Table 4: Impact of the stellar variability on the integrated number of detections expected for COROT. At the timescale of transits, the solar variability as estimated from SOHO data is $\simeq $50 ppm rms. The crowding effect (Sect. 5.2) is expected to remove $\approx $$10\%$from the detections quoted here.
$R_{\rm P}$ solar var. solar var. solar var.
(in $R_\oplus $) $\times 1$ ${\times 10}$ ${\times 50}$
1.0 6 2 0
1.25 18 4 0
1.5 37 10 0
2.0 95 32 2
3.0 240 112 12
5.0 367 289 73
10.0 382 377 274


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