Abstract
Abstract Hinode is Japan’s third solar mission following Hinotori (1981–1982) and Yohkoh (1991–2001): it was launched on 2006 September 22 and is in operation currently. Hinode carries three instruments: the Solar Optical Telescope, the X-Ray Telescope, and the EUV Imaging Spectrometer. These instruments were built under international collaboration with the National Aeronautics and Space Administration and the UK Science and Technology Facilities Council, and its operation has been contributed to by the European Space Agency and the Norwegian Space Center. After describing the satellite operations and giving a performance evaluation of the three instruments, reviews are presented on major scientific discoveries by Hinode in the first eleven years (one solar cycle long) of its operation. This review article concludes with future prospects for solar physics research based on the achievements of Hinode.
Highlights
The Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), successfully launched the M-V Launch Vehicle No 7 (M-V-7) with SOLAR-B aboard at 6:36 am on 2006 September 23 JST (21:36 UTC on September 22) from the Uchinoura Space Center (USC): the spacecraft was nicknamed “Hinode,” meaning “sunrise” in Japanese.This is the third Japanese solar physics mission following Hinotori (ASTRO-A; Kondo 1982) and Yohkoh (SOLARA; Ogawara et al 1991)
Sheared coronal loops followed by ejection of plasma clouds and sudden coronal dimming during solar flares (Sterling et al 2000), X-ray jets (Shimojo et al 1996), and tiny microflares in active regions (Shimizu 1995) have all been recognized as manifestations of magnetic reconnection, and dynamical evolutions of these phenomena were observed for the first time by the Soft X-ray Telescope (SXT) experiment on Yohkoh (Tsuneta et al 1991), which registered more than one million whole-Sun X-ray images, and they were combined into 3 × 105 composite images in order to increase the dynamic range of each image by carefully calibrating the on-orbit performance of the spacecraft (Acton 2016)
With an increase in the default telemetry allocation for X-Ray Telescope (XRT) (23% as compared to the previous value of 15%) after the middle of 2016, XRT is capable of taking X-ray images of the corona with higher exposure cadence and/or with larger field of view (FOV) than before
Summary
Sheared coronal loops followed by ejection of plasma clouds and sudden coronal dimming during solar flares (Sterling et al 2000), X-ray jets (Shimojo et al 1996), and tiny microflares in active regions (Shimizu 1995) have all been recognized as manifestations of magnetic reconnection, and dynamical evolutions of these phenomena were observed for the first time by the Soft X-ray Telescope (SXT) experiment on Yohkoh (Tsuneta et al 1991), which registered more than one million whole-Sun X-ray images, and Based on these discoveries of its predecessors, the Hinode mission (Kosugi et al 2007) was designed to address the fundamental question of how magnetic fields interact with the ionized atmosphere to produce solar variability. The Appendix contains a list of abbreviations used in this article for instrument names and so on
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