Millisecond pulsars are known to be the fastest spinning compact stars and are often found in close binary systems. They are among the most efficient particle accelerators and natural laboratories of fundamental physics. During their evolution, they appear as radio pulsars powered by the rotation of the neutron star magnetic field or as X-ray pulsars powered by the accretion of mass, transferred by a companion star. I will describe the multi-wavelength signatures appearing during the evolution of binary millisecond pulsars, from the accretion state to the radio pulsar state. I will then present the recent observational campaign of the radio millisecond pulsar PSR J1048+2339 performed with Very Large Telescope, Sardinia Radio Telescope, Low-Frequency Array, Galileo telescope, and Swift satellite. The multi-wavelength campaign was aimed at unveiling the physical origin of the double-peaked emission lines in the optical spectra and mapping the distribution of the material in the system. The Doppler map of the Hα emission line revealed a significant emission close to the inner Lagrangian point extending along the free-fall trajectory of the gas. This extended structure is the first direct evidence of an intra-binary shock emission caused by the pulsar wind interacting with the ablated material from the donor.

Brief CV of Dr. Arianna Miraval Zanon:

She got her degree in Astronomy in 2017 at the Padoa University with an observational thesis made at the Osservatorio Astronomico di Cagliari where she analysed data taken with the Sardinia Radio Telescope and the Parkes radio telescope.She got her PhD at the Università dell'Insubria, working at Osservatorio di Merate under the supervision of Dr. Sergio Campana and Dr. Paolo D'Avanzo. For her first postdoc she moved to Osservatorio di Roma to work in the high energies group. She is specialized in the studies of binary systems with millisecond pulsar in X, UV, optical and radio bands.