All Figures

$\begin{figure} \par\includegraphics[width=6.7cm,angle=90]{QuemeraisAA5169f01.eps}\end{figure}$ Figure 1: full-sky map of the velocity difference between the 1996 map and the 1997 map. The data are shown in ecliptic coordinates (west ecliptic longitude). The blue color in the upwind side shows that the upwind velocity in 1997 is slightly slower (in modulus), by 0.4 km s^-1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f02.eps}\end{figure}$ Figure 2: Variation in the LOS velocity as a function of the angle of the LOS with the upwind direction. Here, the upwind direction is taken to be 252.3 $^{\circ }$ , 8.7 $^{\circ }$ . Both curves are very similar showing that the 1996 and 1997 velocity profiles are very close and correspond to solar minimum conditions. The solid line joins the values found in 1996 and the dotted line joins the 1997 values.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f03.eps}\end{figure}$ Figure 3: Difference in LOS velocity between the 1996 orbit and the five other orbits. The velocities are shown as a function of the angle with the upwind direction. The 1996 velocity profile is shown in Fig. 2. The 1997 profile (solid line, top) is very close to the 1996 profile. The 1999 one (solid line bottom) is an intermediary profile, while the 2000 (dotted line), 2001 (dashed line), and 2002 (dash-dot line) profiles are very similar.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,angle=90]{QuemeraisAA5169f04.eps}\end{figure}$ Figure 4: Difference between the velocity maps of 2001 and 1996. The maximum difference is found in the upwind direction with a value around 4 km s^-1. Downwind, the difference is close to zero. Below 10 degrees of latitude, the results are very noisy. Contours of the 1996 velocity map are shifted towards higher latitudes than the contours of the 2001 velocity map. This is due to the existence of anisotropies in the hydrogen distribution of 1996 which create a deviation from the non-isotropic 2001 distribution.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f05.eps}\end{figure}$ Figure 5: LOS kinetic temperature as a function of the upwind angle. The values were obtained for the two orbits in 1996 and 1997. For each orbit, there are 2 curves, one for angles smaller than 30 $^{\circ }$ and one for angles larger than 30 $^{\circ }$ . For angles smaller than 30 $^{\circ }$ , the limit on stellar light counts has been relaxed to ensure that some points with a small contamination are kept. Contrary to hot model predictions, the temperature curve is not monotonic and shows a minimum value of 11 000 K for angles close to 60 $^{\circ }$ . The 1996 values are given by the diamonds and the 1997 values are given by the triangles.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f06.eps}\end{figure}$ Figure 6: Model of the line profile generated for two distinct populations of hydrogen atoms. One has the parameters of the interstellar gas, i.e. velocity of 30 km s^-1 (26 km s^-1 accelerated by selection effects, see text) and a temperature of 6000 K, the other has parameters reflecting a deceleration and heating due to the heliospheric interface, i.e. velocity of 20 km s^-1 and a temperature of 14 000 K. The resulting line profile in the upwind direction has a mean shift of -25 km s^-1 and a temperature of a bit less than 14 000 K. The line profiles are shown in the solar rest frame.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f07.eps}\end{figure}$ Figure 7: LOS temperature as a function of the upwind angle. The values were obtained for the four orbits from 1999 to 2002. The data from 1999 are shown by crosses, those of 2000 by stars, those of 2001 by squares, and the data of 2002 are shown by triangles. There are no values for angles smaller than 20 $^{\circ }$ or larger than 150 $^{\circ }$ because of contamination by stellar light. The two curves from 1996 (dashed line) and 1997 (dotted line) have been added for comparison. First, the temperature minimum seen previously around 60 $^{\circ }$ seems to have shifted towards lower values. Second, the profiles appear cooler by roughly 1000 K everywhere.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f08.eps}\end{figure}$ Figure 8: Upwind interplanetary spectrum measured by STIS on March, 21, 2001. The geocorona (dash line) is more intense than the IP line (factor of 6) but the two lines are well separated because of the Doppler shift between the H atoms and the Earth. The geocoronal emission has been fitted and removed, leaving a larger uncertainty longward of the interplanetary line.
Open with DEXTER

In the text

$\begin{figure} \par\noindent\includegraphics[width=8cm]{QuemeraisAA5169f09.eps}\end{figure}$ Figure 9: Upwind interplanetary spectrum in the solar rest frame. The diamonds show the data, the thin solid line shows a Voigt function fit to the data, the thick solid line shows the deconvolved spectrum obtained from the Voigt function fit assuming that the LSF is given by the geocoronal profile.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.7cm,angle=90]{QuemeraisAA5169f01.eps}\end{figure}$	Figure 1: full-sky map of the velocity difference between the 1996 map and the 1997 map. The data are shown in ecliptic coordinates (west ecliptic longitude). The blue color in the upwind side shows that the upwind velocity in 1997 is slightly slower (in modulus), by 0.4 km s^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm]{QuemeraisAA5169f08.eps}\end{figure}$	Figure 8: Upwind interplanetary spectrum measured by STIS on March, 21, 2001. The geocorona (dash line) is more intense than the IP line (factor of 6) but the two lines are well separated because of the Doppler shift between the H atoms and the Earth. The geocoronal emission has been fitted and removed, leaving a larger uncertainty longward of the interplanetary line.
Open with DEXTER

$\begin{figure} \par\noindent\includegraphics[width=8cm]{QuemeraisAA5169f09.eps}\end{figure}$	Figure 9: Upwind interplanetary spectrum in the solar rest frame. The diamonds show the data, the thin solid line shows a Voigt function fit to the data, the thick solid line shows the deconvolved spectrum obtained from the Voigt function fit assuming that the LSF is given by the geocoronal profile.
Open with DEXTER