[W189] José C. Jiménez: QCD Phase Transitions in the Sky: Twin Stars and their Non-Radial g-modes
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Latin American Webinars on Physics
Nov 11, 2025, 2:48:35 AM11/11/25
to lawphysics
Dear colleagues,
Abstract:Massive ordinary stars (between 8 to 20 solar masses) end their stellar evolution as the so-called neutron stars. They represent the extreme stage of matter before becoming a black hole. Their existence comes from a delicate balance between the Fermi degeneracy pressure of their microscopic degrees of freedom and the gravitational pull. Nevertheless, it is still an open question to calculate the equation of state for these stars through quantum chromodynamics (QCD). In this talk, I will review the fundamental ingredients to study these objects and summarize my recent advancements concerning a specific type of neutron star, the so-called twin stars. If discovered through multimessenger astrophysics, they could provide invaluable information about the nature of the QCD transition. For instance, their non-radial g-modes are sensitive to properties of the hadron-quark transition which in turn might leave unique imprints on upcoming gravitational wave data.
We are excited to invite you to our next webinar on Wednesday, November 12, 15:00 UTC (10:00 am, Bogotá/Chicago). Our guest will be José C. Jiménez (Department of Astrophysics, Brazilian Center for Research in Physics (CBPF), Brazil), who will discuss "QCD Phase Transitions in the Sky: Twin Stars and their Non-Radial g-modes". The abstract can be found below.
Join us via YouTube: https://www.youtube.com/live/XgUAcjtAOew
QCD Phase Transitions in the Sky: Twin Stars and their Non-Radial g-modes
Speaker: José C. Jiménez
Department of Astrophysics, Brazilian Center for Research in Physics (CBPF), Brazil
Host: Joel Jones-PerezDepartment of Astrophysics, Brazilian Center for Research in Physics (CBPF), Brazil
Abstract:Massive ordinary stars (between 8 to 20 solar masses) end their stellar evolution as the so-called neutron stars. They represent the extreme stage of matter before becoming a black hole. Their existence comes from a delicate balance between the Fermi degeneracy pressure of their microscopic degrees of freedom and the gravitational pull. Nevertheless, it is still an open question to calculate the equation of state for these stars through quantum chromodynamics (QCD). In this talk, I will review the fundamental ingredients to study these objects and summarize my recent advancements concerning a specific type of neutron star, the so-called twin stars. If discovered through multimessenger astrophysics, they could provide invaluable information about the nature of the QCD transition. For instance, their non-radial g-modes are sensitive to properties of the hadron-quark transition which in turn might leave unique imprints on upcoming gravitational wave data.
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