@misc{9240944,
  abstract     = {{HD 129590 is a stellar system with a directly imaged debris disk located in the Scorpius–Centaurus association, approximately 420 light years away. With an estimated age of 15 Myr, young systems like HD 129590 have been ideal for studying the development and evolution of exocomets and planetary disks at early epochs of star formation, at a time when such structures are just emerging. Consequently, previous literature has afforded attention to the system's debris disk as part of such efforts. However, in focusing on the debris disk, the internal, as well as orbital, stellar parameters remain uncertain. In this thesis, the properties of the HD 129590 system are investigated in order to shed more light on the stellar components. This is achieved through the analysis of archival high-resolution spectra taken via the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph over different time intervals. Visual inspection of the spectra illustrate that the stellar system under investigation is in fact a binary system composed of two stars. The spectra thus display the characteristics of double-lined spectroscopic binaries. To characterise the orbits of the binary stars, double Voigt profiles are fitted over a selection of lines, whose peak positions enable the extraction of the radial velocities of the stars at different epochs. Over these radial velocity measurements, Keplerian orbits are fitted, thereby extracting the orbital parameters for the two stars. The results reveal a highly eccentric system, with a period of approximately 23 days, and a median mass ratio q=1.001 ± 7%. To characterise the internal properties of the two stars, the pySME software is utilised. Through the software, approximately 30 segments within a roughly 1000 Å spectral region are fit for each star in order to obtain parameters such as effective temperature, surface gravity, metallicity, and projected equatorial radial velocity. The results suggest stars on the boundary between a G-type star and an F-type star, with effective temperatures around 6400 K with uncertainties. Finally, a discussion is had with regards to the limitations of the project, as well as to future work that can be performed to better understand this system.}},
  author       = {{Slaniceanu, Sofia}},
  language     = {{eng}},
  note         = {{Student Paper}},
  title        = {{HD 129590: A Binary System with an Exocomet Belt}},
  year         = {{2026}},
}