All Figures

Figure 1: The computed synchrotron and IC SEDs for jet emission in LS I +61 303 at phases 0.23 (periastron) and 0.5 from radio to TeV energies. The thick lines are SEDs of radiation after attenuation by photon-photon absorption, and the thin lines (above 100 GeV) correspond to the production emission. The data points are adapted from Ray et al. (1997, GBI: white diamonds), Harrison et al. (2000, RXTE: black circles), Chernyakova et al. (2006, INTEGRAL: black squares), Harmon et al. (2004, BATSE: white circles), Schönfelder et al. (2000, COMPTEL: black diamonds), Tavani et al. (1998, EGRET: white triangles), and Albert et al. (2006, MAGIC: black triangles). Radio and X-ray data at periastron and phase 0.5 are available from the literature and shown. The COMPTEL and EGRET data correspond to averaged values for different epochs, and the COMPTEL data is possibly affected by other unnoticed gamma-ray sources within the large COMPTEL detection error box. The observed MAGIC spectrum, being the average one, is dominated by emission at phase 0.5-0.6 and moderately agrees with the computed SED for the same phase. It is worth noting the different SEDs between periastron and phase 0.5, which is due to the different electron SEDs (see Fig. 3) and the strong photon-photon opacities.

Open with DEXTER


In the text

	Figure 2: Top: normalized accretion rate curve. Below: computed light curves of emission in the radio, X-ray, HE and VHE gamma-ray bands.
Open with DEXTER


In the text

Figure 3: The electron SED along the orbit (phases 0: dotted line; 0.23: solid line; 0.5: dashed line; and 0.8: large and small dashed line). Note that for different orbital phases the convective, synchrotron, IC Thomson, and IC KN losses dominate in different energy ranges. The transitions from the non-radiative to the radiative regime are shown with arrows, and the typical radiation energy band is shown for the different electron energies. The normalization of the electron SED also changes along the orbit, depending on the injection and cooling efficiency. Moreover, maximum particle energy changes as well due to losses/acceleration balance.

Open with DEXTER


In the text