| Issue |
A&A
Volume 575, March 2015
|
|
|---|---|---|
| Article Number | A112 | |
| Number of page(s) | 13 | |
| Section | Astrophysical processes | |
| DOI | https://doi.org/10.1051/0004-6361/201424713 | |
| Published online | 05 March 2015 | |
Online material
Appendix A
Appendix A.1: Maps normalizing through FGeV
In Sect. 3.2, we presented the maps for intermediate adiabatic losses (v = 109 cm s-1) and intermediate magnetic fields (ξ = 10-2, which yields B fields of ~10 G close to the massive star to ~1 G far from it). In this section, we present the maps for the normalization set to reproduce the observed GeV flux for four extreme scenarios, varying between fast/slow adiabatic losses (v = c and v = 108 cm s-1, respectively) and high/low magnetic fields (ξ = 1 – B between 10–102 G – and ξ = 10-4 – B between 0.1–1 G – respectively). The results are shown in Figs. A.1–A.20.
Appendix A.2: Maps normalizing through FMeV
In Sect. 3.2, we presented the maps for intermediate adiabatic losses (v = 109 cm s-1) and intermediate magnetic fields (ξ = 10-2, which yields B fields of ~10 G close to the massive star to ~1 G far from it). In this section, we present the maps for the normalization set to reproduce the observed MeV flux for four extreme scenarios, varying between fast/slow adiabatic losses (v = c and v = 108 cm s-1, respectively) and high/low magnetic fields (ξ = 1 – B between 10–102 G – and ξ = 10-4 – B between 0.1–1 G – respectively). The results are shown in Figs. A.21–A.40.
 |
Fig. A.1
Injection luminosity of relativistic particles in the emitter in the case of fast non-radiative losses and a weak magnetic field. The normalization was set to reproduce an energy flux in the 0.1–10 GeV range equal to 2.8 × 10-10 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.2
As in Fig. A.1 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.3
As in Fig. A.1 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.4
As in Fig. A.1 but showing the integrated energy flux in the 1–30 MeV energy band. |
| Open with DEXTER | |
 |
Fig. A.5
As in Fig. A.1 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.6
Injection luminosity of relativistic particles in the emitter in the case of slow non-radiative losses and a weak magnetic field. The normalization was set to reproduce an energy flux in the 0.1–10 GeV range equal to 2.8 × 10-10 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.7
As in Fig. A.6 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.8
As in Fig. A.6 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.9
As in Fig. A.6 but showing the integrated energy flux in the 1–30 MeV energy band. |
| Open with DEXTER | |
 |
Fig. A.10
As in Fig. A.6 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.11
Injection luminosity of relativistic particles in the emitter in the case of fast non-radiative losses and a strong magnetic field. The normalization was set to reproduce an energy flux in the 0.1–10 GeV range equal to 2.8 × 10-10 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.12
As in Fig. A.11 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.13
As in Fig. A.11 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.14
As in Fig. A.11 but showing the integrated energy flux in the 1–30 MeV energy band. |
| Open with DEXTER | |
 |
Fig. A.15
As in Fig. A.11 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.16
Injection luminosity of relativistic particles in the emitter in the case of slow non-radiative losses and a strong magnetic field. The normalization was set to reproduce an energy flux in the 0.1–10 GeV range equal to 2.8 × 10-10 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.17
As in Fig. A.16 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.18
As in Fig. A.16 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.19
As in Fig. A.16 but showing the integrated energy flux in the 1–30 MeV energy band. |
| Open with DEXTER | |
 |
Fig. A.20
As in Fig. A.16 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.21
Injection luminosity of relativistic particles in the emitter in the case of fast non-radiative losses and a weak magnetic field. The normalization was set to reproduce an energy flux in the 1–30 MeV range equal to 2.6 × 10-9 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.22
As in Fig. A.21 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.23
As in Fig. A.21 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.24
As in Fig. A.21 but showing the integrated energy flux in the 0.1–10 GeV energy band. |
| Open with DEXTER | |
 |
Fig. A.25
As in Fig. A.21 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.26
Injection luminosity of relativistic particles in the emitter in the case of slow non-radiative losses and a weak magnetic field. The normalization was set to reproduce an energy flux in the 1–30 MeV range equal to 2.6 × 10-9 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.27
As in Fig. A.26 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.28
As in Fig. A.26 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.29
As in Fig. A.26 but showing the integrated energy flux in the 0.1–10 GeV energy band. |
| Open with DEXTER | |
 |
Fig. A.30
As in Fig. A.26 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.31
Injection luminosity of relativistic particles in the emitter in the case of fast non-radiative losses and a strong magnetic field. The normalization was set to reproduce an energy flux in the 1–30 MeV range equal to 2.6 × 10-9 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.32
As in Fig. A.31 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.33
As in Fig. A.31 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.34
As in Fig. A.31 but showing the integrated energy flux in the 0.1–10 GeV energy band. |
| Open with DEXTER | |
 |
Fig. A.35
As in Fig. A.31 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
 |
Fig. A.36
Injection luminosity of relativistic particles in the emitter in the case of slow non-radiative losses and a strong magnetic field. The normalization was set to reproduce an energy flux in the 1–30 MeV range equal to 2.6 × 10-9 erg cm-2 s-1. |
| Open with DEXTER | |
 |
Fig. A.37
As in Fig. A.36 but showing the emitter’s size divided by its distance to the star. |
| Open with DEXTER | |
 |
Fig. A.38
As in Fig. A.36 but showing the integrated energy flux in the 0.3–10 keV energy band. |
| Open with DEXTER | |
 |
Fig. A.39
As in Fig. A.36 but showing the integrated energy flux in the 0.1–10 GeV energy band. |
| Open with DEXTER | |
 |
Fig. A.40
As in Fig. A.36 but showing the integrated energy flux in the 0.1–10 TeV energy band. |
| Open with DEXTER | |
© ESO, 2015
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