Time Variability of the “Quiet” Sun Observed with TRACE. II. Physical Parameters, Temperature Evolution, and Energetics of Extreme-Ultraviolet Nanoflares

By Markus J. Aschwanden, T. Tarbell, R. Nightingale, C. Schrijver, A. Title, C. Kankelborg, Piet Martens, H. Warren. 2000

290 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/484e00117f65b51dc6b923bb84186b2cb6fb7c2d

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Citations in the corpus

Statistics, Morphology, and Energetics of Ellerman Bombs (2002, unknown): “Several statistical properties of EBs are similar to statistical properties of EUV and soft X-ray BPs in the transition region and the low corona (Shimizu 1995; Krucker & Benz 1998; Berghmans, Clette, & Moses 1998; Parnell & Jupp 2000; Aschwanden et al. 2000; Aletti et al. 2000).”
Avalanche models for solar flares (Invited Review) (2001, background): “In the context of Equation (2), Parker’s conjecture evidently requires α > 2, and observations are now getting close to detecting 1024 erg events (Aschwanden et al., 2000b).”
SUPERFLARES ON SOLAR-TYPE STARS OBSERVED WITH KEPLER. I. STATISTICAL PROPERTIES OF SUPERFLARES (2013, background): “It is interesting to note that these distributions are quite similar to those for solar flares (e.g., Aschwanden et al. 2000) and stellar flares on red dwarfs (e.g., Shakhovskaia 1989).”
Nanoflare Statistics from First Principles: Fractal Geometry and Temperature Synthesis (2002, methodology): “…with single instruments in a restricted temperature range (e.g., Berghmans, Clette, & Moses 1998; Krucker & Benz 1998; Parnell & Jupp 2000; Aschwanden et al. 2000b, 2000c), while only few studies with more comprehensive temperature coverage exist (Berghmans, McKenzie, & Clette 2001;…”
An Ab Initio Approach to the Solar Coronal Heating Problem (2004, background): “This balance is for a typical point in time, and it is obvious that the heating in the corona is decreasing with height, as found from TRACE data by a number of authors (Schrijver et al. 1999; Aschwanden et al. 2000a, 2001).”
EUV Flare Activity in Late-Type Stars (2000, background): “…flare energies, from α ≈ 1.6 for small active-region transient brightenings (Shimizu 1995) to α = 2.3 − 2.6 for small events in the quiet solar corona (Krucker & Benz 1998), and other " intermediate " values (e.g., Porter, Fontenla, & Simnett 1995; Aschwanden et al. 2000; Parnell & Jupp 2000).”
Elementary Loop Structures in the Solar Corona Analyzed from TRACE Triple-Filter Images (2005, methodology): “…0:56) ; 109 cm 3 for 30 loops detected in 171 8 with EIT (Aschwanden et al. 1999), ne ¼ (2:44 0:87) ; 109 cm 3 for 18 loops detected in 195 8 with EIT (Aschwanden et al. 2000a), ne ¼ (3:12 1:00) ; 109 cm 3 for 17 loops detected in 284 8 with EIT (Aschwanden et al. 2000a), and ne 109 cm 3 for 41…”
Can Superflares Occur on Our Sun (2012, background): “The dashed line, dotted line, and dot-dashed line indicate the power-law distribution of solar flares observed in EUV (Aschwanden et al. 2000), soft X-rays (Shimizu 1995), and hard X-rays (Crosby et al. 1993), respectively.”
Observational Tests of Damping by Resonant Absorption in Coronal Loop Oscillations (2003, unknown): “12 in Aschwanden et al. 2000).”
25 Years of Self-Organized Criticality: Solar and Astrophysics (2014, background): “…Veronig et al. (2002a,b), Aschwanden and Freeland (2012); 16) Krucker and Benz (1998), McIntosh and Gurman (2005); 17) Parnell and Jupp (2000), Aschwanden et al. (2000b), Benz and Krucker (2002), Aschwanden and Parnell (2002), Georgoulis et al. (2002); 18) Aschwanden and Shimizu (2013),…”
Statistical properties of superflares on solar-type stars based on 1-min cadence data (2015, background): “The frequencyenergy distribution of solar flares can be fitted by a simple power-law function with an index of −1.5 to −1.9 in the flare energy range between 1024 and 1032 erg (e.g., Aschwanden et al. 2000; Shimizu1995; Crosby et al. 1993).”
RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, methodology): “…1025 erg per event, and in EUV using the SOHO EUV Imaging Telescope (EIT; Krucker & Benz 1998; Benz & Krucker 2002) and TRACE (Parnell & Jupp 2000; Aschwanden et al. 2000), providing energies between 1024 and 1027 erg. Small events in active regions, termed ‘‘active region transient…”
The solar magnetic field (2006, background): “The energy output from the chromosphere and corona is considerable: about 1000 and 300 Wm−2 are the estimated mean outward energy flux densities from the respective atmosphere layer of the quiet Sun [556, 557] into EUV and x-ray radiation, electron heat conduction and into the solar wind.”