Table 1:

H fluxes, equivalent widths, and Rossby numbers of the LMXBs displayed in Fig. 5.

Object	EW(H)a					b			Refs.c
	[Å]	[K]	[dex]	[106 erg cm-2 s-1]	[dex]	[days]	[days]	[dex]
A0620-00			4.2			22.7	0.32	-1.85	1, 2
Nova Muscae 1991		d	4.1d			24.6	0.43	-1.74	3,4
Cen X-4e			3.9			24.7	0.63	-1.58	5, 6
Cen X-4f			3.9			24.7	0.63	-1.58	6, 7
Nova Scorpii 1994			3.7			7.6	2.62	-0.60	8, 9, 10

Notes.  ^a Corrected equivalent width of narrow H component of the secondary star. ^b Convective turnover time derived from the equations in Noyes et al. (1984) for dwarfs stars and using the turnover times given in Basri (1987) for subgiant and giant stars. ^c References: (1) González Hernández et al. (2004), (2) McClintock & Remillard (1986), (3) Casares et al. (1997), (4) Remillard et al. (1992), (5) Torres et al. (2002), (6) González Hernández et al. (2005), (7) D'Avanzo et al. (2005), (8) Shahbaz et al. (1999), (9) González Hernández et al. (2008a), (10) van der Hooft et al. (1998). ^d Adopted values according to the effective temperature and surface gravity for the spectral type and orbital period. ^e H equivalent width obtained from Torres et al. (2002). ^fH equivalent width obtained from D'Avanzo et al. (2005).