SPICE EUV spectrometer for the Solar Orbiter mission

Fludra, A.; Griffin, Douglas; Caldwell, M.; Eccleston, Paul; Cornaby, James; Drummond, D.; Grainger, W.; Greenway, Paul; Grundy, Timothy; Howe, C.; McQuirk, C.; Middleton, Kevin; Poyntz-Wright, O.; Richards, A. G.; Rogers, Kevin; Sawyer, C.; Shaughnessy, Bryan; Sidher, S.; Tosh, Ian; Beardsley, S.; Burton, G.; Marshall, A.; Waltham, Nicholas R.; Woodward, S.; Appourchaux, T.; Philippon, Anne; Auchère, F.; Buchlin, É.; Gabriel, A. H.; Vial, J. C.; Schühle, U.; Curdt, W.; Innes, D. E.; Meining, Stefan; Peter, Hardi; Solanki, S. K.; Teriaca, L.; Gyo, Manfred; Büchel, V.; Haberreiter, M.; Pfiffner, Daniel; Schmutz, W.; Carlsson, Mats; Haugan, S. V. H.; Davila, J. M.; Jordan, Patrick R.; Thompson, W. T.; Hassler, D. M.; Walls, B.; DeForest, C. E.; Hanley, J.; Johnson, J. R.; Phelan, Patrick T.; Blecha, Laura; Cottard, H.; Paciotti, G.; Autissier, Nordahl; Allemand, Y.; Relecom, K.; Munro, G.; Butler, Alison; Klein, R.; Gottwald, Alexander

doi:10.1117/12.2027581

Cited by 20 publications

(9 citation statements)

References 2 publications

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“…The next solar UV spectroscopic capability for solar physics is the SPICE instrument (Fludra et al 2013) that will be flown on Solar Orbiter. This will observe two wavelength bands at 704-790 and 973-1049 Å, which give excellent coverage from the chromosphere through the transition region to the corona, and thus will allow the UV burst heating to be tracked through the layers of the atmosphere.…”

Section: Discussionmentioning

confidence: 99%

Solar Ultraviolet Bursts

et al. 2018

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The term "ultraviolet (UV) burst" is introduced to describe small, intense, transient brightenings in ultraviolet images of solar active regions. We inventorize their properties and provide a definition based on image sequences in transition-region lines. Coronal signatures are rare, and most bursts are associated with small-scale, canceling oppositepolarity fields in the photosphere that occur in emerging flux regions, moving magnetic features in sunspot moats, and sunspot light bridges. We also compare UV bursts with similar transition-region phenomena found previously in solar ultraviolet spectrometry and with similar phenomena at optical wavelengths, in particular Ellerman bombs. Akin to the lat-Electronic supplementary material The online version of this article (https://doi.

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Section: Discussionmentioning

confidence: 99%

Solar Ultraviolet Bursts

et al. 2018

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“…The Solar Orbiter satellite will accommodate the Spectral Investigation of the Coronal Environment (SPICE) instrument (Fludra et al 2013). SPICE covers two EUV wavelength bands, one of which will include the Ly-β line.…”

Section: Simulation Of Spice Profilesmentioning

confidence: 99%

Modeling of the Hydrogen Lyman Lines in Solar Flares

Brown

Fletcher

Kerr

et al. 2018

ApJ

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The hydrogen Lyman lines (91.2 nm < λ<121.6 nm) are significant contributors to the radiative losses of the solar chromosphere, and they are enhanced during flares. We have shown previously that the Lyman lines observed by the Extreme Ultraviolet Variability instrument onboard the Solar Dynamics Observatory exhibit Doppler motions equivalent to speeds on the order of 30 km s −1 . However, contrary to expectations, both redshifts and blueshifts were present and no dominant flow direction was observed. To understand the formation of the Lyman lines, particularly their Doppler motions, we have used the radiative hydrodynamic code, RADYN, along with the radiative transfer code, RH, to simulate the evolution of the flaring chromosphere and the response of the Lyman lines during solar flares. We find that upflows in the simulated atmospheres lead to blueshifts in the line cores, which exhibit central reversals. We then model the effects of the instrument on the profiles, using the Extreme Ultraviolet Variability Experiment (EVE) instrumentʼs properties. What may be interpreted as downflows (redshifted emission) in the lines, after they have been convolved with the instrumental line profile, may not necessarily correspond to actual downflows. Dynamic features in the atmosphere can introduce complex features in the line profiles that will not be detected by instruments with the spectral resolution of EVE, but which leave more of a signature at the resolution of the Spectral Investigation of the Coronal Environment instrument onboard the Solar Orbiter.

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“…The Spectral Investigation of the Coronal Environment (SPICE, Fludra et al, 2013) on board the Solar Orbiter operates at extreme ultraviolet wavelength in two bands, 704-790Å and 973-1049Å, which are dominated by emission lines from a wide range of ions of H, C, O, N, Ne, S, Mg, Si and Fe. These lines are formed at temperatures from 10 4 to 10 7 K, allowing the study of the solar atmosphere from the chromosphere in the Lyman-β line up to the flaring corona (e.g.…”

Section: Solar Orbitermentioning

confidence: 99%

Nonequilibrium Processes in the Solar Corona, Transition Region, Flares, and Solar Wind (Invited Review)

et al. 2017

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We review the presence and signatures of the non-equilibrium processes, both non-Maxwellian distributions and non-equilibrium ionization, in the solar transition region, corona, solar wind, and flares. Basic properties of the non-Maxwellian distributions are described together with their influence on the heat flux as well as on the rates of individual collisional processes and the resulting optically thin synthetic spectra. Constraints on the presence of highenergy electrons from observations are reviewed, including positive detection of non-Maxwellian distributions in the solar corona, transition region, flares, and wind. Occurrence of non-equilibrium ionization is reviewed as well, especially in connection to hydrodynamic and generalized collisional-radiative modelling. Predicted spectroscopic signatures of non-equilibrium ionization depending on the assumed plasma conditions are summarized. Finally, we discuss the future remote-sensing instrumentation that can be used for detection of these non-equilibrium phenomena in various spectral ranges.

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SPICE EUV spectrometer for the Solar Orbiter mission

Cited by 20 publications

References 2 publications

Solar Ultraviolet Bursts

Solar Ultraviolet Bursts

Modeling of the Hydrogen Lyman Lines in Solar Flares

Nonequilibrium Processes in the Solar Corona, Transition Region, Flares, and Solar Wind (Invited Review)

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