Arpita Misra (Jagiellonian University, Cracow)
Supermassive black hole (SMBH) spin plays a central role in shaping relativistic jets, yet direct measurements of spin and its evolution remain challenging. Radio jets provide an indirect yet powerful probe of SMBH spin dynamics through their morphology, orientation, and temporal behavior. The radio galaxies exhibiting X-shaped or S-shaped jets are key candidates to study the spin evolution as they highlight a dynamic interplay between the jets, the central active region, and the intergalactic medium. In this talk, I will present observational evidence linking the jet properties of winged radio galaxies to the evolving spin of SMBHs, primarily focusing on S-shaped radio galaxies. Using multiwavelength and multi-frequency radio data, I will discuss how features such as jet reorientation, spectral aging, and large-scale morphology in post-merger and merging systems offer insights into changes in the spin axis. These results highlight the role of radio jets as tracers of SMBH spin evolution and demonstrate how detailed radio studies can constrain the physical processes governing black hole growth and feedback across cosmic time.
Daniela Turis-Gallo (Universidad de Valparaiso, Chile)
Massive stars play a fundamental role in stellar evolution, feedback processes, and the chemical enrichment of galaxies. However, determining their fundamental parameters remains challenging because strong rotational effects, such as stellar deformation and gravity darkening, significantly modify their observed spectra. I will present a model-based spectroscopic analysis of rapidly rotating massive stars that consistently accounts for stellar oblateness and gravity darkening. Using synthetic spectra generated with the ZPEKTR code, we derive stellar parameters—in particular, the inclination angle and equatorial rotation velocity—from photospheric lines. I will analyse the intrinsic limitations of the ZPEKTR code as a function of stellar rotation rate, identifying the parameter space in which the models remain reliable and in which systematic uncertainties become significant. I will also show the application of the code to a sample of Be stars observed with high spectral resolution. Our results are compared with independent determinations from the literature, including interferometric measurements, providing a critical assessment of the accuracy of spectroscopic methods.
Juan Pablo Hidalgo (University of Rome)
Large-scale magnetic fields have been observed in about 10% of main-sequence early-type stars. Notably, chemically peculiar Ap/Bp stars can host surface magnetic fields with mean strengths between 200 G and 30 kG. Unlike late-type stars, whose magnetic fields have complex geometries and are likely generated by convective dynamos, the observed magnetic fields of early-type stars have simpler geometries, and are stable over long timescales, with virtually no variability over several decades. Because these stars have thick radiative envelopes and convective cores, surface dynamos are unlikely to account for the observed magnetism. Consequently, the origin of these magnetic fields remains uncertain. In this talk, I will review recent progress in some of the main theories proposed to explain the magnetism in early-type stars, exploring dynamos hosted by their convective cores, and their interaction with fossil fields inherited from earlier evolutionary stages. Furthermore, I will discuss ongoing simulations of pre-main-sequence stellar evolution aimed at constraining the structure and properties of these primordial fields.
Bogumił Pilecki (CAMK, Warsaw)
Dominika Król (Harvard Smithonian CfA)
Maciek Wielgus (Instituto de Astrofísica de Andalucía, IAA-CSIC, Granada, Hiszpania)
Laetitia Gibaud (Department of Physics, University of Białystok)
Samik Mitra (Astrophysics and Relativity Group International Centre for Theoretical Sciences, Bengaluru, India)
