Statistical Analysis of the Energy Distribution of Nanoflares in the Quiet Sun

By C. Parnell, Peter E. Jupp. 2000

265 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7a5424706b6d68b73f9b370b111d6dcbb7770e0f

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Citations in the corpus

Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “These DC mechanisms are often associated with nanoflares: tiny episodic bursts of energy that may dominate the coronal heating (Parker 1988; Parnell and Jupp 2000; Joulin et al. 2016).”
Temporal aspects and frequency distributions of solar soft X-ray flares (2002, methodology): “Krucker & Benz (1998) and Parnell & Jupp (2000) analyzed energy distributions of events from quiet Sun regions, so-called network flares (Krucker et al. 1997), observed in Extreme Ultraviolet emission, finding α in the range 2.3–2.6 and 2.1–2.6, respectively.”
25 Years of Self-Organized Criticality: Solar and Astrophysics (2014, background): “However, the anomalously steeper powerlaw slopes reported for nanoflares early on (Benz and Krucker 1998; Parnell and Jupp 2000), have been downwardcorrected later on due to inadequate modeling effects (McIntosh and Charbonneau 2001; Benz and Krucker 2002; Aschwanden and Parnell 2002), and are now…”
EUV Flare Activity in Late-Type Stars (2000, background): “For " normal " flares, α ≈ 1.5 − 1.8 (Crosby et al. 1993); it takes different values for smaller 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 " va”
RHESSI Microflare Statistics. I. Flare-Finding and Frequency Distributions (2008, methodology): “Observations of bursts in the quiet Sun have estimated the thermal energy to be between 1024 and 1026 erg (Krucker & Benz 1998; Parnell & Jupp 2000).”
X-ray spectroscopy of stars (2009, background): “Solar studies indicate α values of 1.6−1.8 for ordinary solar flares (Crosby et al, 1993), but some recent studies of low-level flaring suggestα = 2.0−2.6 (Krucker and Benz, 1998; Parnell and Jupp, 2000).”
Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds (2005, background): “The energy release from each event is generally thought to be small, categorized as a microflare or nanoflare [ Parnell and Jupp, 2000; Katsukawa and Tsuneta, 2001].”
RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, methodology): “…finding energies of 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…”
The Sun in Time: Activity and Environment (2007, background): “From solar studies, α ≈ 1.6 – 1.8 for ordinary solar flares (Crosby et al., 1993), but some recent studies of low-level flaring suggest α = 2.0 − 2.6 (Krucker and Benz, 1998; Parnell and Jupp, 2000).”
Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs (2019, background): “Over short time scales of minutes to a few hours, they emit energy ranging form 1023 erg (nanoflares; e.g. Parnell & Jupp 2000) to 1033 − 1038 erg (superflares; e.g. Shibayama et al. 2013).”
A Flux-Tube Tectonics Model for Solar Coronal Heating Driven by the Magnetic Carpet (2002, methodology): “Krucker et al. (1997) have observed microflares with the EIT instrument on SOHO, while Parnell & Jupp (2000) have detected nanoflares with TRACE and shown that most of them lie above supergranule boundaries, although there are not yet any detections at a small enough size to be providing the bulk…”
Time Variability of the “Quiet” Sun Observed with TRACE. II. Physical Parameters, Temperature Evolution, and Energetics of Extreme-Ultraviolet Nanoflares (2000, methodology): “In the same energy range, another T RACE data set of 171/195 Ðlter ratiosA has been analyzed by Parnell & Jupp (2000), who employ a similar variability detection algorithm (however, without discrimination of Ñarelike and nonÑare events), and Ðnd from a number of 4497 events with a signiÐcance of º3…”
Stellar Activity on the Young Suns of Orion: COUP Observations of K5-7 Pre-Main-Sequence Stars (2005, background): “Recent statistical investigations suggest = 2.0–2.6 for small flares in the quiet solar corona (Krucker & Benz 1998; Parnell & Jupp 2000).”
Nanoflare Statistics from First Principles: Fractal Geometry and Temperature Synthesis (2002, methodology): “…heating by numerous undetectable nanoflares is one of the most quoted theories in the context of coronal heating, and support of this hypothesis has been sought by apparent measurements of power-law distributions of nanoflare energies with values of e2 (Krucker & Benz 1998; Parnell & Jupp 2000).”
An Ab Initio Approach to the Solar Coronal Heating Problem (2004, background): “…appeared to be the most promising candidate, but it now seems that the energy dissipated in the observed flare distribution, extrapolated to a cutoff at nanoflare energies, is too small (Aschwanden et al. 2000c; Parnell & Jupp 2000; Aschwanden & Parnell 2002; Aschwanden & Charbonneau 2002).”
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).”