Table 2: Photometric amplitudes in the UBVRI and rotational periods of PTTSs in Lindroos systems.

Star
$\Delta U$ $\Delta B$ $\Delta V$ $\Delta R$ $\Delta I$ Period
            SP (B-band) SP (V-band) SL (B-band) SL (V-band)
  (mag) (mag) (mag) (mag) (mag) (days) (days) (days) (days)

(a)
                 
HD 33802 B 0.15 0.08 0.07 0.05   2.8 (99) 2.8 (99) 2.8 (98) 2.8 (99)
HD 40494 B 0.30 0.09 0.07 0.05 - 6.1 (99) 6.4 (99) 6.4 (99) 6.4 (99)
HD 53191 B 0.10 0.05 0.04 0.03 0.03 4.3 (99) 4.4 (99) 4.5 (97) 4.4 (99)
HD 60102 B 0.14 0.12 0.09 0.09 0.09 1.8 (99) 1.9 (99) 1.8 (99) 1.9 (99)
(b)                  
HD 90972 B - 0.05 0.04 0.04 0.04 3.2 (91) 3.2 (91) 3.4 (93) 3.2 (93)
HD 113703 B - 0.09 0.05 0.05 0.04 8.2 (99) 7.7 (98) 8.1 (99) 7.6 (99)
HD 113791 B 0.08 - - - - 3.9 (96)1 - 3.81 (98) -
HD 143939 B - - - 0.07 0.07 3.02(97) 3.23 (85) 3.02 (97) 3.23 (97)
(c)                  
HD 86388 B - - 0.05 - - - 5.3 (85) - 5.7 (<90)
HD 38622 C - 0.10 0.06 0.03 - - - - -
HD 129791 B 0.07 0.03 0.03 0.03 0.02 - - - -
Notes: The sample has been divided in three groups according to the uncertainties of the derived periods: (a) stars with more secure (or probable) periods; (b) stars with less secure (or possible) periods; and (c) stars without periods and stars for which we could not derive a period; 1 obtained with U-band data; 2 obtained with R-band data; 3 obtained with I-band data.

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