Connections between the cycle-to-cycle light curve and O−C variations of non-Blazhko RR Lyrae stars

Open Access

Table 1.

Kepler non-Blazhko RRab stars.

Name	P₀	σ_e	σ_η	p^AIC	p^BIC	Remarks
	(d)	(×10⁻⁵ d)	(×10⁻⁵ d)
V839 Cyg	0.4337742	3.06	0.60	0.74	0.94
V368 Lyr	0.4564859	4.10	1.04	0.73	0.96
V715 Cyg	0.4707059	5.32	0.98	0.85	0.50	M4
KIC 6100702	0.4881452	6.93	0.63	0.73	0.95	(f₁)
V349 Lyr	0.5070742	7.15	1.61	0.66	0.94
V782 Cyg	0.5236375	7.81	1.14	0.73	0.96
FN Lyr^*	0.5273986	3.32	1.47	0.73	0.96	(f₁)
KIC 9658012	0.533195	9.29	1.93	0.73	0.93	f₂
V784 Cyg	0.5340947	7.65	1.06	0.73	0.96
V2470 Cyg	0.5485897	6.51	0.94	0.73	0.96	f₁, aRRd?
KIC 9717032	0.556908	6.03	1.65	0.73	0.33	M4
V1107 Cyg	0.5657795	6.34	1.48	0.73	0.96
V894 Cyg	0.5713865	6.95	2.63	0.74	0.94	f₂
V1510 Cyg^*	0.5811426	3.98	3.37	0.69	0.95	f₂
NQ Lyr	0.5877889	5.12	2.05	0.73	0.96	f₁, (f₂), aRRd?
NR Lyr^*	0.6820268	7.41	2.36	0.73	0.95	(f₁)
KIC 7030715	0.6836125	7.08	2.22	0.73	0.95
AW Dra	0.6872186	4.92	4.42	0.63	0.92

Notes. Columns of the table indicate (in order) the names and pulsation periods, P₀, of the analysed stars; the fitted σ_e and σ_η parameters of the best statistical model and their probabilities, p^AIC and p^BIC, using the AIC and BIC, respectively. From the O−C data of the stars marked with an asterisk, one or two significant short-period signals were pre-whitened. Finally, f₁ and f₂ are the additional frequencies published by Benkő et al. (2019), identified with the frequencies of the first and second radial overtones.

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