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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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A non-radial eruption in a quadrupolar magnetic configuration with a coronal null

TL;DR: In this paper, the authors reported one of the several homologous non-radial eruptions from NOAA active region (AR) 11158 that are strongly modulated by the local magnetic field as observed with the Solar Dynamic Observatory.
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Thermal instability and non-equilibrium in solar coronal loops: from coronal rain to long-period intensity pulsations

TL;DR: In this paper, a connection between the observed properties of hot and cool material in thermal non-equilibrium and instability and the underlying coronal heating mechanisms is made, and the outstanding open questions in what constitutes a new, rapidly growing field of solar physics are identified.
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Solar Cycle Variation in Solar Irradiance

TL;DR: The correlation between solar irradiance and the 11-year solar activity cycle is evident in the body of measurements made from space, which extend over the past four decades as discussed by the authors, and the key challenges in reconciling the divergence between the two have been discussed.
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Apparent Solar Tornado-Like Prominences

TL;DR: In this paper, the authors discuss two different cases where prominences on the limb might appear to have a tornado-like behavior, one case of apparent vortical motions in prominence spines and barbs arises from the 2D counterstreaming plasma motion along the prominence spine and bars together with oscillations along individual threads.
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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