Flare Plasma Cooling from 30 MK down to 1 MK modeled from Yohkoh, GOES, and TRACE observations during the Bastille Day Event (14 July 2000)

By Markus J. Aschwanden, D. M. Alexander. 2001

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View Paper: https://www.semanticscholar.org/paper/f08701a7314f2514d18923f1694ad6cb566b7996

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In Astronomy and Astrophysics

Citations in the corpus

Updated Expressions for Determining Temperatures and Emission Measures from Goes Soft X-Ray Measurements (2005, background): “…detectors have provided an essentially uninterrupted monitor of the Sun’s activity for 30 years, and are a valuable resource for the study of past solar activity and the prediction of space weather (e.g., Bornmann, 1990, Phillips and Feldman, 1995, Aschwanden and Alexander, 2001, Garcia, 2004).”
OBSERVING FLUX ROPE FORMATION DURING THE IMPULSIVE PHASE OF A SOLAR ERUPTION (2011, background): “The delay is probably caused by the cooling from high to low temperature of the plasma located in and surrounding the reconnection region (Aschwanden & Alexander 2001; Warren et al. 2003).”
RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, background): “It is important to remove these instrumental effects to recover the underlying DEM, but this is a complicated process and has only been successful for individual large flares (cf. Aschwanden & Alexander 2001).”
An Observational Overview of Solar Flares (2011, background): “…wavelength, their angle with respect to the magnetic polarity inversion line may increase, as report d sinceSkylabin many events (e.g., Sakurai et al. 1992; Sakao 1994; Masuda et al. 2001; Aschwanden & Alexander 2001; Su et al. 2006; Schmahl et al. 2006; Ji et al. 2008; Liu et al. 2009b).”
Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares (2011, background): “…that thermal conduction dominates in flare loops at high temperatures as observed in soft Xray wavelengths, while radiative cooling dominates in the later phase in postflare loops as observed in EUV wavelengths (Antiochos and Sturrock 1978; Culhane et al. 1994; Aschwanden and Alexander 2001).”
Particle acceleration and kinematics in solar flares – A Synthesis of Recent Observations and Theoretical Concepts (Invited Review) (2002, background): “…and Benz 1997, 6) Aschwanden et al. 1993a, 1995c, Melendez 1998; Melendez et al., 1999, Xie et al. 2000, 7) Hanaoka 1999, 8) Dennis et al. 1984, Aschwanden et al. 1993a, 1995c, 1995d, 9) Aschwanden, Benz, and Kane 1990, 10) Benz, Csillaghy, and Aschwanden 1996, 11) Aschwanden and Alexander 2001.”
Hard X-ray emission from the solar corona (2008, background): “observed in realistic flares, where we know that multiple loops, “lighting up” at different times, are involved (Hori et al 1998; Aschwanden and Alexander 2001; Warren 2006).”
Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology (2010, background): “The problem of the cooling of hot or post-flare loops was previously studied in both observation and theory by many authors (e.g. Antiochos & Sturrock 1978; Antiochos 1980; Culhane et al. 1994; Cargill et al. 1995; Harra-Murnion et al. 1998; Aschwanden & Alexander 2001; Kamio et al. 2003).”