Notes. P_rot is the rotational period. The values displayed here are literature photometric periods, but we assume them to be equal to the rotational periods of the individual stars (Strassmeier 2009), which are assumed to be equal to one another due to tidal locking (Song et al. 2013). P_orb is the orbital period, a is the semi-major axis from the literature and a_Kep is the semi-major axis computed using the masses in Table 2, the orbital period and Kepler’s Third Law: ). For this we of course needed both masses and the orbital period. If one of these was unknown, we indicated this with ‘-’. The Keplerian semi-major axis is then also unknown and indicated with ‘-’. Only a sin (i) and M sin³ (i) were known for BD+334462, explaining the lower limit on a and on a_Kep.

References. (1) (Strassmeier & Rice 2003); (2) (Rosén et al. 2018); (3) (Henry et al. 1995); (4) (Griffin 2009); (5) (Fekel et al. 2002); (6) (Strassmeier et al. 1989); (7) (Halbwachs et al. 2018); (8) (Heckert et al. 1988); (9) (Crampton et al. 1979); (10) (Glebocki & Stawikowski 1995); (11) (Fekel et al. 2005); (12) (Osten et al. 2016); (13) (Montes et al. 1998); (14) (Griffin 1985); (15) (Eker & Doherty 1987); (16) (Conti 1967); (17) (Barrado y Navascues et al. 1998); (18) (Popper 1988); (19) (Montes et al. 1995); (20) (Gary et al. 2012); (21) (Torres & Ribas 2002); (22) (Strassmeier et al. 1999); (23) (Donati et al. 1992); (24) (Berdyugina et al. 1998); (25) (Frasca et al. 2006); (26) (Padmakar et al. 2000); (27) (Griffin et al. 2006).