Table 6: Published Blazhko periods from some previous data sets of RR Lyr. If error bars are given in the publication, they are added. We stress that this table is far from exhaustive, but just indicative of the likely change of the star's Blazhko period.
Reference Years $\Delta T$ (d) $P_{\rm B}$ (listed) Comments
Shapley (1916) 1899-1914(1) 5540 40 $P_{\rm B}\simeq 70P_0^{(2)}$
Balász & Detre (1943) 1935-1941 2188 41 $P_{\rm B}\simeq 72.4P_0^{(3)}$
Struve & Blaauw (1948) 1947 42 42 $P_{\rm B}\simeq 75P_0^{(4)}$
Walraven (1949) 1947 201 41(5)  
Fringant (1961)(1) 1949-1956 2500+ 40.8 (1),(6) $P_{\rm B} \simeq 72 P_0$
Preston et al. (1965) 1961-1964 1026 (Ph.), 855 (Sp.)(7) 40.8(8)  
Detre & Szeidl (1973) 1899-1972 25000+ 41(9)  
Belserene (1999) 1993-1994 477 39.2  
Smith et al. (2003) 1996 77 40 ($\pm$ 1)  
This paper 2003-2004 421 38.8 $\pm$ 0.1  
(1) Result also based on older data sets by other observers.
(2) Derived from the variations in time of the median magnitude. Also mention of a longer cycle of 16.5 years.
(3) The authors write that the light curve variations of RR Lyr can most easily be discribed by a superposition of two pulsations with the period P0=0.567 d and P1=0.559 d.
(4) From the variation in the radial velocity curve.
(5) An additional period is mentioned, about three times longer than $P_{\rm B}$.
(6) The author mentions four periods of RR Lyr: P0=0.5668 d, $P_{\rm B}=40.8$ d, $P_3 \simeq 3P_{\rm B}$, and P4of about 10 years.
(7) Simultaneous spectroscopic and photometric data.
(8) Reference to Fringant's (1961) elements.
(9) First mention of RR Lyr's "4-year cycle''. The authors report that during one and the same "4-year cycle'' $P_{\rm B}$ remained constant.

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