Research
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2024.09.03
The role of mixing, mass-loss and rotation in stellar evolution
Despite the efforts made in recent decades to obtain more realistic stellar models, considerable uncertainties still remain due to our incomplete knowledge of some complex physical processes that occur within them, such as accretion, convection, mass loss, rotation, to name a few of them. Modeling these processes still relies on empirical calibrations and this has a significant impact on theore...
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2024.08.29
Exploring Stellar Astrophysics and Star-Planet Interactions Through Observational Studies
Photometric and spectroscopic observations of individual stars, binaries, and group of stars in coeval populations offer valuable insights into various stellar characteristics, such as chemical abundance, radial velocity, multiplicity, mass, distance, and age. The chemical abundances provide critical information about the internal physics of stars, the interactions between planets and their hos...
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2024.06.05
Cosmological formation of globular clusters
Cosmological formation of globular cluster
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2024.05.29
A closer look at the building blocks of planetesimals: characterizing the dust content of protoplanetary disks
The dust content of protoplanetary disks plays a crucial role in the planet formation process. The key ingredients are not only the total budget of solid mass and the dust particle size distribution, but also how these are distributed throughout the protoplanetary disk. Characterizing the dust surface density, particle properties, and size distribution within the disk and its substructures is, ...
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2024.05.14
Gravitational radiation from oscillations of ultracompact stars
By analytically solving the Teukolsky gravitational wave equation for the spacetime of an ultracompact star of constant density, we derive exact and simple formulae that completely describe weakly damped oscillations trapped inside such stars. No similar complete analytic solution was known before, despite several attempts to find it. Our solution is cast in terms of the quasi normal modes of o...
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