Recent solar physics missions have shown the definite role of waves and magnetic fields deep in the inner corona, at the chromosphere-corona interface, where dramatic and physically dominant changes occur. HiRISE (High Resolution Imaging and Spectroscopy Explorer), the ambitious new generation ultra-high resolution, interferometric, and coronagraphic, solar physics mission, proposed in response to the ESA Voyage 2050 Call, would address these issues and provide the best-ever and most complete solar observatory, capable of ultra-high spatial, spectral, and temporal resolution observations of the solar atmosphere, from the photosphere to the corona, and of new insights of the solar interior from the core to the photosphere. HiRISE, at the L1 Lagrangian point, would provide meter class FUV imaging and spectro-imaging, EUV and XUV imaging and spectroscopy, magnetic fields measurements, and ambitious and comprehensive coronagraphy by a remote external occulter (two satellites formation flying 375 m apart, with a coronagraph on a chaser satellite). This major and state-of-the-art payload would allow us to characterize temperatures, densities, and velocities in the solar upper chromosphere, transition zone, and inner corona with, in particular, 2D very high resolution multi-spectral imaging-spectroscopy, and, direct coronal magnetic field measurement, thus providing a unique set of tools to understand the structure and onset of coronal heating. HiRISE’s objectives are natural complements to the Parker Solar Probe and Solar Orbiter-type missions. We present the science case for HiRISE which will address: i) the fine structure of the chromosphere-corona interface by 2D spectroscopy in FUV at very high resolution; ii) coronal heating roots in the inner corona by ambitious externally-occulted coronagraphy; iii) resolved and global helioseismology thanks to continuity and stability of observing at the L1 Lagrange point; and iv) solar variability and space climate with, in addition, a global comprehensive view of UV variability.
|Early online date||05 Mar 2022|
|Publication status||Published - Dec 2022|
Bibliographical noteFunding Information:
The authors would like to thank the anonymous referee for the very careful reading of the paper and for suggesting structural changes for a more fluent read. Sources of funding acknowledged are: R.E. acknowledges the support received from the Science and Technology Facilities Council (STFC) UK (grant number ST/M000826/1 at the University of Sheffield). L.D. is grateful to the Centre National d’Etudes Spatiales (CNES) for R&T support received to develop SOLARNET interferometric breadboard and new generation of FUV robust solar telescopes (SUAVE). M.B.K and HM are grateful to the Science and Technology Facilities Council (STFC), (UK, Aberystwyth University, grant number ST/S000518/1). F.Z. acknowledges the support received by the Universitá degli Studi di Catania (Piano per la Ricerca Universitá di Catania 2016-2018 - Linea di intervento 2) and by the Italian MIUR-PRIN grant 2017APKP7T on Circumterrestrial Environment: Impact of Sun-Earth Interaction.
© 2022, The Author(s).
- Solar atmosphere
- Solar physics mission
- Ultra-high resolution
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science