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"For the first time, we're really nailing down what the outflow speed is," he says.
Simultaneous measurements by two antennas show similar patterns of scintillation, and the time lag for maximum cross-correlation gives an estimate for the solar wind outflow speed.
Model electron densities are derived from the collisional part of the O VI λ1037.6 Å line and the proton outflow speed is calculated from mass flux conservation along the magnetic field lines.
By the comparison of the outflow speed obtained by interplanetary scintillation measurements with observed pho-tospheric field strength Kojima et al. (2005) have found that the solar wind velocity is better correlated with surface magnetic field strength, divided by the expansion factor, Br,0/f: They claim that Br,0/f is a better index for the speed of solar wind than individual 1/f or Br,0.
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These wind speeds approach those observed over polar coronal holes at solar minimum, but the outflow speeds in these coronal holes between 2 and 3 R⊙ are different.
The outflow speeds for the large equatorial coronal holes observed by UVCS are 3 4 times lower than those in polar coronal holes between 2 and 3 R⊙.
Specifically, we find outflow speeds of Ne7+ ions of about 5 km s−1 and of Mg8+ ions of 15 km s−1 with respect to quiet-Sun (QS) regions.
The enhanced activity of IL resulting from increased cortical DA outflow speeds up the process of inhibition of both PL and CeA (via ITC).
The outflow from the top side of the disc is at super escape speed velocities with the result that the mass outflow is predominantly from the top side of the disc.
Lastly, the outflow fraction of escaping ions that have speeds above the escape speed is varying as presented in Fig. 5 (panels f and l).
Using basic traffic flow and route choice models we investigate how outflow and speed limit control can affect the final equilibrium turning fractions.
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