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.

Breve CV della Dr.ssa Arianna Miraval Zanon:

Laureata in Astronomia nel 2017 all'Università di Padova con una tesi osservativa svolta presso l'Osservatorio di Cagliari analizzando dati del Sardinia Radio Telescope e del radio telescopio di Parkes. Ha ottenuto il suo dottorato presso l'Università dell'Insubria, lavorando presso l'Osservatorio di Merate con la supervisione del Dr Sergio Campana e del Dr Paolo D'Avanzo. Si è poi trasferita all'Osservatorio di Roma nel gruppo di alte energie per il suo primo postdoc. Si è specializzata nello studio di sistemi binari con pulsar al millisecondo in banda X, UV, ottica e radio.