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36 results for “solar images”
Active Region Magnetograms for Solar Flare Prediction: Extra Dataset Images for ARs 1981 through 2469
<p>This dataset is the extra images associated with Dryad dataset <a href="https://doi.org/10.5061/dryad.qjq2bvqmj">https://doi.org/10.5061/dryad.qjq2bvqmj</a>. These images are consistently sized images of active region magnetograms from the National Aeronautics and Space Administration's (NASA's) Solar Dynamics Observatory (SDO). These data are the full sized images (600x600 pixels) for active regions (ARs) 1981 through 2469 in .fits format. These are images that were removed from the preconfigured dataset https://doi.org/10.5061/dryad.jq2bvq898.</p>
Active Region Magnetograms for Solar Flare Prediction: Extra Dataset Images for ARs 1528 through 1980
<p>This dataset is the extra images associated with Dryad dataset <a href="https://doi.org/10.5061/dryad.qjq2bvqmj">https://doi.org/10.5061/dryad.qjq2bvqmj</a>. These images are consistently sized images of active region magnetograms from the National Aeronautics and Space Administration's (NASA's) Solar Dynamics Observatory (SDO). These data are the full sized images (600x600 pixels) for active regions (ARs) 1528 through 1980 in .fits format. These are images that were removed from the preconfigured dataset https://doi.org/10.5061/dryad.jq2bvq898.</p>
Active region magnetograms for solar flare prediction: Extra images dataset
<p>In this dataset, we provide a comprehensive collection of magnetograms from the National Aeronautics and Space Administration's (NASA's) Solar Dynamics Observatory (SDO). The dataset incorporates data from three sources and provides SDO Helioseismic and Magnetic Imager (HMI) magnetograms of solar active regions as well as labels of corresponding flaring activity. This dataset will be useful for image analysis or solar physics research related to magnetic structure, its evolution over time, and its relation to solar flares. The dataset will be of interest to those researchers investigating automated solar flare prediction methods, including supervised and unsupervised machine learning (classical and deep), binary and multi-class classification, and regression. This dataset contains those images that were removed from the preconfigured datasets (see usage notes below).</p>
Active region magnetograms for solar flare prediction: Extra images dataset
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Girasol, a sky imaging and global solar irradiance dataset
<p>The energy available in Micro Grid (MG) that is powered by solar energy is tightly related to the weather conditions in the moment of generation. Very short-term forecast of solar irradiance provides the MG with the capability of automatically controlling the dispatch of energy. We propose to achieve this using a data acquisition systems (DAQ) that simultaneously records sky imaging and Global Solar Irradiance (GSI) measurements, with the objective of extracting features from clouds and use them to forecast the power produced by a Photovoltaic (PV) system. The DAQ system is nicknamed as the <em>Girasol Machine</em> (Girasol means Sunflower in Spanish). The sky imaging system consists of a longwave infrared (IR) camera and a visible (VI) light camera with a fisheye lens attached to it. The cameras are installed inside a weatherproof enclosure that it is mounted on an outdoor tracker. The tracker updates its pan an tilt every second using a solar position algorithm to maintain the Sun in the center of the IR and VI images. A pyranometer is situated on a horizontal support next to the DAQ system to measure GSI. The dataset, composed of IR images, VI images, GSI measurements, and the Sun's positions, has been tagged with timestamps.</p>
Quiet-time solar interferometric imaging data from Zhang et al. 2022
<p>Dataset from the paper "Imaging of the Quiet Sun in the Frequency Range of 20–80 MHz" by Peijin Zhang et al., 2022</p>
Data for the manuscript named 'Soft X-ray imaging of the magnetosheath and cusps under different solar wind conditions: MHD simulations'
<p> This is the data used by the manuscript named 'Soft X-ray imaging of the magnetosheath and cusps under different solar wind conditions: MHD simulations'.</p> <p> The uploaded data is the X-ray intensity data for all the five cases studied in the manuscritpt. 'Casen' (n=1, 2, 3, 4, and 5) in the name of each data file indicates the case number, and 'sat pointX' (X=A, B, C, D) show the satellite positions analyzed in the manuscript. </p> <p> The data can be read by IDL using the following program statments:</p> <p>openr,lun,datai,/get_lun<br> xgse=0. & ygse=0. & zgse=0.<br> readf,lun,xgse,ygse,zgse ;;;;(satellite position in the GSE coordinate)<br> xsat=0. & ysat=0. & zsat=0.<br> readf,lun,xsat,ysat,zsat ;;;;(satellite position in the GSM coordinate)<br> xpoint=0. & ypoint=0. & zpoint=0.<br> readf,lun,xpoint,ypoint,zpoint ;;;;(satellite pointing of SXI, aim point)<br> nthtmax=0L & nphimax=0L<br> readf,lun,nthtmax,nphimax ;;;;(number of the tht and phi grids)<br> thti=fltarr(nthtmax) & phii=fltarr(nphimax)<br> readf,lun,thti,format='(e14.6)' ;;;;(the tht grids)<br> readf,lun,phii,format='(e14.6)' ;;;;(the phi grids)<br> Pxraytp=fltarr(nthtmax,nphimax)<br> readf,lun,Pxraytp,format='(e14.6)' ;;;;(X-ray intensity)<br> close,lun<br> free_lun,lun</p>
Girasol, a sky imaging and global solar irradiance dataset
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SD4EO - Physically Based Rendering images of human settlements for solar panel detection
<p>This dataset contains part of the results of the SD4EO project, including images corresponding to the use case of solar panel detection on human settlements. The dataset contains images that have been simulated corresponding to low altitude aerial images. Each image in the dataset includes pixel-level labels for each element present in the image, ensuring perfect accuracy due to the synthetic nature of the images. This eliminates common errors in manual or semi-automatic labeling processes.</p> <p><strong>Image labeling</strong></p> <p><strong>(Open Street Map color code)</strong></p> <div> <table> <tbody> <tr> <td> <p><strong>Element</strong></p> </td> <td> <p><strong>R</strong></p> </td> <td> <p><strong>G</strong></p> </td> <td> <p><strong>B</strong></p> </td> </tr> <tr> <td> <p>Road</p> </td> <td> <p>255</p> </td> <td> <p>255</p> </td> <td> <p>255</p> </td> </tr> <tr> <td> <p>Building</p> </td> <td> <p>196</p> </td> <td> <p>182</p> </td> <td> <p>171</p> </td> </tr> <tr> <td> <p>Highway</p> </td> <td> <p>232</p> </td> <td> <p>146</p> </td> <td> <p>162</p> </td> </tr> <tr> <td> <p>Industrial zone</p> </td> <td> <p>234</p> </td> <td> <p>203</p> </td> <td> <p>228</p> </td> </tr> <tr> <td> <p>Parking</p> </td> <td> <p>238</p> </td> <td> <p>238</p> </td> <td> <p>238</p> </td> </tr> <tr> <td> <p>Railway</p> </td> <td> <p>112</p> </td> <td> <p>112</p> </td> <td> <p>112</p> </td> </tr> <tr> <td> <p>Residential zone</p> </td> <td> <p>224</p> </td> <td> <p>223</p> </td> <td> <p>223</p> </td> </tr> <tr> <td> <p>Vegetation</p> </td> <td> <p>174</p> </td> <td> <p>223</p> </td> <td> <p>163</p> </td> </tr> <tr> <td> <p>Water</p> </td> <td> <p>170</p> </td> <td> <p>211</p> </td> <td> <p>223</p> </td> </tr> </tbody> </table> </div> <p>For solar panels masks white color is used to mark the pixels corresponding to solar panels.</p> <p><br><strong>Image name convention</strong></p> <p>The name convention follows the next schema of fields, separated by the character “_”</p> <p>- ID number</p> <p>- Sub ID number</p> <p>- Meters per pixel resolution</p> <p>- Type of image: color, labels, solarpanels</p> <p><strong>Creation and funding</strong></p> <p>All the images have been generated using a tool developed in Unity. This tool will be soon available to enable the generation of new datasets.</p> <p>This research work has been funded by the European Space Agency (ESA) under the FutureEO program and the SD4EO project (Contract No.: 4000142334/23/I-DT), supervised by the ESA Φ-lab.</p> <p><strong>License and attribution</strong></p> <p>This dataset <span>is</span> licensed under a <a href="https://creativecommons.org/licenses/by/4.0/">Creative Commons Attribution 4.0 International License</a> (CC <span>BY</span> <span>4.0</span>).</p> <p><span>When using the images from this dataset, please attribute them as follows: "Synthetic images created by the research group ARTEC - IRTIC - University of Valencia".</span></p>
Resulting videos from the article: A Novel Technique for the Extraction of Dynamic Events in Extreme Ultraviolet Solar Images
<p>Videos called 'MFM PCP DMD ...' correspond to Figure 5 in the mentioned article. They show comparison of MFM, PCP, and DMD algorithms. Upper images in each year correspond to the separated background matrix, the lower images correspond to matrix of dynamic component. The videos cover 1.7 hours of observations starting at 06:00:00 UTC on 2011 June 7, 16:50:00 UTC on 2012 April 16 and 18:30:11 UTC on 2014 October 2.<br><br>The other videos correspond to Figure 7 in the article. They compare the results from PCP algorithm applied to the 30.4 and 17.1 nm AIA bandpasses. The videos starting at 16:50:00 UTC on 2012 April 16 and 18:30:11 UTC on 2014 October 2, respectively, and cover 1.7 hours of observations.</p>
Gamma-Ray Imager Polarimeter for Solar Flares Project
<p> We propose here to develop the <em>Gamma-Ray Imager/Polarimeter for Solar flares </em>(<em>GRIPS</em>), the next-generation instrument for high-energy solar observations. <em>GRIPS </em>will provide a nearoptimal combination of high-resolution imaging, spectroscopy, and polarimetry of solar-flare gamma-ray/hard X-ray emissions from ~20 keV to &gt;~10 MeV (see Table 1). The key new technology (already developed for non-solar astrophysics by collaborator Steven Boggs) is that of a 3D position-sensitive germanium detector (3D-GeD) that allows the position and energy deposition of every photon interaction to be recorded individually, even within the same detector. With the 3D-GeDs, <em>GRIPS </em>can use a new single-grid imaging system, called the Multi- Pitch Rotating Modulator (MPRM), that provides a near-ideal point response function with twice the throughput per cm2 of detector area compared to the rotating modulation collimator (RMC) imaging of <em>RHESSI</em>. In addition, since Compton scattering (the dominant interaction at &gt;~150 keV) of the incident photons can be tracked by the 3D-GeDs, much of the background can be rejected and the polarization of photons can be determined.</p> <p> The proposed balloon-borne <em>GRIPS </em>consists of a Spectrometer/Polarimeter with sixteen 3DGeDs in four stacked 2_2 planes, together with a single rotating MPRM grid placed 8 meters away, to provide a full-Sun field-of-view and angular resolution (12.5-arcsec FWHM at gamma ray energies) sufficient to separate the footpoints of 2.2 MeV sources for almost all flares.</p> <p> The spacecraft-borne version of <em>GRIPS </em>is envisioned to have sixty-four 3D-GeDs in four stacked 4_4 planes, together with a single grid ~20 meters away, in a spinning spacecraft. Such a space <em>GRIPS </em>would provide a tremendous leap forward for high-energy solar physics, with order of magnitude increases in effective area for gamma-ray line (and hard X-ray) imaging, and much better angular resolution and image quality (see Table 1). A space <em>GRIPS </em>will allow the 0.511 MeV positron-annihilation line and the weaker prompt nuclear de-excitation lines to be imaged for the first time. Together with line shifts and shapes from the simultaneous high-resolution spectroscopy, such an instrument will provide powerful new diagnostics of the flare energy release and particle acceleration process. Furthermore, precise polarization measurements would be obtained for the first time to constrain models and determine beaming of energetic electrons.</p>
High Spectral Resolution, High Cadence, Imaging X-ray Microcalorimeters for Solar Physics - Phase 2 Project
<p> Microcalorimeter x-ray instruments are non-dispersive, high spectral resolution, broad-band, high cadence imaging spectrometers. We have been developing these instruments for x-ray astrophysics for over 25 years and have successfully flown them on both suborbital and orbital observatories. Microcalorimeter spectrometers are true spatial-spectral event-driven instruments. The core instrument for the Astro-H observatory to be launched in 2014 and for the International X-ray Observatory planned for around 2022 [1] are both microcalorimeter spectrometers. For the past two years, supported by the Solar and Heliospheric ROSES program, we have been adapting this highly successful technology to the very different requirements of solar physics. This leverages the large NASA investment in this technology to produce instruments optimized for solar physics with only a moderate development program.</p> <p> During the past two years, we have developed a high spatial resolution, high cadence microcalorimeter optimized for solar observations with a ground-breaking spectral resolving power of nearly 3000 at 6 keV. This exceeds the performance goals of our program. In fact, the single-pixel performance achieved during this program is already sufficient for a solar optimized instrument as described in section 2, albeit using small arrays of detectors. We propose here to continue this successful program by developing large focal-plane arrays, optimized for solar physics and their read-out systems. This complements our existing development programs in astrophysics, where we have already produced and tested kilo-pixel arrays for IXO. The end-result of the proposed work will be a solar-optimized detector system proven and ready for integration into a suborbital payload and then onto a space-borne observatory. Both the suborbital program and an orbital instrument would allow high cadence spatial-spectral observations across the x-ray band from 0.1 to above 10 keV, enabling new science as described in section 1.4. Ultimately this will produce instrumentation suitable for deployment on an Explorer-class mission and, possibly, a remote sensing contribution to the Solar Energetic Particle Acceleration and Transport (SEPAT) Solar-Terrestrial Probe [2]. &nbsp;</p>
US Participation in the Solar Orbiter Multi Element Telescope for Imaging and Spectroscopy (METIS) Project
<p> The <em>Multi Element Telescope for Imaging and Spectroscopy, METIS</em>, investigation has been conceived to perform off-limb and near-Sun coronagraphy and is motivated by the aim of addressing the three key scientific questions identified as the focus of the HELEX program. These questions concern: the origin and heating/acceleration of the solar wind streams; the origin, acceleration and transport of the solar energetic particles; and the transient ejection of coronal mass and its evolution in the inner heliosphere (coronal mass ejections, CME&rsquo;s).</p> <p> The investigation aims to provide crucial tests apt to verify the hypotheses and models on the following main issues of solar coronal physics that have been developed primarily during the SOHO era:</p> <p> &bull; Is the slow solar wind originating according to more than one physical process and which is the level of contribution of the possible different sources of slow wind to the heliospheric wind observed &lsquo;in situ&rsquo;?</p> <p> &bull; How does the magnetic field topology control the outflow velocity and composition of the slow and fast solar wind?</p> <p> &bull; Is the magnetic field controlling the emergence of the fast wind at the base of coronal holes?</p> <p> &bull; Do polar plumes and inter-plume regions have a role in channeling the fast wind?</p> <p> &bull; Is ion cyclotron dissipation of fast Alfv&eacute;n waves the primary energy deposition process in the fast wind? &bull; Is the reconnection at the base of coronal holes responsible for the generation of waves and turbulence that energize the fast wind?</p> <p> &bull; Which is the nature of coronal heating in open and closed field regions?</p> <p> &bull; Which is the source of the seed particles of the Solar Energetic Particles (SEPs)?</p> <p> &bull; Which is the role of coronal shocks driven by coronal mass ejections in energizing SEPs? &bull; Which are the mass and magnetic fluxes carried out from the Sun during transient events?</p> <p> &bull; How does the evolution of the coronal magnetic field, inferred from the large-scale evolution of the outer corona, trigger coronal mass ejections?</p> <p> &bull; How does the corona re-adjust after coronal mass ejections on medium-term time scales, ranging between 3 and 10 days (not yet established in the outer corona)?</p> <p> &bull; How do the quiescent streamers evolve on time scales ranging between 3 and 10 days? The crucial tests for addressing and solving these still open issues can be achieved by combining the instrument&rsquo;s versatility with the uniqueness of the Solar Orbiter mission profile, which allows: a close approach to the Sun thus leading to a significant improvement in spatial resolution; quasi co-rotation with the Sun, which allows to nearly freeze for several days both the on-disk inner corona and the outer corona in the plane of the sky and, thus, disentangle the evolution of coronal structures and solar rotational effects on medium-term time scales, an outof- ecliptic view of the Sun. METIS instrument is designed to combine and extend the imaging and spectroscopic capabilities of the SOHO and STEREO coronagraphs and spectrometers in order to exploit at &nbsp;</p>
The Focusing Optics X-ray Solar Imager (FOXSI): Update & Second Launch Project
<p> Particle acceleration in solar flares and its contribution to coronal heating are among the main&nbsp; unsolved problems in heliophysics. Accelerated electrons in a plasma radiate hard X-ray (HXR)&nbsp; emission through the well-known process of bremsstrahlung. HXR observations therefore are a&nbsp; powerful diagnostic tool, providing quantitative measurements of flare-accelerated electrons. Since&nbsp; bremsstrahlung emission depends on the density of the ambient medium, solar HXR emission is&nbsp; usually brightest from below the transition region, where the density increases rapidly towards the&nbsp; photosphere. Electron beams entering the chromosphere lose energy quickly through collisions and&nbsp; produce relatively intense HXR emission at the footpoints of magnetic field lines. Electron beams&nbsp; moving in the relatively tenuous corona suffer very few collisions, losing little energy and producing&nbsp; only faint HXR emission. Present-day HXR instrumentation does not have the sensitivity to see&nbsp; faint HXR emission from electrons traveling in the corona, nor the dynamic range to see such&nbsp; faint emission in the presence of bright HXR footpoint emission in the chromosphere. Existing&nbsp; observations therefore show us only where energetic electrons are stopped, but not where they&nbsp; are accelerated, nor along what path they escape from the acceleration site. The most sensitive&nbsp; solar HXR observations so far are provided by the Reuven Ramaty High Energy Spectroscopic&nbsp; Imager (RHESSI) (Lin et al. 2002). These measurements are obtained with a non-focusing rotation&nbsp; modulation collimator (RMC) imaging technique (Hurford et al. 2002). RMCs and other types&nbsp; of non-focusing imaging, however, have intrinsically limited dynamic range and sensitivity. HXR&nbsp; focusing optics can overcome both of these limitations (Section 1.2.2).&nbsp;</p> <p> The Focusing Optics X-ray Solar Imager (FOXSI) is a sounding rocket payload funded under the&nbsp; NASA Low Cost Access to Space (LCAS) program to test HXR focusing optics combined with&nbsp; silicon strip detectors for solar observations (Krucker et al. 2009). The FOXSI program is being led&nbsp; by the Space Sciences Laboratory at UC Berkeley in collaboration with the Marshall Space Flight&nbsp; Center (MSFC) and the Japan Aerospace Exploration Agency (JAXA). FOXSI is on schedule&nbsp; and on budget for a launch in October 2010. FOXSI will offer imaging spectroscopy and&nbsp; unprecedented HXR sensitivity and dynamic range. FOXSI will be !100 times more sensitive than&nbsp; RHESSI at 10 keV, and, for the first time, detect the non-thermal counterparts of quiet sun network&nbsp; flares (Section 1.2.4).&nbsp;</p> <p> Here we propose a continuation of the FOXSI program which includes data analysis&nbsp; and a second flight with an upgraded version of FOXSI. At moderate cost, we propose to&nbsp; enhance the effective area, in particular at higher energies (by a factor of !4 at 15 keV), by adding&nbsp; 3 more shells to the existing 7-shell optics (see Figure 9). Furthermore, our Japanese collaborators&nbsp; will provide, at no cost, newly available double-sided cadmium telluride (CdTe) detectors as&nbsp; a replacement for the Si detectors to allow us to take full advantage of the effective area at higher&nbsp; energies. A second flight will therefore not only allow us to continue testing HXR focusing&nbsp; optics for solar observations and also test newly developed CdTe strip detectors&nbsp; in flight but is also expected to provide a significant increase in scientific return. In&nbsp; this two year proposal, the first year (2011) will be used to upgrade the FOXSI payload and to&nbsp; analyze data from the first flight, while the second flight is planned for the midd
Thin Silicon Detector Technology for Use in Imaging Solar ENAs Project
<p> <strong>Top Level Objective: </strong>To enable capabilities for imaging and spectral measurements of energetic neutral hydrogen atoms (ENAs) produced with energies <em>&sim;</em>1MeV/nuc in explosive solar events.</p> <p> <strong>Overarching Science Question: </strong>How and why does the Sun vary and affect the Earth and the rest of the solar system? [NASA 2010 Science Plan]</p> <p> <strong>Primary Scientific Application: </strong>Investigation of energetic particle acceleration by shocks and/or magnetic reconnection in the solar corona. <strong>Technology: </strong>Ultra-thin (<em>&lt;</em><em>&sim; </em>10 <em>&mu;</em>m) silicon strip detectors with spatial resolution an order of magnitude better than previously achieved. <strong>Approach: </strong>Detectors fabricated on thin membranes supported by a thick frame made using micro-electro-mechanical systems (MEMS) techniques starting from commercially-available silicon-on-insulator (SOI) wafers. <strong>Technical Advantages: </strong>Ease of manufacture, mechanical robustness, excellent membrane uniformity, flexible approach that can be customized for numerous applications.</p> <p> <strong>Most Immediate Application: </strong>ENA imaging in SEP events using a combination of coded aperture imaging and <em>dE/dx </em>versus total energy particle identification with energy threshold below 1MeV.</p> <p> <strong>Benefits for Heliophysics: </strong>ENA imaging capability provides a fundamentally new probe of acceleration processes occurring in the corona.</p> <p> <strong>Status of Development: </strong>Simpler position-sensitive thin <em>dE/dx </em>detectors produced from SOI wafers has been demonstrated and are planned for use on the Solar Probe Plus mission.</p> <p> <strong>Proposed New Effort: </strong>1) Produce and test thin detectors with position resolution <em>&sim;</em>0.1&ndash;0.2mm. 2) Produce thin dead layers suitable for detectors with overall thickness <em>&lt;</em>10 <em>&mu;</em>m. 3) Determine how thin <em>dE/dx </em>detectors can be made using the SOI technique. 4) Demonstrate how large a detector active area can be achieved using SOI. 5) Simulate application of this type of detector in a solar ENA imager.</p> <p> <strong>Technological Goal: </strong>Take the thin-silicon strip detector technology from TRL2 (technology concept and/or application formulated) to TRL3-4 (analytical and experimental critical function and/or characteristic proof-of-concept [TRL3]; component and/or breadboard validation in laboratory environment [TRL4]) to enable future prototyping of an optimized solar ENA imager. &nbsp;</p> <p> N/A</p>
Solar Bolometric Imager for Investigating the Sources of Solar Irradiance Variability Project
<p> N/A</p>
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Allen Brain Atlas
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International Brain Laboratory public data
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OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.