Observations in situ suggest that intermediate FIP elements such as S (the high FIP element with the lowest FIP) behave differently on open and closed magnetic field lines ( 13), making abundance ratios such as Si/S potentially more useful diagnostics than others such as Fe/O. In particular, the SEP/solar wind–to–photospheric abundance ratio pattern as a function of FIP is different, and the magnitude of the enhancement for some element ratios is also different ( 13). ![]() In situ measurements of SEP and solar wind abundances suggest otherwise. The missions of the Heliophysics System Observatory are essential tools to understand the whole Sun-Earth coupled system.Ī key question is whether the coronal material that seeds the SEP population during large, gradual events-those with high ion fluxes and the greatest impact on near-Earth space infrastructure-originates from the same source locations as the solar wind and is simply shock-accelerated later by CMEs. Field reversals that we see close-in where the probes operate are different than what we see at Earth ( 4). For an operational space weather predictive capability, we still need to understand what happens in the near-Earth environment. The discovery of magnetic field reversals, dubbed “switchbacks” ( 3), raises questions about the extent to which we can connect activity seen at Earth with dynamics in the source regions on the Sun. Already the new measurements from PSP are fundamentally altering long-held views. The recently launched Parker Solar Probe (PSP) ( 1) and Solar Orbiter ( 2) missions will investigate the Sun from a closer vantage point than ever before, allowing further insights into these basic processes. From a space weather perspective, we must elucidate the mechanisms that drive solar flares, coronal mass ejections (CMEs), and solar energetic particles (SEPs). We need to understand and characterize the processes that form and heat the solar atmosphere and accelerate the solar wind into the heliosphere. One of the central goals of heliophysics is to understand the origins of solar activity and predict its impact on the terrestrial space environment. This source material is continually released from magnetic confinement and accelerated as SEPs following M-, C-, and X-class flares. The plasma confined closest to that region, where the coronal magnetic field strength is high (a few hundred Gauss), develops the SEP composition signature. Our results localize the elemental fractionation process to the top of the chromosphere. We show that the elemental composition signature detected spectroscopically at the footpoints explains the measurements made by particle counting techniques near Earth. ![]() Here, we use multi-messenger observations from the Heliophysics System Observatory to identify plasma confined at the footpoints of the hot, core loops of active region 11944 as the source of major gradual SEP events in January 2014. Glasgow) Public outreach web application on the science of sunspots (US PBS NOVA TV show) Institut d Astrophysique Spatiale, Paris: SDO data browse tool uses Helioviewer API to deliver images ( client-user/ias_sdo_data/project-index.Shock waves associated with fast coronal mass ejections (CMEs) accelerate solar energetic particles (SEPs) in the long duration, gradual events that pose hazards to crewed spaceflight and near-Earth technological assets, but the source of the CME shock-accelerated plasma is still debated. Use Cases Catalog of AIA images and movies based on RHESSI flare list (in development, Iain Hannah, U. 16 What is JPEG 2000? JPEG 2000 = wavelet-based compression standard Advantages: Multi-resolution Images at different resolutions are automatically created during wavelet compression Random image access Selected parts + quality layers can be accessed remotely Flexible file format Well-suited for archivesġ7 Remote Image Access via JPIP JPIP = JPEG 2000 Interactive Protocol Provides a client server architecture for interactively transmitting image data over networks Can request arbitrary parts and quality levels of image series JHELIOVIEWER Browser JPIP Client JHELIOVIEWER Server JPIP Server METADATA HANDLER JPIP data stream and headers image request JPEG 2000 PARSER/ REFORMATTER JPEG 2000 IMAGE REPOSITORY SOLAR EVENT MANAGER CLIENT CACHE MODEL USER INTERFACE LAYER MANAGER target image IMAGE RENDERER/ DECODER data search query EVENT Server METADATA CATALOG LOCAL CACHE event catalog search query event data EVENT CATALOG WEB SERVICE EVENT CATALOG REPOSITORY Müller et al., Computing in Science & Engineering (2009)Ĥ0 Helioviewer API In order to facilitate third-party application developers who wish to use content from and interact with, a number of Application Programming Interfaces (APIs) have been developed, offering access to a variety of components used by Helioviewer.
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