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

Howard, R. A.; Vourlidas, A.; Korendyke, C. M.; Plunkett, S. P.; Carter, Michael T.; Wang, Dennis; Rich, N.; McMullin, D.; Lynch, S.; Thurn, Adam; Clifford, Greg; Socker, D. G.; Thernisien, A.; Chua, D.; Linton, M. G.; Keller, David; Janesick, James R.; Tower, John R.; Grygon, Mark; Hagood, R.; Bast, William D.; Liewer, Paulett C.; DeJong, E.; Velli, Marco; Mikić, Z.; Bothmer, V.; Rochus, Pierre; Halain, Jean-Philippe; Lamy, Philippe

doi:10.1117/12.2027657

Cited by 19 publications

(12 citation statements)

References 8 publications

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“…The method holds promise for improving the extraction of quantitative information from shocks in the corona using remote sensing observations. It can readily use observations from different vantage points, including from the imagers (Howard et al, 2013;Vourlidas et al, 2016) aboard the upcoming Solar Orbiter (Müeller et al, 2013) and Solar Probe Plus (Fox et al, 2016) missions to be compared with direct in situ measurements from these missions. The technique will also greatly improve the results from any future joint coronagraphic imaging and off-limb spectroscopy of shocks (Bemporad and Mancuso, 2011;Vourlidas and Bemporad, 2012).…”

Section: Discussionmentioning

confidence: 99%

The density compression ratio of shock fronts associated with coronal mass ejections

Kwon

Vourlidas

2018

J. Space Weather Space Clim.

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-We present a new method to extract the three-dimensional electron density profile and density compression ratio of shock fronts associated with coronal mass ejections (CMEs) observed in white light coronagraph images. We demonstrate the method with two examples of fast halo CMEs (∼2000 km s À1 ) observed on 2011 March 7 and 2014 February 25. Our method uses the ellipsoid model to derive the threedimensional geometry and kinematics of the fronts. The density profiles of the sheaths are modeled with double-Gaussian functions with four free parameters, and the electrons are distributed within thin shells behind the front. The modeled densities are integrated along the lines of sight to be compared with the observed brightness in COR2-A, and a x 2 approach is used to obtain the optimal parameters for the Gaussian profiles. The upstream densities are obtained from both the inversion of the brightness in a pre-event image and an empirical model. Then the density ratio and Alfvénic Mach number are derived. We find that the density compression peaks around the CME nose, and decreases at larger position angles. The behavior is consistent with a driven shock at the nose and a freely propagating shock wave at the CME flanks. Interestingly, we find that the supercritical region extends over a large area of the shock and lasts longer (several tens of minutes) than past reports. It follows that CME shocks are capable of accelerating energetic particles in the corona over extended spatial and temporal scales and are likely responsible for the wide longitudinal distribution of these particles in the inner heliosphere. Our results also demonstrate the power of multi-viewpoint coronagraphic observations and forward modeling in remotely deriving key shock properties in an otherwise inaccessible regime.

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Section: Discussionmentioning

confidence: 99%

The density compression ratio of shock fronts associated with coronal mass ejections

Kwon

Vourlidas

2018

J. Space Weather Space Clim.

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“…The sophisticated baffle design allows WISPR to meet this requirement and allows for high signal-to-noise ratio (SNR) imaging ranging from SNR = 20 at the inner FOV at closest perihelion to SNR = 5 at the largest distance and FOV angles. The detectors are 2048 × 1920 format APS CMOS devices developed for the SoloHI program (Howard et al 2013). APS devices are much less susceptible to radiation damage than the more common CCD devices and are therefore the best option for this mission.…”

Section: System Descriptionmentioning

confidence: 99%

“…The WISPR design draws its heritage from the SECCHI heliospheric imagers aboard the Solar Terrestrial Earth Relations Observatory (STEREO; Kaiser et al 2008) mission and from the SoloHI imager (Howard et al 2013) under development for ESA's Solar Orbiter mission scheduled for launch in 2017 (Müller et al 2013). In fact, SoloHI provides many of the design elements and subsystems for adaptation into the WISPR design.…”

Section: Design Philosophymentioning

confidence: 99%

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

et al. 2015

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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.

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“…WISPR is being developed with significant heritage from the SECCHI heliospheric imagers aboard the STEREO mission and from the SoloHI imager under development for ESA's Solar Orbiter mission [2] scheduled for launch in 2017. In fact, SoloHI, described elsewhere in this volume [3] , provides many of the design elements and subsystems for adaptation into the WISPR design.…”

Section: The Solar Probe Plus (Spp) Missionmentioning

confidence: 99%

“…The sophisticated baffle design allows WISPR to meet this requirement and allows for high signal-to-noise (SNR) imaging ranging from 20 at the inner FOV at closest perihelion to 5 at the largest distance and FOV angles. The detectors are 2048x1920 format Active Pixel Sensor (APS) CMOS devices developed for the SoloHI program [3,4] . APS devices are much less susceptible to radiation damage than the more common CCD devices and are therefore the best option for this mission.…”

Section: Wispr Instrument Designmentioning

confidence: 99%

Seeing the corona with the solar probe plus mission: the wide-field imager for solar probe+ (WISPR)

Vourlidas

Howard

Plunkett

et al. 2013

Solar Physics and Space Weather Instrumentation V

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The Solar Probe Plus (SPP) mission scheduled for launch in 2018, will orbit between the Sun and Venus with diminishing perihelia reaching as close as 7 million km (9.86 solar radii) from Sun center. In addition to a suite of in-situ probes for the magnetic field, plasma, and energetic particles, SPP will be equipped with an imager. The Wide-field Imager for the Solar PRobe+ (WISPR), with a 95º radial by 58º transverse field of view, will image the fine-scale coronal structure of the corona, derive the 3D structure of the large-scale corona, and determine whether a dust-free zone exists near the Sun. Given the tight mass constrains of the mission, WISPR incorporates an efficient design of two widefield telescopes and their associated focal plane arrays based on novel large-format (2kx2k) APS CMOS detectors into the smallest heliospheric imaging package to date. The flexible control electronics allow WISPR to collect individual images at cadences up to 1 second at perihelion or sum several of them to increase the signal-to-noise during the outbound part of the orbit. The use of two telescopes minimizes the risk of dust damage which may be considerable close to 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.

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

Cited by 19 publications

References 8 publications

The density compression ratio of shock fronts associated with coronal mass ejections

The density compression ratio of shock fronts associated with coronal mass ejections

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

Seeing the corona with the solar probe plus mission: the wide-field imager for solar probe+ (WISPR)

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