Testing magnetically confined wind shock models for β Cephei using XMM-Newton and Chandra phase-resolved X-ray observations

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Table 4:

The line fluxes measured in the RGS spectrum. Fluxes are in 10^-6 photons cm^-2 s^-1.
Det.	Line ID	$\lambda$	Flux	Error
RGS2	Ne X Ly $\alpha$	12.132	10.6	1.7
RGS2	Ne IX r	13.447	10.4	1.7
RGS2	Ne IX i	13.550	8.8	1.7
RGS2	Ne IX f	13.700	1.6	0.9
RGS2	Fe XVII	15.010	21.7	2.2
RGS2	Fe XVII	15.190	6.1	1.4
RGS2	Fe XVII	15.260	8.9	1.6
RGS2	Fe XVIII+O VIII Ly $\beta$	16.010	6.6	1.9
RGS2	Fe XVII	16.070	3.6	1.9
RGS2	Fe XVII	16.780	17.7	2.0
RGS2	Fe XVII	17.050	20.8	3.1
RGS2	Fe XVII	17.096	18.9	3.0
RGS2	O VII	18.627	6.8	1.5
RGS2	O VIII Ly $\alpha$	18.970	59.4	3.2
RGS1	O VII r	21.600	45.1	3.4
RGS1	O VII i	21.800	41.3	3.2
RGS1	O VII f	22.100	4.8	1.9
RGS2	N VII Ly $\alpha$	24.780	21.2	2.2
RGS2	N VI r	28.790	18.4	2.3
RGS2	N VI i	29.080	17.2	2.3
RGS2	N VI f	29.530	2.4	1.8

Source LaTeX | All tables | In the text

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