of the film-substrate interfaces and the open volume defects. A study of the depth profiling and morphological characterization of AlN thin films deposited on two types of Si substrates is presented. Thin films of thicknesses between 200 and 400 nm were deposited during two deposition times using a reactive sputter magnetron. These films were characterized by means of X-ray diffraction and imaging techniques (SEM and TEM). To analyze the composition of the films, energy dispersive X-ray spectroscopy was applied. Positron annihilation spectroscopy, specifically Doppler broadening spectroscopy, was used to gather information on the depth profiling of open volume defects inside the films and the AlN films-Si substrate interfaces. The results are interpreted in terms of the structural changes induced in the films as a consequence of changes in the deposition time (i.e., thicknesses) and of the orientation of the substrates. Fil: Macchi, Carlos Eugenio. Universidad Nacional del Centro de la Provincia de Buenos Aires. Facultad de Ciencias Exactas. Instituto de Física de Materiales; Argentina Fil: Burgi, Juan Mauel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Rosario. Instituto de Física de Rosario (i); Argentina Fil: García Molleja, Javier. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Rosario. Instituto de Física de Rosario (i); Argentina Fil: Mariazzi, Sebastiano. Universitá di Trento. Dipartimento di Fisica; Italia Fil: Piccoli, Mattia. Universitá di Roma Tre. Dipartimento di Ingegneria Meccanica ed Industriale; Italia Fil: Bemporad, Edoardo. Universitá di Roma Tre. Dipartimento di Ingegneria Meccanica ed Industriale; Italia Fil: Feugeas, Jorge Nestor. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Rosario. Instituto de Física de Rosario (i); Argentina Fil: Sennen Brusa, Roberto . Universitá di Trento. Dipartimento di Fisica; Italia Fil: Somoza, Alberto Horacio. Universidad Nacional del Centro de la Provincia de Buenos Aires. Facultad de Ciencias Exactas. Instituto de Física de Materiales; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas; Argentina

Published
2014

42. Comparing extrapolations of the coronal magnetic field structure at 2.5 R⊙ with multi-viewpoint coronagraphic observations.

Author

Sasso, C., Pinto, R. F., Andretta, V., Howard, R. A., Vourlidas, A., Bemporad, A., Dolei, S., Spadaro, D., Susino, R., Antonucci, E., Abbo, L., Da Deppo, V., Fineschi, S., Frassetto, F., Landini, F., Naletto, G., Nicolini, G., Nicolosi, P., Pancrazzi, M., and Romoli, M.

Subjects
MAGNETIC structure, MAGNETIC fields, EXTRAPOLATION, SOLAR corona, SOLAR magnetic fields, ROTATION of the Sun
Abstract

The magnetic field shapes the structure of the solar corona, but we still know little about the interrelationships between the coronal magnetic field configurations and the resulting quasi-stationary structures observed in coronagraphic images (such as streamers, plumes, and coronal holes). One way to obtain information on the large-scale structure of the coronal magnetic field is to extrapolate it from photospheric data and compare the results with coronagraphic images. Our aim is to verify whether this comparison can be a fast method to systematically determine the reliability of the many methods that are available for modeling the coronal magnetic field. Coronal fields are usually extrapolated from photospheric measurements that are typically obtained in a region close to the central meridian on the solar disk and are then compared with coronagraphic images at the limbs, acquired at least seven days before or after to account for solar rotation. This implicitly assumes that no significant changes occurred in the corona during that period. In this work, we combine images from three coronagraphs (SOHO/LASCO-C2 and the two STEREO/SECCHI-COR1) that observe the Sun from different viewing angles to build Carrington maps that cover the entire corona to reduce the effect of temporal evolution to about five days. We then compare the position of the observed streamers in these Carrington maps with that of the neutral lines obtained from four different magnetic field extrapolations to evaluate the performances of the latter in the solar corona. Our results show that the location of coronal streamers can provide important indications to distinguish between different magnetic field extrapolations. [ABSTRACT FROM AUTHOR]

Published
2019
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45. Model predictive control application to spacecraft rendezvous in mars sample return scenario

Author

Saponara, M., Barrena, V., Bemporad, A., Hartley, E.N., Maciejowski, J.M., Richards, A.G., Tramutola, A., and Trodden, P.

Abstract

Model Predictive Control (MPC) is an optimization-based control strategy that is considered extremely attractive in the autonomous space rendezvous scenarios. The Online Recon¦guration Control System and Avionics Architecture (ORCSAT) study addresses its applicability in Mars Sample Return (MSR) mission, including the implementation of the developed solution in a space representative avionic architecture system. With respect to a classical control solution High-integrity Autonomous RendezVous and Docking control system (HARVD), MPC allows a signi¦cant performance improvement both in trajectory and in propellant save. Furthermore, thanks to the online optimization, it allows to identify improvements in other areas (i. e., at mission de¦nition level) that could not be known a priori.

Published
2013

46. Model predictive control application to spacecraft rendezvous in mars sample return scenario

Author

Edward N. Hartley, A. Tramutola, Arthur Richards, Paul Trodden, V. Barrena, M. Saponara, Jan M. Maciejowski, and Alberto Bemporad

Subjects
Engineering, Model predictive control, business.industry, Control system, Real-time computing, Rendezvous, A priori and a posteriori, Performance improvement, Architecture, Avionics, business, Simulation, Space rendezvous
Abstract

Model Predictive Control (MPC) is an optimization-based control strategy that is considered extremely attractive in the autonomous space rendezvous scenarios. The Online Recon¦guration Control System and Avionics Architecture (ORCSAT) study addresses its applicability in Mars Sample Return (MSR) mission, including the implementation of the developed solution in a space representative avionic architecture system. With respect to a classical control solution High-integrity Autonomous RendezVous and Docking control system (HARVD), MPC allows a signi¦cant performance improvement both in trajectory and in propellant save. Furthermore, thanks to the online optimization, it allows to identify improvements in other areas (i. e., at mission de¦nition level) that could not be known a priori.

Published
2013
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47. ($ \begin{array}{ccc}1& 0& \begin{array}{cc}\bar{1}& 1\end{array}\end{array}$) preferential orientation of polycrystalline AlN grown on SiO2/Si wafers by reactive sputter magnetron technique

Author

Javier García Molleja, Edoardo Bemporad, Raul Eduardo Bolmaro, J. Bürgi, Mattia Piccoli, Jorge Feugeas, and Aldo F. Craievich

Subjects
010302 applied physics, Diffraction, Materials science, Condensed matter physics, Nanotechnology, 02 engineering and technology, Substrate (electronics), Nitride, 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Electronic, Optical and Magnetic Materials, Orientation (vector space), Sputtering, 0103 physical sciences, Cavity magnetron, Crystallite, Texture (crystalline), 0210 nano-technology, Instrumentation
Abstract

Aluminum nitride (AlN) is a ceramic compound that could be used as a processing material for semiconductor industry. However, the AlN crystalline structure plays a crucial role in its performance. In this paper, polycrystalline AlN films have been grown onto Si(1 1 1) and Si(1 0 0) (with an oxide native coverage of SiO 2 ) wafers by RSM (reactive sputter magnetron) technique using a small (5 L) reactor. The development of polycrystalline AlN films with a good texture along ( 1 0 1 ¯ 1 $ \begin{array}{ccc}1& 0& \begin{array}{cc}\bar{1}& 1\end{array}\end{array}$ ) planes, i.e., semi-polar structure, was shown. Analyses were done using X-ray diffraction in the Bragg-Brentano mode and in the GIXRD (grazing incidence X-ray diffraction) one, and the texture was determined through pole figures. The structure and composition of these films were also studied by TEM and EDS techniques. Nevertheless, the mapping of the magnetic field between the magnetron and the substrate has shown a lack of symmetry at the region near the substrate. This lack of symmetry can be attributable to the small dimensions of the chamber, and the present paper suggests that this phenomenon is the responsible for the unusual ( 1 0 1 ¯ 1 $ \begin{array}{ccc}1& 0& \begin{array}{cc}\bar{1}& 1\end{array}\end{array}$ ) texture developed.

Published
2016
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