Addition et Soustraction de Divers Nombres par un Nombre à 1 Chiffre (Gros Caractère) (A)

Two of the examples (December 21, 1997; March 5, 1998) are low- to intermediate-shear cross- ings; one contains two magnetopause crossings under conditions of exceptionally high

We present a linear clustering model of cosmic infrared background (CIB) anisotropies at large scales that is used to measure the cosmic star formation rate density up to redshift

stratosphere and lower mesosphere is presented in Figure 3 for the October 2003 – April 2004 period, using both MIPAS and GOMOS data for latitudes higher than 65°N.. The daily-

The results obtained from the model when the neutral wind is given by HWM90 reproduce the observations that the electron density at 600 km altitude is higher in the summer

change in the calculated wave azimuth. W can also be calculated from the average of the line-of-sight velocities in the o€-vertical beams, i.e. Figure 6 shows a visible-light

In this case we can expect variation of the energetic particle source amplitude (which is proportional to the electron density in a cloud), pitch-angle anisotropy, and

A surprising result was that for pulsation signals away from the local ®eld line resonance (FLR) frequency the phase of the ionospheric Doppler oscillations was found to

Correlation coecient between CUTLASS ®rst range returns and EISCAT electron density at 235 km, introducing a time delay in the CUTLASS data proportional to the distance from