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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 Database of Flare Ribbon Properties from the Solar Dynamics Observatory. I. Reconnection Flux

TL;DR: In this article, the authors present a database of 3137 solar flare ribbon events corresponding to every flare of GOES class C1.0 and greater within 45 degrees from the central meridian, from April 2010 until April 2016, observed by the Solar Dynamics Observatory.
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Structures of Interplanetary Magnetic Flux Ropes and Comparison with Their Solar Sources

TL;DR: In this paper, the magnetic field-line twist distribution within interplanetary magnetic flux ropes is systematically derived and examined, showing that the amount of twisted flux per AU in MCs is comparable with the total reconnection flux on the Sun, and the sign of the MC helicity is consistent with the signs of the helicity of the solar source region judged from the geometry of postflare loops.
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A statistical study of decaying kink oscillations detected using SDO/AIA

TL;DR: In this paper, the authors carried out a statistical study of kink oscillations using extreme ultraviolet imaging data from a previously compiled catalogue and found that the initial oscillation amplitude is correlated with the initial amplitude of coronal loops.
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The SPoCA-suite: Software for extraction, characterization, and tracking of active regions and coronal holes on EUV images

TL;DR: In this paper, a set of segmentation procedures (known as the SPoCA-suite) is introduced to retrieve AR and CH properties on EUV images taken from SOHO-EIT, STEREO-EUVI, PROBA2-SWAP, and SDO-AIA.
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Three-dimensional radio and x-ray modeling and data analysis software: revealing flare complexity

TL;DR: In this paper, an enhanced software architecture allows the user to import photospheric magnetic field maps and perform magnetic field extrapolations to generate 3D magnetic field models; investigate the magnetic topology by interactively creating field lines and associated flux tubes; populate the flux tubes with user-defined non-uniform thermal plasma and anisotropic, nonuniform, non-thermal electron distributions; and compare the model-derived images and spectra with observational data.
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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