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\t\t\t\t\t\t26\/11\/2024<\/span> Hidden in plain sight within the Sun\u2019s glare is the ultra-hot yet ghostly faint solar corona, source of the solar wind and solar storms. The only way to see this key element of the Solar System is either through the remarkable cosmic coincidence that gives rise to total solar eclipses \u2013 the fact that the Sun is not only 400 times bigger than our Moon but also about 400 times further away, allowing it to cover the solar disc entirely \u2013 or else through artificial Sun-obscuring telescopes.\u00a0<\/p>\n<\/div>\n The biggest and most ambitious of these \u2018coronagraphs\u2019 is about to become reality: ESA’s Proba-3 mission involves two spacecraft forming one giant virtual instrument, with one spacecraft covering the Sun for the other. But how does it work in practice?<\/p>\n<\/p><\/div>\n The crown of light that surrounds the eclipsed Sun has been studied for centuries, but astronomers thought the corona might actually originate from the Moon or Earth\u2019s atmosphere. Finally, it was ascertained that the corona was in fact the solar atmosphere, normally remaining unseen except during eclipses because it is a million times fainter than the fiery face of the Sun.<\/p>\n In 1931 French astronomer Bernard Lyot \u2013 based high in the Pyrenees to observe above the bulk of Earth\u2019s atmosphere \u2013 completed the first \u2018coronagraph\u2019: a telescope incorporating a disc to occult the Sun, allowing sustained study of the corona.<\/p>\n<\/p><\/div>\n Driving back waves of light\u00a0 <\/b><\/p>\n \u201cThis might sound simple, but it\u2019s rendered much harder by the peculiar fact that light acts as both particles and waves,\u201d explains Damien Galano, ESA\u2019s Proba-3 mission manager. \u201cThis means some light spills around the edge of whatever\u2019s blocking it, like waves around a seawall. This phenomenon is known as \u2018diffraction\u2019; it needs to be designed against to minimise unwanted sunlight reaching your instrument.\u201d<\/p>\n The best way around diffraction is to move an occulting disc further from its telescope. \u201cThis is why total solar eclipses give us such an excellent view of the corona, because the Moon is around 384 000 km away from Earth, so diffraction effects are minimal,\u201d explains Andrei Zhukov, Principal Investigator of Proba-3\u2019s main instrument, Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun, ASPIICS.<\/p>\n<\/p><\/div>\n \u00a0Enter formation flying<\/b><\/p>\n \u201cAstronomers can\u2019t outdo natural eclipses, but \u2018external coronagraphs\u2019 in both Earth and space do place the occulter as far from the telescope as possible. In space our practical options have been limited however; for instance, the LASCO-C2 coronagraph aboard the ESA-NASA SOHO solar observatory has its occulter just 70 cm away, within the spacecraft body.\u201d<\/p>\n So what about flying the occulter on a separate spacecraft altogether, as far away as possible? Researcher Philippe Lamy led the Laboratoire d’Astrophysique de Marseille team which first devised the ASPIICS concept: \u201cBy moving them much further apart we\u2019d be able to see much closer to the edge of the solar disc, so formation flying seemed a natural fit. It wasn\u2019t an entirely new idea, because the US and Soviet Union had attempted it during the 1975 Apollo-Soyuz mission, when a cylindrical Apollo spacecraft blocked out the Sun for the watching Soyuz spacecraft \u2013 but the bright glare produced by propellant thrusting from the spacecraft spoiled the view.\u201d<\/p>\n<\/p><\/div>\n ASPIICS was first designed by the Laboratoire d’Astrophysique de Marseille team about two decades ago, following a formation flying call for ideas from French space agency CNES, then found a home within ESA\u2019s technology-demonstrating Proba satellite series.<\/p>\n Rapid rate of observations<\/b><\/p>\n \u201cToday we have two ways of observing the corona from space,\u201d notes Andrei Zhukov. \u201cExtreme ultraviolet imagers aboard space missions such as NASA\u2019s SDO and ESA\u2019s Proba-2 observe Sun in a small field of view around it whereas externally-occulted coronagraphs observing in white light show the outer part of the corona only. That leaves a gap in observation that Proba-3 will fill, for six hours at a time.\u201d<\/p>\n<\/p><\/div>\n In addition, Proba-3 will observe at a much more rapid rate than previous space-based coronagraphs. SOHO\u2019s LASCO-C2 usually updates its view only once every 12 minutes, while Proba-3 will have a 1-minute standard cadence, upgradable to a maximum 30 seconds, to yield fine details of the evolution of the massive explosions called Coronal Mass Ejections. \u201cWhen I first heard about it, Proba-3 seemed like science fiction technology,\u201d adds Andrei Zhukov. \u201cBut the real-life design will truly deliver excellent science.\u201d<\/p>\n \u201cThere was a lot of discussions on the design,\u201d recalls mission scientist Joe Zender. \u201cIt became a compromise between what in theory the technology can provide and what we can practically achieve in space.\u201d Early trade-off calculations came up with a 150-m operating distance for the Coronagraph and Occulter spacecraft \u2013 attempting to balance optical performance with workable tracking efficiency and propellant budgets \u2013 and the need to fix their relative positions to just a few millimetres of precision.<\/p>\n<\/p><\/div>\n Double disc design<\/b><\/p>\n Practical experimentation also played a role, including an ESA StarTiger R&D programme performed in 2009 by a team of European engineers that worked altogether at Laboratoire d’Astrophysique de Marseille for six months.<\/p>\n StarTiger concentrated on developing and testing the most critical subsystems of the instrument, including the \u201cShadow Position Sensors\u201d and \u201cOcculter Position Sensors\u201d providing absolute references for the alignment and pointing of the two spacecraft, and the occulting disc. The project also yielded valuable findings on the best ways to engineer the edge of the occulting disc to minimise spillover light.<\/p>\n<\/p><\/div>\n This 1.4 m diameter occulting disc to be flown on the Occulter spacecraft provided a crucial design element. It was produced by Airbus in Spain in carbon fibre reinforced plastic \u2013 a composite material whose strength and rigidity sees it employed for everything from wind turbine blades to Formula 1 cars and spacecraft hulls \u2013 based on a mould from Euro-Composites in Luxembourg.<\/p>\n \u201cAnd in fact Proba-3 has a second much smaller but equally important and precisely manufactured occulting disc, placed within its central lens, just 3.5mm in diameter,\u201d adds Damien Galano. \u201cThe 19th<\/sup> century experiments that established light as a wave showed that straylight spilling over a disc would constructively interfere in such a way that it is concentrated at the centre of the resulting shadow. This disc blocks much of those spillover wavelets; once that was ready we could really start testing out the rest of ASPIICS too.\u201d<\/p>\n<\/p><\/div>\n 150-m long virtual instrument<\/b><\/p>\n As a result, while the alignment of lenses and occulters in a standard externally occulter coronagraph results in a coronal field of view that starts at around 2.5 times the extent of the Sun\u2019s disc, for Proba-3 that figure is just 1.1 solar radii.<\/p>\n The flight model of the instrument built by Centre Spatial de Li\u00e8ge, CSL, is being hosted on Proba-3\u2019s Coronagraph spacecraft, although the Occulter spacecraft forms an integral part of the instrument too \u2013 effectively the pair form a virtual 150-m long instrument.<\/p>\n<\/p><\/div>\n Joe Zender comments: \u201cSuccess will rely on the formation flying technology working as planned, of course, but the closer we get to launch, the more I realise the excitement of what we are doing, including co-observations with many other solar observing missions.\u201d<\/p>\n Andrei Zhukov adds: \u201cAfter our approximately four-month commissioning stage the plan is to have two six-hour observing periods per week, determined by the mission\u2019s need to conserve propellant. Instead of glimpsing the inner corona for just a few minutes during occasional terrestrial solar eclipses we\u2019ll be keeping watch over sets of six-hour eclipses on demand, with a really good view of all the processes taking place, notably the eruption of CMEs and the acceleration of the solar wind.\u201d<\/p>\n<\/p><\/div>\n
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