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Open AccessJournal ArticleDOI

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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Journal ArticleDOI

Critical Height of the Torus Instability in Two-ribbon Solar Flares

TL;DR: In this article, the background field of source active regions is approximated by a potential field extracted from the Bz component of vector magnetograms provided by the Helioseismic and Magnetic Imager.
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A Survey of Nanoflare Properties in Active Regions Observed with the Solar Dynamics Observatory

TL;DR: In this article, the authors examined 15 different active regions (ARs) observed with the Solar Dynamics Observatory and analyzed their nanoflare properties, finding that the widespread cooling reported previously for NOAA AR 11082 is a generic property of all ARs.
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IRIS, Hinode, SDO, and RHESSI Observations of a White Light Flare Produced Directly by Non-thermal Electrons

TL;DR: In this article, the authors measured the temporal variation of the plasma properties in the bright kernel in the chromosphere and corona and found that explosive evaporation was observed when the white light emission occurred, even though the intensity enhancement in hotter lines is quite weak.
Journal ArticleDOI

Solar Demon – an approach to detecting flares, dimmings, and EUV waves on SDO/AIA images

TL;DR: An overview of Solar Demon is given, with a focus on the algorithms for EUV wave detection and characterization, and several first results, such as flare and dimming butterfly diagrams for the rising part of Solar Cycle 24, are presented.
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Determining heating rates in reconnection formed flare loops of the m8.0 flare on 2005 may 13

TL;DR: In this article, the authors used the spatially resolved (down to 1'') UV light curves and the thick-target hard X-ray emission to construct heating functions of a few thousand flare loops anchored at the UV footpoints, and computed plasma evolution in these loops using the enthalpy-based thermal evolution of loops model.
References
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Journal ArticleDOI

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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