2026-08-16T05:28:59Zhttps://docta.ucm.es/rest/oai/request

oai:docta.ucm.es:20.500.14352/347392024-06-04T15:22:52Zcom_20.500.14352_14col_20.500.14352_15

Castro Rubio, Elisa De López Santiago, Javier Peri, C. S. Bonito, R. Miceli, M. Albacete Colombo, J. F. Benaglia, P. 2023-06-19T14:54:48Z 2023-06-19T14:54:48Z 2013-10-20 2041-8205 10.1088/2041-8205/776/2/L22 https://hdl.handle.net/20.500.14352/34739 http://dx.doi.org/10.1088/2041-8205/776/2/L22 http://iopscience.iop.org/ Protostellar jets appear at all stages of star formation when the accretion process is still at work. Jets travel at velocities of hundreds of km s^-1, creating strong shocks when interacting with the interstellar medium. Several cases of jets have been detected in X-rays, typically showing soft emission. For the first time, we report evidence of hard X-ray emission possibly related to non-thermal processes not explained by previous models of the post-shock emission predicted in the jet/ambient interaction scenario. HH 80 is located at the south head of the jet associated with the massive protostar IRAS 18162-2048. It shows soft and hard X-ray emission in regions that are spatially separated, with the soft X-ray emission region situated behind the region of hard X-ray emission. We propose a scenario for HH 80 where soft X-ray emission is associated with thermal processes from the interaction of the jet with denser ambient matter and hard X-ray emission is produced by synchrotron radiation at the front shock. eng open access Evidence of non-thermal x-ray emission from HH 80 journal article