Synchrotron Emission From Protostellar Jets

ADRIANA R., RODRÍGUEZ K.; CARLOS CARRASCO-GONZÁLEZ

Morelia

Congreso; Multiple Scale Star Formation; 2017

Instituto de Radioastronomía y Astrofísica, UNAM

Protostellar jets are well known to be dominated by radio emission of thermal electrons. Interestingly, non-thermal emission in some protostellar jets has beenproposed through the detection of negative spectral indices at radio wavelengths. Through the detection of linearly polarized emission in the HH 80-81 protostellar jet(Carrasco-Gonzalez et al. 2010), the nature of the non-thermal emission have been confirmed as synchrotron. This implies that protostellar jets are able to accelerateparticles up to relativistic energies. However, the acceleration mechanism and even the place where particles are accelerated is still unclear.In this work we present results of an observational campaign with the JVLA to study the synchrotron emission from a sample of protostellar jets, and discuss in thecontext of particle acceleration. We analyze high sensitivity multi-frequency data of two representative protostellar jets: HH 80-81, and the Triple Source in Serpens;which are known to be driven by a massive and an intermediate-mass protostar, respectively. We found that the particle acceleration is most probably taken placewhere the jet strongly impacts against the dense ambient medium through Diffusive Shock Acceleration mechanism. In the case of our new observations on HH 80-81,we resolve the jet in a highly collimated component, which also shows signs of particle acceleration through internal shocks.