Search

There are several types of Galactic sources that can potentially accelerate charged particles up to GeV and TeV energies. These accelerated particles can produce Very High Energy (VHE, E >100 GeV) γ-ray emission through different processes like for example inverse Compton scattering of ambient photon fields by accelerated electrons. We present here the results of our observations of the source class of γ-ray binaries and the subclass of binary systems known as novae with the MAGIC telescopes. The focus lies on the five sources: nova V339 Del, AE Aquarii, SS 433, MWC656 and LS I +61°303. The binary system LS I +61°303 was observed in a long-term monitoring campaign for 8 years. We show the newest results on our search for superorbital variability also in context with contemporaneous optical observations. MWC656 is a unique detected high-mass X-ray binary system, since it is up to now the only one known composed of a Be star and a black hole. Furthermore, we present the observations of the only super-critical accretion system known in our galaxy: SS 433. Finally, results of our multiwavelength observation campaign regarding the cataclysmic variable AE Aquarii and the results of the follow-up observations of the nova V339 Del will be discussed in these proceedings. [ABSTRACT FROM AUTHOR]

A few binary systems display High Energy (100 MeV-100 GeV) and/or Very High Energy (>= 100 GeV) gamma-ray emission. These systems also display non-thermal radio emission+that can be resolved with long-baseline radio interferometers, revealing the presence of outflows. It is expected that at very low frequencies the synchrotron radio emission covers larger angular scales than has been reported up to now. Here we present preliminary results of the first deep radio observations of the gamma-ray binary LS I +61 303 with LOFAR, which is sensitive to extended structures on arcsecond to arcminute scales. [ABSTRACT FROM AUTHOR]

Gamma-ray binary systems are still a sparsely populated source class. Although the individual gamma-ray binaries share some common features, it is not possible to explain their emission mechanisms in a common framework yet. We present the highlights from our MAGIC observations of the best studied northern binary system, LS I +61°303, revealing its complex emission behavior. Furthermore we present observations of the binary HESS J0632+057 which MAGIC observed during an X-ray outburst in 2011. We compare these binary systems, and discuss common features as well as possible differences between them. [ABSTRACT FROM AUTHOR]

LS I+61°303 is one of the best studied gamma ray binaries. Discovered as an emitter of variable TeV fluxes with the MAGIC telescope and studied in more detail later by MAGIC and VERITAS. Here we show the up to now largest data sample recorded by the MAGIC telescope and present the proof of a periodic nature of the variable flux at TeV energies. We furthermore give an account of the variabilities on different timescales and the spectral behavior in different orbital stages of the compact object. In addition we will show hints for a correlation between the TeV emission and the emission in the X-ray band. [ABSTRACT FROM AUTHOR]

LS I +61 303 is one of the most studied X-ray binary systems because of its two peculiarities: On the one hand being the probable counterpart of the variable gamma ray source 2CG 135+01 and on the other hand being a periodic radio source. The recent discovery of a radio emitting jet extending ca. 200 AU at both sides of a central core in all evidence has shown the occurrence of accretion/ejection processes in this system. However, the radio outbursts do not occur at periastron passage, where the accretion is at its maximum, but several days later. In addition, when the gamma-ray emission of 2CG 135+01 is examined along the orbital phase of LS I +61 303 one sees that this emission seems to peak at periastron passage. Here in detail we analyse the trend of the gamma-ray data versus orbital phase and discuss the delay between peaks at gamma-rays and in the radio band within the framework of a two-peak accretion/ejection model proposed by Taylor et al. and further developed by Martí & Paredes. © 2005 American Institute of Physics [ABSTRACT FROM AUTHOR]