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Zur Helligkeit bei Staubsturm steht da:
6. Dust storm-related brightness excesses
Having fit the dust-free photometry with an empirical model it is now possible to analyze the brightness excess in more detail by differencing dust storm photometry from the model. However, the residuals for photometry that Schmude (2002) obtained during that 2001 storm revealed significantly more scatter on short time scales than would be expected from the RMS values for his dust-free data in Table 2. This suggested that the full empirical model in α, θ, and is not an appropriate comparison for the dust storm data because the surface of the planet is obscured. Therefore the residuals were re-computed for only the α component of the model, which reduced the scatter to levels comparable to the RMS quantities for Schmude's dust-free data.
The top portion of Table 11 lists the statistics for all data taken during large dust storms from 1954 to the present and reveals substantial brightness increases in the V, R, and, I bands, with a peak in R. The average B filter excess is much smaller and the U filter data are too few in number to permit a reliable assessment. Data from the dust storms of 2001 and 2003–2004 are summarized separately in the lower two portions of the table. The residuals for the 2001 event are plotted in Fig. 7 and indicate a very rapid increase in brightness followed by a gradual decline that lasted several months. By contrast, the 2003–2004 storm shown in Fig. 8 seems to have brightened Mars more gradually.
Table 11. Magnitude excess during global dust storms
Code:
Period/filter Data points Residuals to α-only model
All Average Maximum RMS
I 35 -0.111 -0.247 0.144
R 36 -0.151 -0.306 0.185
V 83 -0.098 -0.290 0.130
B 46 -0.038 -0.214 0.104
U 8 -0.106 -0.177 0.125
2001 Max. linear dust fit RMS to linear dust fit
I 28 -0.146 -0.195 0.055
R 29 -0.194 -0.243 0.057
V 43 -0.147 -0.250 0.045
B 22 -0.070 -0.133 0.060
2003–2004 Max. linear dust fit RMS to linear dust fit
V 11 -0.070 -0.083 0.025
Dazu brauch man noch:
Table 1. Specifications of the UBVRI photometric system
Code:
Units are nm U B V R I
Central wavelength 360 440 550 700 900
Full width at half maximum 70 100 90 220 240
Der Planet ist also im visuellen (V) etwa 0,1m heller. Am stärksten ist der Effekt im Rotkanal (0,15m).