The sustained post-outburst brightness of Nova Per 2018, the evolved companion, and the long orbital period

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Table 4.

Properties of the CS to the WD in V392 Per from fitting to Padova isochrones on the 2MASS plane, as a function of E_B − V reddening.

E_B − V	Age	M_CS		L_CS	R_CS	M_WD	a	P
	(Gyr)	(M_⊙)	(K)	(L_⊙)	(R_⊙)	(M_⊙)	(R_⊙)	(days)
0.63	10.0	1.03	4740	13	5.36	0.58	12.58	4.07
						1.10	14.49	4.38
0.72	3.6	1.35	4875	15	5.34	0.61	11.81	3.36
						1.10	13.37	3.61
1.18	1.4	1.92	5915	31	5.31	0.66	11.20	2.70
						1.10	12.39	2.90

Notes. The JHK_S photometry of V392 Per is corrected for the contribution in quiescence of the hot component (cf. red line in Fig. 3). The orbital separation (a) and period (P) are computed assuming that CS fills its Roche lobe (see Sect. 6 for details).

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