Since 2017 the Solar Ultraviolet Imager (SUVI: Darnel et al., 2022), on the several Geostationary Operational Environmental Satellite (GOES-R) spacecraft, has been observing through six passbands, with peak wavelengths at 9. Researchers provide new clue to solar coronal heating problem. The Sun Watcher with Active Pixels and Image Processing instrument (SWAP: Seaton et al., 2013b Halain et al., 2013) is a large field-of-view (FOV) extreme-ultraviolet (EUV) observing telescope onboard the European Space Agency’s (ESA) Project for Onboard Autonomy 2 (PROBA2) spacecraft (Santandrea et al., 2013), observing a FOV of \(\approx 1.7\times 1.7\) solar radii (as measured from the disk center \(\mathrm\)), passbands with peak wavelengths at 9.4, 13.1, 17.1, 19.3, 21.1, 30.4, and 33.5 nm. The solar corona evolves on a variety of timescales closely connected with the evolution of the coronal magnetic field. We also highlight SWAP’s imaging capabilities, techniques that have been applied to observations to enhance the off-limb observations and its legacy. The review is broadly divided into three main sections of SWAP-based studies about: i) long-lived phenomena, such as streamers, pseudo-streamers, and coronal fans ii) dynamic phenomena, such as eruptions, jets, EUV waves, and shocks iii) coronal EUV emission generation. 'The problem of coronal heating was first discovered in the. The solar surface is blocked out in this view. The chief problem standing in the way of an answer. The Suns surface is considerably too brilliant to see the corona, which is much fainter. The extreme heat of the Sun’s corona is one of the most vexing problems in astrophysics. mage of the suns corona, taken by NASAs STEREO Ahead spacecraft on June 8, 2010. In this article, we present a review of all publications that have utilized these observations to explore the extended EUV corona, highlighting the unique contributions made by SWAP. One of the interesting problems in space research is explaining why the sun's atmosphere (its corona) is so much hotter than its surface. It has helped shape our understanding of this previously understudied region, and pioneered research into the middle corona. (2009) The mystery of why temperatures in the solar corona, the suns outer atmosphere, soar to several million degrees Kelvin (K) much hotter than temperatures nearer the suns surfacehas puzzled scientists for decades. The Sun Watcher with Active Pixels and Image Processing (SWAP) instrument onboard ESA’s PRoject for On Board Autonomy 2 (PROBA2) has provided the first uncompressed, high-cadence, continuous, large field-of-view observations of the extended extreme-ultraviolet (EUV) corona for over a complete solar cycle. Blue regions indicate plasma near 10 million degrees K.
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |