Eclipsing time variations in close binary systems: Planetary hypothesis vs. Applegate mechanism

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Table 1

Summary of relevant system parameters for close binaries with planetary candidates investigated where we use the usual nomenclature and τ is the age of the binary system (see also Sect. 2). Sources for the data are given below.

System	a_bin/R_⊙	P_bin/d	M_sec/M_⊙	R_sec/R_⊙	T_sec/K	L_sec/L_⊙	τ/Gyr	Type	spectral class	Sources

HS 0705+6700	0.81	0.0958	0.134	0.186	2900	0.00219^∗	5^∗∗	Al	sdB+dM	1, 2, 3
HW Vir	0.860	0.117	0.142	0.175	3084	0.003	5^∗∗	Al	sdB+dM	4, 5, 6
NN Ser	0.934	0.130	0.111	0.149	2920	0.00147^∗	2	No	DA01+M4	7, 8, 9
NSVS14256825	0.80	0.110	0.109	0.162	2550	0.000994^∗	5^∗∗	EB	sd0B+dM	3
NY Vir	0.77	0.101	0.15	0.14	3000	0.00142^∗	5^∗∗	Al	sdB+dM	3, 10, 11
HU Aqr	0.69	0.0868	0.18	0.22	3400	0.00580^∗	1^∗	AM	WD+M4V	12, 13, 14
QS Vir	1.27^∗	0.151	0.43	0.42	3100	0.0146^∗	5^∗∗	Al	DA+M2-4	15, 16, 17
RR Cae	1.62^∗	0.304	0.183	0.209	3100	0.00362^∗	4.5^∗	Al	DA7.8+M4	18, 19, 20
UZ For	0.788^∗	0.0879	0.14	0.177	2950	0.00213^∗	1^∗	AM	M4.5	21, 22
DP Leo	0.59^∗	0.0624	0.1	0.134^∗	2710^∗	0.000867^∗	2.5^∗	AM	WD	23, 24
V471 Tau	3.3	0.522^∗	0.93	0.96	5040	0.40	1	Al	K2V+DA	25, 26, 27

RU Cnc	27.76^∗	10.17	1.42	4.83	4940^∗	12.5^∗	3.3^∗	RS	dF9+dG9	23, 28
AW Her	24.86	8.82^∗	1.35	3.0	5110^∗	5.49^∗	4.0^∗	RS	G2IV	23, 28
HR 1099	11.2^∗	2.84	1.3	4.0	4940^∗	8.6^∗	4.5^∗	RS	K2	29, 30, 31, 32
BX Dra	4.06	0.579	2.08	2.13	6980	9.66	0.5^∗	RR	F0IV-V	23, 33
SZ Psc	15.04^∗	3.97	1.62	5.1	5004^∗	14.7^∗	2.1^∗	RS	K1IV+F8V	23, 34, 35, 36

Notes. We denoted calculated values with an asteriks. In case no age estimates are given in the literature, we adopt a canonical age of 5 Gyr, indicated as ^∗∗. The term secondary does not necessarily refer to the lower mass component, rather it refers to the component of the binary for which we pursued the calculations. For RR Cae, DP Leo, and UZ For, we estimated the WD progenitor masses using the fits provided by Meng et al. (2008) assuming solar metallicity. In the case of DP Leo and UZ For, we adopted the main-sequence lifetime of the progenitor plus 0.5 Myr as a rough age estimate. In RR Cae, we added the cooling age of the WD, which is given as t_cool ~ 1Gyr by ref. 18. The abbreviations for the system type are: Al: eclipsing binary of Algol type (detached); EB: eclipsing binary; No: Nova; AM: CV of AM Her type (polar); RR: variable star of RR Lyr type; and RS: variable star of RS CVn type. The horizontal line separates the PCEB systems from other close binaries.

Reference. (1) Beuermann et al. (2012a); (2) Drechsel et al. (2001); (3) Almeida et al. (2012); (4) Beuermann et al. (2012b); (5) Lee et al. (2009); (6) Wood & Saffer (1999); (7) Parsons et al. (2010a); (8) Beuermann et al. (2010); (9) Beuermann et al. (2013); (3) Almeida et al. (2012); (10) Kilkenny et al. (1998); (11) Qian et al. (2012); (12) Schwope et al. (2011); (13) Wittenmyer et al. (2012); (14) Goździewski et al. (2015); (15) O’Donoghue et al. (2003); (16) Parsons et al. (2010b); (17) Drake et al. (2014); (18) Maxted et al. (2007); (19) Gianninas et al. (2011); (20) Zorotovic & Schreiber (2013); (21) Bailey & Cropper (1991); (22) Potter et al. (2011); (23) Pourbaix et al. (2004); (24) Beuermann et al. (2011); (25) O’Brien et al. (2001); (26) Hussain et al. (2006); (27) Hardy et al. (2015); (28) Tian et al. (2009); (29) Fekel (1983); (30) García-Alvarez et al. (2003); (31) Frasca & Lanza (2004, 2005); (32) Gray et al. (2006); (33) Park et al. (2013); (34) Jakate et al. (1976); (35) Popper (1988); (36) Wang et al. (2010) .

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