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The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

TLDR
The Atmospheric Imaging Assembly (AIA) as discussed by the authors provides multiple simultaneous high-resolution full-disk images of the corona and transition region up to 0.5 R ⊙ above the solar limb with 1.5-arcsec spatial resolution and 12-second temporal resolution.
Abstract
The Atmospheric Imaging Assembly (AIA) provides multiple simultaneous high-resolution full-disk images of the corona and transition region up to 0.5 R ⊙ above the solar limb with 1.5-arcsec spatial resolution and 12-second temporal resolution. The AIA consists of four telescopes that employ normal-incidence, multilayer-coated optics to provide narrow-band imaging of seven extreme ultraviolet (EUV) band passes centered on specific lines: Fe xviii (94 A), Fe viii, xxi (131 A), Fe ix (171 A), Fe xii, xxiv (193 A), Fe xiv (211 A), He ii (304 A), and Fe xvi (335 A). One telescope observes C iv (near 1600 A) and the nearby continuum (1700 A) and has a filter that observes in the visible to enable coalignment with images from other telescopes. The temperature diagnostics of the EUV emissions cover the range from 6×104 K to 2×107 K. The AIA was launched as a part of NASA’s Solar Dynamics Observatory (SDO) mission on 11 February 2010. AIA will advance our understanding of the mechanisms of solar variability and of how the Sun’s energy is stored and released into the heliosphere and geospace.

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Fast extreme-ultraviolet dimming associated with a coronal jet seen in multi-wavelength and stereoscopic observations

TL;DR: In this article, a coronal jet was observed near the limb on 2010 June 27 by the Hinode/X-Ray Telescope (XRT), EUV Imaging Spectrograph (EIS), and Solar Optical Telescope (SOT), and by the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), and on the disk by STEREO-A/EUVI.
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Deep Flare Net (DeFN) model for solar flare prediction.

TL;DR: Wang et al. as discussed by the authors developed a solar flare prediction model using a deep neural network (DNN), named Deep Flare Net (DeFN), which can calculate the probability of flares occurring in the following 24 hours in each active region, which is used to determine the most likely maximum classes of flares via a binary classification.
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Unambiguous Evidence of Filament Splitting-induced Partial Eruptions

TL;DR: In this paper, the authors investigated two partial eruption events including a confined and a successful one, and they confirmed the existence of extended bald-patch sections for the successful eruption, signified by brightenings in the body of one filament and between the rising and remaining parts of both filaments.
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Triggering an Eruptive Flare by Emerging Flux in a Solar Active-Region Complex

TL;DR: In this article, the evolution of the photospheric magnetic flux and the coronal structure was analyzed, and it was found that the flux emergence triggered the eruption by interaction with overlying flux in a non-standard way.
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Measurements of EUV Coronal Holes and Open Magnetic Flux

TL;DR: In this paper, the authors measured coronal hole areas and magnetic flux in these holes, and compared the measurements with calculations by the PFSS model, and showed that coronal holes in low latitudes contribute significantly to the total open magnetic flux.
References
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CHIANTI - an atomic database for emission lines - I. Wavelengths greater than 50 Å

TL;DR: The CHIANTI database as mentioned in this paper is a set of atomic data and transition probabilities necessary to calculate the emission line spectrum of astrophysical plasmas, including atomic energy levels, atomic radiative data such as wavelengths, weighted oscillator strengths and A values, and electron collisional excitation rates.
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The X-Ray Telescope (XRT) for the Hinode Mission

TL;DR: The X-ray Telescope (XRT) of the Hinode mission as mentioned in this paper provides an unprecedented combination of spatial and temporal resolution in solar coronal studies, and the high sensitivity and broad dynamic range of XRT, coupled with the spacecraft's onboard memory capacity and the planned downlink capability, will permit a broad range of solar studies over an extended period of time for targets ranging from quiet Sun to X-flares.
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