1. Response to Comment on “Tail Reconnection Triggering Substorm Onset”
by Vassilis Angelopoulos, James P. McFadden, Davin Larson, Charles W. Carlson, Stephen B. Mende, Harald Frey, Tai Phan, David G. Sibeck, Karl-Heinz Glassmeier, Uli Auster, Eric Donovan, Ian R. Mann, I. Jonathan Rae, Christopher T. Russell, Andrei Runov, Xu-Zhi Zhou, and Larry Kepko
Science
Volume 324(5933):
June 12, 2009
Published by AAAS

2. Fig. 1 (A) Ion distribution function at P2 near the time of reconnection onset in Vperp-Vpar space.
(A) Ion distribution function at P2 near the time of reconnection onset in Vperp-Vpar space. (B) Same for P1. (C, F, I, and K) Convective ion flow velocity. (D, G, J, and L) ZGSM (Geocentric Solar Magnetospheric) component of the magnetic field. (E and H) Integrated (EVxB)y on P1 and P2, showing local flux transport. Vertical lines correspond to reconnection and current disruption onsets from (1).
Vassilis Angelopoulos et al. Science 2009;324:1391
Published by AAAS

3. Fig. 2 (A) Kyoto Provisional AL index, used in (2), and THEMIS AL index, including additional Canadian stations.
(A) Kyoto Provisional AL index, used in (2), and THEMIS AL index, including additional Canadian stations. (B) Mid-latitude Pi2 pulsation data from Pine Ridge, used in (1). (C) Total lobe pressure determined from low-energy plasma and magnetic field data on P1 and P2 satellites. (D) Same as in Fig. 1, E and H, but for a longer interval. (E and H) Ion partial flow velocity from the ESA instruments on P1 and P3, respectively. (F and H) Same as Fig. 1, C and I, but for a longer interval. (G and I) Magnetic field on P1 and P3. All vectors are in GSM coordinates; X component is blue, Y component is green, and Z component is red. Vertical lines correspond to tail reconnection onset for the two substorms, based on the times of tailward or equatorward flow.
Vassilis Angelopoulos et al. Science 2009;324:1391
Published by AAAS