Radiation-driven winds of hot luminous stars - XVIII. The unreliability of stellar and wind parameter determinations from optical vs. UV spectral analysis of selected central stars of planetary nebulae and the possibility of some CSPNs as single-star supernova Ia progenitors

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Volume 592 (August 2016)

A&A, 592 (2016) A158

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Table A.1

Shock structures in the winds of the central stars of NGC 2392, IC 4593, IC 418, and NGC 6826, determined from fits of the calculated O vi lines to the FUSE observations.

NGC 2392		IC 4593		IC 418		NGC 6826

[L_X] = −6.0^*		[L_X] = −6.3^*		[L_X] = −6.6		[L_X] = −6.4

r/R_∗	T_s(r)	r/R_∗	T_s(r)	r/R_∗	T_s(r)	r/R_∗	T_s(r)

1.20	0.26	1.11	0.05	1.12	0.04	1.09	0.05
1.31	0.35	1.23	0.12	1.32	0.07	1.42	0.14
1.53	0.50	1.38	0.23	1.57	0.13	1.81	0.29
1.75	0.61	1.75	0.51	1.83	0.19	2.20	0.42
2.18	0.76	2.11	0.76	2.38	0.29	3.42	0.68
2.67	0.87	4.18	1.55	3.07	0.38	5.75	0.92
4.29	1.06	5.39	1.77	4.73	0.52	9.34	1.06
8.85	1.23	11.3	2.21	9.27	0.65	18.1	1.19
27.1	1.33	29.1	2.47	27.4	0.76	41.5	1.26
51.4	1.35	52.7	2.55	51.6	0.78	53.2	1.28
75.7	1.36	76.4	2.58	75.8	0.79	76.6	1.29
100.	1.37	100.	2.60	100.	0.80	100.	1.30

Notes. The table lists characteristic values of the radial distributions of the maximum local shock temperatures T_s(r) (in units of 10⁶ K) and the integrated relative X-ray luminosities L_X/L_bol (where [L_X] = log (L_X/L_bol)) emitted by the shock cooling zones embedded in the winds.

^(*)

We note that Herald & Bianchi (2011), based on a less elaborate treatment of shock structures, obtained integrated relative X-ray luminosities L_X/L_bol which for the central stars of NGC 2392 ([L_X] = −4.4) and IC 4593 ([L_X] = −4.8) are almost a factor of 100 higher than our values. (Their parameters have also been determined from fits of the calculated O vi lines to the observations.) However, as pointed out by the authors themselves, their results will certainly be revised by the application of a more sophisticated treatment of X-rays, which they state is an ongoing development.

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