Elemental Abundances and Post-Coronal Mass Ejection Current Sheet in a Very Hot Active Region

By A. Ciaravella, J. C. Raymond, Jun Yu Li, P. Reiser, L. Gardner, Y. Ko, S. Fineschi. 2002

139 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d1ac706b500fb73a635dd6ad787cf0cc83dd6d8a

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In Astronomy and Astrophysics

1. J. C. Raymond
2. A. A. Ballegooijen
3. Guillermo Stenborg
4. J. Lin
5. S. Cranmer
6. Y. Ko
7. K. Reeves
8. T. Forbes

Citations in the corpus

• Evidence for the Formation of a Large-Scale Current Sheet in a Solar Flare (2003, background): “There is some further observational evi- 1 Department of Physics, Catholic University of America, 620 Michigan Avenue, Washington, DC 20064. dence of current sheets associated with CMEs (Webb et al. 2003; Ciaravella et al. 2002; Ko et al. 2003).”
• RECONNECTION OUTFLOWS AND CURRENT SHEET OBSERVED WITH HINODE/XRT IN THE 2008 APRIL 9 “CARTWHEEL CME” FLARE (2010, background): “Our thickness estimate of (4-5)x103 km is at least 10 times narrower than the estimate range of (30-100)x103 km measured by Ciaravella & Raymond (2008), Lin et al. (2007), Webb et al. (2003), Ciaravella et al. (2002), and Ko et al. (2002).”
• The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions (2004, background): “…details of CME processes in a realistic plasma environment, and the results regarding the dynamic behavior of the current sheet are fairly consistent with observations (see Švestka 1996; Švestka et al. 1997; Švestka & Fárnı́k 1998; Ciaravella et al. 2002; Ko et al. 2003; and Webb et al. 2003).”
• AUTOMATED LASCO CME CATALOG FOR SOLAR CYCLE 23: ARE CMEs SCALE INVARIANT? (2008, background): “Ample observational and numerical evidence proves their existence and dynamics observed as bursty outflow (e.g. Ko et al. 2003; Webb et al. 2003; Riley et al. 2007; Ciaravella et al. 2002; Bemporad et al. 2006, and references therein).”
• Dynamical and Physical Properties of a Post-Coronal Mass Ejection Current Sheet (2003, methodology): “The appearance of the [Fe xviii] emission means a temperature as high as 6 106 K in that area (Ciaravella et al. 2002).”
• Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 (2005, background): “…from the Ultraviolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory (SOHO) together with other remote-sensing data, Ciaravella et al. (2002) and Ko et al. (2003) have conducted comprehensive analyses of various aspects of several eruptive processes that clearly…”
• Ultraviolet spectroscopy of the extended solar corona (2006, background): “On 23 March 1998, Ciaravella et al. (2002) detected a very narrow feature in the [Fe XVIII] 97.4 nm line formed near 10 K on the line connecting bright post-flare loops and the core of a CME.”