RUSSIAN JOURNAL OF EARTH SCIENCES, VOL. 17, ES4003, doi:10.2205/2017ES000606, 2017


Figure 9. (a) Latitudinal distribution on 2001, 02/01 (day 032) of the particle precipitation zones as derived from the OVATION-prime model (left top panel); WIC intensity along the longitude $\Lambda=317.5\mbox{°}$ on 0425:55 UT (upper panel), magnetic field disturbance (solid line – $X$ component; dashed line – $Z$ component; dotted line – $Y$ component) along $\sim 330\mbox{°}$ profile as compared with reference field at 0425 UT estimated for the period 0428 UT $\pm$2.5 min (left third panel), and Pi2 power in the 5–30 mHz band (left bottom panel) taken during the time interval around auroral activation (0430 UT $\pm 2.5$ min). {b} The same format but for $\Lambda=325.5\mbox{°}$, UVI image at 0444:20 UT, magnetic field disturbance as compared with reference field at 0437 UT estimated for the period 0443 UT $\pm$2.5 min (right third panel), and Pi2 power during 0445 UT $\pm$7.5 min.


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Citation: Martines-Bedenko V. A., V. A. Pilipenko, M. J. Engebretson, M. B. Moldwin (2017), Time-spatial correspondence between Pi2 wave power and ultra-violet aurora bursts, Russ. J. Earth Sci., 17, ES4003, doi:10.2205/2017ES000606.


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