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On Formation Of A Shock Wave In Front Of A Coronal Mass Ejection With Velocity Exceeding The Critical One

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New study confirms conclusions made in [6]; according to it, there is a disturbed region expended along the CME propagation direction in front of a coronal mass ejection whose velocity u is lower than the critical uC relative to the surrounding coronal plasma. The time difference brightness (plasma density) in the disturbed region smoothly decreases to larger distances in front of CME.

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“…Notice that CMEs with velocities V close to the critical velocity VC (Figure 2 d-g) propagate near the plane of the sky; thus, their measured velocity is close to the real one ( Figure 2 shows coordinates of places of the CME initiation on the solar disk, taken from [2] and Solar-Geophysical Data 3.5 (http://sgd.ngdc.noaa.gov). Appearance of such a discontinuity at the front boundary of the disturbed region at V > V C was first described in [6].…”

Global network of slow solar wind

“…[23] The concept of a pseudostreamer belt has been discussed for some time in the literature, although not by that name [e.g., Eselevich, 1998;Eselevich et al 1999;Zhao and Webb, 2003]. Here, following Titov et al [2011], we propose that pseudostreamer belts are threaded by the quasi-or true separatrix layers of the separatrix-web (S-web) model of the slow solar wind proposed by Antiochos et al [2011Antiochos et al [ , 2012.…”

White-Light Observations and Polarimetric Analysis of the Solar Corona During the Eclipse of 1 August 2008

“…The NL configuration is obtained from WSO magnetic field calculations in the potential approximation (http://wso.stanford.edu/synsourcel.html). The NL shape, in the first approximation, is known to be similar to that of the streamer belt (Wilcox and Hundhausen, 1983;Eselevich, Fainshtein, and Rudenko, 1999). Figures 2 and 3 present streamers and their corresponding NL regions (streamer belt), marked by the same symbols (SE, NE, etc.).…”

“…Nowadays three large-scale structures are distinguished that differ in the configuration of their magnetic fields. These are coronal holes (coronal regions with open field lines), the coronal streamer belt (separating coronal holes with opposite magnetic polarity), and chains of streamers (Eselevich, Fainshtein, and Rudenko, 1999) or pseudostreamers (Wang, Sheeley, and Rich, 2007), separating coronal holes with the same magnetic field polarity. The feet of the streamer belt and chains of streamers (pseudo-streamers) are formed by closed field lines with different configurations (see monographs Schwenn and Marsch, Aschwanden, 1990Aschwanden, , 2004 as well as other original papers Hoeksema, 1984;Eselevich, Fainshtein, and Rudenko, 1999;Wang, Sheeley, and Rich, 2007).…”