# The Exotic Zoo of Millisecond Pulsars in Globular Clusters: a multi-wavelength study

## TL;DR

This study employs multi-wavelength radio and optical observations to discover new millisecond pulsars and their companions in globular clusters, revealing diverse companion types and insights into pulsar evolution.

## Contribution

It introduces an innovative archival radio data stacking method for faint pulsar detection and reports the discovery of new pulsars and companions in globular clusters.

## Key findings

- Discovered three new pulsars in Terzan 5.
- Identified six new companion stars, increasing known companions by ~40%.
- Characterized companion types, including He white dwarfs and a main-sequence star with Hα emission.

## Abstract

This thesis work is focused on the study of millisecond pulsars in globular cluster by using multi-wavelength observations obtained with radio and optical telescopes. Radio observations have been used to search for and timing the pulsars. While classical search routines are based on the analysis of single and long time sequence of data, we present here an alternative method. This method exploits the large amount of available archival radio data to search for very faint pulsars by stacking all the daily power spectra. This method led to the discovery of three new pulsars in the stellar system Terzan 5. Optical observations have been exploited to search for millisecond pulsar optical counterparts, whose emission is totally dominated by the companion stars. Six new companion stars have been discovered, thus increasing by ~40% the total number of companions identified in globular clusters. In particular, four companions turned out to be He white dwarfs, as expected from the canonical formation scenario. One companion turned out to be a very faint and non-degenerate object, showing a strong variability which is likely the result of a strong heating of the stellar side exposed to the pulsar injected flux. Finally, one companion is a main-sequence star which shows a strong H{\alpha} emission likely due to a low-level accretion probably from a residual disk. This system can be located in an early evolutive stage, immediately preceding the reactivation of an already re-accelerated pulsar. Furthermore, we identified the companion star to a transient low-mass X-ray binary. Conclusion are drawn in the final chapter, where the evolution of millisecond pulsars is discussed and possible future developments are suggested.