Chandra high-resolution spectra of Apep Plume: Exploring the colliding-wind picture in X-rays

Home

All issues

Volume 693 (January 2025)

A&A, 693 (2025) A266

Full HTML

Open Access

Table 2.

CSW spectral fit results.

	β = 0.6
χ²/d.o.f.	240.36/343
Ṁ_s (mass-loss reduction)	0.42
Mg	0.28 $_{- 0.08}^{+ 0.08}$ $^{+0.08}_{-0.08}$
Si	0.68 $_{- 0.10}^{+ 0.10}$ $^{+0.10}_{-0.10}$
S	1.81 $_{- 0.41}^{+ 0.42}$ $^{+0.42}_{-0.41}$
Fe	0.87 $_{- 0.27}^{+ 0.28}$ $^{+0.28}_{-0.27}$
F_X (10⁻¹² ergs cm⁻² s⁻¹)	8.13 (35.5)
log L_X (ergs s⁻¹)	34.39

Notes. Results from the best CSW model fits to the HETG X-ray spectra of Apep Plume with partial electron heating at the shock fronts (β = T_e/T). The listed quantities are the mass-loss scaling factor (Ṁ_s), the chemical abundances, the observed X-ray flux (F_X; followed in parentheses by the unabsorbed X-ray flux), and the logarithm of the X-ray luminosity (log L_X) for the adopted distance of 2.4 kpc to Apep Plume. The last two quantities are in the 0.5−10 keV energy range. Errors are 1σ errors from the fit.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.