Table 2.
Main results regarding the radio emission from the modelled stellar BSs.
| System | Radiation type | Lw⊥ [erg s−1] | fNT,e | UB/UNT,e | ηH | Comments |
|---|---|---|---|---|---|---|
| BD+43°3654 | NT | ≈7 × 1036 | 0.013 | ∼4 | < 0.3 | The observed spectral index at ν > 1 GHz implies a NT spectrum. |
| BD+60°2522 | NT | ≈1 × 1036 | 0.04 | ∼1.5 | < 0.15 | The observed spectral index at ν > 1 GHz implies a NT spectrum. |
| G1 | Hybrid/NT | ≈1 × 1035 | 0.03 | ∼2 | 0.1 | The observed flux density at 887.5 MHz cannot be solely thermal and is most likely dominated by NT emission. |
| G3 | NT | ≈2 × 1035 | 0.01 | ∼6 | < 0.1 | The nature of the emission is inconclusive due to uncertainties in Ṁw and the lack of broadband spectral coverage. |
| Thermal | < 0.002 | > 30 | 0.45 | |||
| Vela X-1 | NT | ≈1 × 1035 | 0.013 | ∼5 | < 0.3 | A reduction in the IL is needed to reproduce the Hα surface brightness, and the observed flux density at 887.5 MHz cannot be solely thermal. A NT-dominated spectrum is thus favoured. |
| Thermal | < 0.003 | > 25 | 1 | |||
Notes. Column 3 shows the power injected in the RS by the stellar wind (typically, Lw⊥ ≈ 0.5 − 0.7 Lw). Columns 4–6 are model parameters: the fraction of the injected power that goes into electrons, the magnetic-to-electrons energy density ratio, and the IL width parameter; we fix ηB = 0.2 for all systems. Column 7 summarises our conclusions about the origin of the emission of each source.
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