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1. The Solar Orbiter Heliospheric Imager (SoloHI)

Author

J. J. Cerullo, Dennis Wang, Simon Plunkett, P. L. Lamy, S. Yerushalmi, A. P. Rouillard, J.-P. Halain, A. Thernisien, R. Baugh, D. H. Chua, R. A. Howard, Guillermo Stenborg, Robin C. Colaninno, M. T. Carter, Samuel Tun-Beltran, Spiros Patsourakos, R. Hagood, F. Auchere, Angelos Vourlidas, Sean Lynch, Dennis G. Socker, Richard A. Harrison, L. Smith, Volker Bothmer, Holly Gilbert, Greg Clifford, James Robert Janesick, Pierre Rochus, Mark Grygon, Clarence M. Korendyke, S. Koss, D. R. McMullin, Marco Velli, O. C. St. Cyr, A. Uhl, C. Mariano, P. C. Liewer, H. Dennison, K. Eisenhauer, N. Rich, T. Hunt, Jon A. Linker, Mark G. Linton, David Keller, John Robertson Tower, Adam Thurn, H. M. Maldonado, R. Farkas, Naval Research Laboratory (NRL), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Space Systems Research Corporation (SSRC), Silver Engineering, Inc., SRI International, Stinger Ghaffarian Technologies, Inc. (SGT, Inc.), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), University of California [Los Angeles] (UCLA), University of California (UC), Predictive Sciences Inc., Georg-August-University = Georg-August-Universität Göttingen, Centre Spatial de Liège (CSL), Université de Liège, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), 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), University of Ioannina, NASA Goddard Space Flight Center (GSFC), ASRC Federal Space and Defense, University of California, Georg-August-University [Göttingen], European Space Agency (ESA), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), 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), and 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)

Subjects
Physics, Zodiacal light, 010504 meteorology & atmospheric sciences, Data products, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], zodiacal dust, Sun, Astronomy and Astrophysics, telescopes, Astrophysics, Solar physics, 01 natural sciences, law.invention, Orbiter, Space and Planetary Science, law, 0103 physical sciences, Thermal, space vehicles, Aerospace engineering, business, 010303 astronomy & astrophysics, corona, 0105 earth and related environmental sciences
Abstract

Aims. We present the design and pre-launch performance of the Solar Orbiter Heliospheric Imager (SoloHI) which is an instrument prepared for inclusion in the ESA/NASA Solar Orbiter mission, currently scheduled for launch in 2020.Methods. The goal of this paper is to provide details of the SoloHI instrument concept, design, and pre-flight performance to give the potential user of the data a better understanding of how the observations are collected and the sources that contribute to the signal.Results. The paper discusses the science objectives, including the SoloHI-specific aspects, before presenting the design concepts, which include the optics, mechanical, thermal, electrical, and ground processing. Finally, a list of planned data products is also presented.Conclusions. The performance measurements of the various instrument parameters meet or exceed the requirements derived from the mission science objectives. SoloHI is poised to take its place as a vital contributor to the science success of the Solar Orbiter mission.

Published
2020

2. The Wide-Field Imager for Solar Probe Plus (WISPR)

Author

Jeff S. Morrill, A. Thernisien, Pierre Rochus, Jeffrey R. Hall, Damien H. Chua, Simon Plunkett, Adam Thurn, Emmanuel Mazy, Volker Bothmer, Phares J. Grey, Russell A. Howard, Dennis G. Socker, Clarence M. Korendyke, E. M. DeJong, Jens Rodmann, Marco Velli, Zoran Mikic, Mark G. Linton, Sean Lynch, N. Rich, Greg Clifford, P. C. Liewer, Dennis Wang, R. Hagood, M. T. Carter, Peter Van Duyne, and Angelos Vourlidas

Subjects
Physics, Earth's orbit, 010504 meteorology & atmospheric sciences, Spacecraft, business.industry, Thomson scattering, Detector, Astronomy, Astronomy and Astrophysics, Solar radius, 01 natural sciences, Corona, Solar wind, Optics, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Orbit (dynamics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The Wide-field Imager for Solar PRobe Plus (WISPR) is the sole imager aboard the Solar Probe Plus (SPP) mission scheduled for launch in 2018. SPP will be a unique mission designed to orbit as close as 7 million km (9.86 solar radii) from Sun center. WISPR employs a 95∘ radial by 58∘ transverse field of view to image the fine-scale structure of the solar corona, derive the 3D structure of the large-scale corona, and determine whether a dust-free zone exists near the Sun. WISPR is the smallest heliospheric imager to date yet it comprises two nested wide-field telescopes with large-format (2 K × 2 K) APS CMOS detectors to optimize the performance for their respective fields of view and to minimize the risk of dust damage, which may be considerable close to the Sun. The WISPR electronics are very flexible allowing the collection of individual images at cadences up to 1 second at perihelion or the summing of multiple images to increase the signal-to-noise when the spacecraft is further from the Sun. The dependency of the Thomson scattering emission of the corona on the imaging geometry dictates that WISPR will be very sensitive to the emission from plasma close to the spacecraft in contrast to the situation for imaging from Earth orbit. WISPR will be the first ‘local’ imager providing a crucial link between the large-scale corona and the in-situ measurements.

Published
2015

3. The solar and heliospheric imager (SoloHI) instrument for the solar orbiter mission

Author

Simon Plunkett, M. T. Carter, Dennis G. Socker, James Robert Janesick, Pierre Rochus, D. H. Chua, Clarence M. Korendyke, E. M. DeJong, N. Rich, John Robertson Tower, Adam Thurn, David Keller, Volker Bothmer, D. R. McMullin, Marco Velli, Russell A. Howard, Greg Clifford, Mark G. Linton, Jean-Philippe Halain, William Bast, Arnaud Thernisien, P. C. Liewer, Angelos Vourlidas, Mark Grygon, Philippe Lamy, R. Hagood, Dennis Wang, Zoran Mikic, and Sean Lynch

Subjects
Physics, Solar conjunction, 010504 meteorology & atmospheric sciences, Comet tail, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Solar irradiance, 7. Clean energy, 01 natural sciences, Corona, law.invention, Solar wind, Orbiter, law, Physics::Space Physics, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Heliosphere, 0105 earth and related environmental sciences
Abstract

The SoloHI instrument for the ESA/NASA Solar Orbiter mission will track density fluctuations in the inner heliosphere, by observing visible sunlight scattered by electrons in the solar wind. Fluctuations are associated with dynamic events such as coronal mass ejections, but also with the “quiescent” solar wind. SoloHI will provide the crucial link between the low corona observations from the Solar Orbiter instruments and the in-situ measurements on Solar Orbiter and the Solar Probe Plus missions. The instrument is a visible-light telescope, based on the SECCHI/Heliospheric Imager (HI) currently flying on the STEREO mission. In this concept, a series of baffles reduce the scattered light from the solar disk and reflections from the spacecraft to levels below the scene brightness, typically by a factor of 10 12 . The fluctuations are imposed against a much brighter signal produced by light scattered by dust particles (the zodiacal light/F-corona). Multiple images are obtained over a period of several minutes and are summed on-board to increase the signal-to-noise ratio and to reduce the telemetry load. SoloHI is a single telescope with a 40⁰ field of view beginning at 5⁰ from the Sun center. Through a series of Venus gravity assists, the minimum perihelia for Solar Orbiter will be reduced to about 60 Rsun (0.28 AU), and the inclination of the orbital plane will be increased to a maximum of 35⁰ after the 7 year mission. The CMOS/APS detector is a mosaic of four 2048 x 1920 pixel arrays, each 2-side buttable with 11 µm pixels.

Published
2013

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