Table 6: Seasonal ephemerids for spin maxima of BG CMi according to the linear fit $t_E=T_0+P\cdot (E-E_0).$
T₀-2 400 000 P $\phi_5$ E₀

52661.32970(11) 0.010572652 (66) 0.001 722 713

53041.43489 (2) 0.010572451 (28) 0.013 758 665

53390.87981 (9) 0.010572466(116) -0.003 791 717

53105.31448 (6) 0.0105725772(20) 0.020 764 707

**Table 6:** Seasonal ephemerids for spin maxima of BG CMi according to the linear fit $t_E=T_0+P\cdot (E-E_0).$
T₀-2 400 000	P	$\phi_5$	E₀
52661.32970(11)	0.010572652 (66)	0.001	722 713
53041.43489 (2)	0.010572451 (28)	0.013	758 665
53390.87981 (9)	0.010572466(116)	-0.003	791 717
53105.31448 (6)	0.0105725772(20)	0.020	764 707

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and comparison stars
	3 Separation of spin and orbital variability
	4 Color variability with the phase of orbital and spin period
	5 194-minute orbital period
	6 Variability of the spin period
	7 Conclusions
	References