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Table 3

Results of the fits of the X-ray spectra of HD 45314.

tbabs*wind*(apec(2T)+gauss)
Epoch logNwind kTh Norm1 kTs Norm2 Eline EWline d.o.f.
(cm−2) (keV) (cm−5) (keV) (cm−5) (keV) (keV) (10−14 erg cm−2 s−1)

Apr. 2012 0.16 ± 0.05 1.06 387 3.9 15.5 95.3
Apr. 2012 0.27 (fix.) 8.9 10−5 (fix.) 0.18 ± 0.05 1.16 387 4.0 15.2 93.6
Oct. 2014 0.19 ± 0.07 0.99 456 3.1 9.9 52.4
Oct. 2014 0.27 (fix.) 8.9 10−5 (fix.) 0.19 ± 0.06 1.05 456 3.6 9.6 52.1
Mar. 2016 0.86 72 1.8 2.4 8.4

tbabs*wind*(power+gauss)

Epoch logNwind α Norm Eline EWline d.o.f.
(cm−2) (photons keV−1 cm−2 s−1) (keV) (keV) (10−14 erg cm−2 s−1)

Apr. 2012 0.15 ± 0.06 1.10 387 3.9 15.3 98.6
Oct. 2014 0.16 ± 0.06 1.00 456 3.2 9.9 54.0
Mar. 2016 1.02 75 1.6 2.7 6.9

Notes. All fits assume an interstellar neutral hydrogen column density of 1.9 × 1021 cm−2. For the April 2012 (high state) and October 2014 (shell state) observations, two types of thermal models are considered: single temperaturemodels as well as two temperature models where the properties of the cooler component were set to those derived in the March 2016 (low state) observation. The normalization of the apec models corresponds to , where d is the distance of the source (in cm), andne and nH are the electron and hydrogen number densities of the source (in cm−3). The photon index of the power law is labelled α, and the normalization of the power law is given for a photon energy of 1 keV. The soft, medium, and hard energy domains correspond to the 0.5–1.0, 1.0–2.0, and 2.0–10.0 keV bands, respectively. The fluxes in the last three columns correspond to observed values, that is they are not corrected for interstellar absorption.

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