Left:  Solar wind speed, magnetic field strength, and density from the
observing interval shown in Figure 2.  This has been mapped back to
the Sun using the constant velocity approximation.  The horizontal
axis shows time in terms of the day the solar wind left the Sun.
DoY 141 is May 21, 1997 and DoY 154 is June 3, 1997.  The three
intervals, I1, I2, and I3, and the two solid data points in field
strength and density are discussed below.

Right:  Ultraviolet Coronagraph Spectrometer (UVCS) Lyman alpha
intensity from DoY 141-153, in the 9-10 degree latitude range,
during the May 1997 SOHO-Ulysses quadrature: (top) Lyman alpha
intensity at 3.5 solar radii; (bottom) Lyman alpha intensity at
4.5 solar radii.  Values have been averaged over the observing
interval; the 1-sigma error bar is too small to show up on the
scale of this figure.  The intervals marked I1, I2, and I3 are
discussed below.

Results from the May 1997 quadrature:

1. It is straightforward to match up features in the solar wind at
Ulysses at 5.1 AU and at 3.5-4.5 solar radii in the UVCS data.  This
removes virtually any uncertainty resulting from using the constant
velocity approximation to map solar wind back to the Sun during this
period.  The three intervals, I1, I2, and I3, apparently correspond
to the different appearance of the streamer belt shown in Figure 1
and, by inference, to the streamer belt being parallel to the equator
in I1 and I3, and inclined to the equator in I2.

2. The solar wind was unusually smooth during the entire interval.

3. We do not show the data but only note that Doppler dimming of the
O VI 1032/1037 line ratio implies the solar wind speed is less than
100 km/s at 3.5 solar radii, while it exceeds 100 km/s at 4.5 solar
radii.

4. The "forest" of rays on 26 May appears in the Ulysses density
data but not in the flow speed.

5. Assuming the brightness boundary of the streamer is the fast/slow
wind boundary, there is no evidence of mixing or equatorward flow
between 5 solar radii and 5.1 AU at this boundary.

(Suess et al., JGR, 105 (A11), 25033-25051, 2000)