BEGIN:VCALENDAR VERSION:2.0 PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN BEGIN:VEVENT SUMMARY:Unified equation of state probing compact stars DTSTART:20250312T170000Z DTEND:20250312T190000Z DTSTAMP:20260916T130801Z UID:5d323077-edf5-4e8b-bf12-43c692dcf136 SEQUENCE:2 CREATED:20250310T120726Z DESCRIPTION:Meeting ID: 971 1964 8836Passcode Zoom (se necessária): 13463 1The equation of state (EoS) of neutron stars plays a crucial role in dete rmining their internal composition and observable properties. In this stud y\, we construct an EoS\, incorporating a 1st order phase transition from hadronic to quark matter using a Maxwell construction\, and apply it for m odelling both static and rotating neutron stars. In the quark matter phase \, we consider the effects of vector repulsion and color superconductivity \, which significantly alter the stiffness of the EoS and the onset of the deconfinement phase transition\, respectively.Our results in the static c ase provide very good agreement with the astrophysical constraints extract ed from the gravitational wave (GW) signal GW170817 and even the subsolar- mass compact object HESS J1731-347. For non-vanishing rotational velocitie s\, we compare our outcomes with a collection of measurements of the most recent millisecond pulsar (MSP) measurements and again find consistency wi th the observational data. Additionally\, we developed a model of accretio n matter onto rotating hybrid stars with finite magnetic. The model predic ts a set of measurable parameters that can be verified by future data.Furt hermore\, we apply an alternative approach for unified treatment of quark- hadron matter\, i.e. the framework of quarkyonic matter. We for the first time introduce the effects of color superconductivity in the quark gluon p lasma to the framework of quarkyonic matter. In upcoming publications\, we will examine the impact of colour superconductivity in quarkyonic matter and compare it to the Maxwell construction of the 1st order phase transiti on. LAST-MODIFIED:20250310T120738Z LOCATION:Sala de Formação Avançada do DF (2-8.11) + Zoom (Formato Híbr ido) URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/unified-equation-of-state- probing-compact-stars/ X-ALT-DESC;FMTTYPE=text/html:

Meeting ID: 971 196 4 8836
Passcode Zoom (se necessária): 134631

The equation of state (EoS) of neutron stars plays a crucial role in de termining their internal composition and observable properties. In this st udy\, we construct an EoS\, incorporating a 1st order phase transition fro m hadronic to quark matter using a Maxwell construction\, and apply it for modelling both static and rotating neutron stars. In the quark matter pha se\, we consider the effects of vector repulsion and color superconductivi ty\, which significantly alter the stiffness of the EoS and the onset of t he deconfinement phase transition\, respectively.

Our results in the static case provide very good agreement with the astrophysical constraints extracted from the gravitational wave (GW) s ignal GW170817 and even the subsolar-mass compact object HESS J1731-347. F or non-vanishing rotational velocities\, we compare our outcomes with a co llection of measurements of the most recent millisecond pulsar (MSP) measu rements and again find consistency with the observational data. Additional ly\, we developed a model of accretion matter onto rotating hybrid stars w ith finite magnetic. The model predicts a set of measurable parameters tha t can be verified by future data.

Furthe rmore\, we apply an alternative approach for unified treatment of quark-ha dron matter\, i.e. the framework of quarkyonic matter. We for the first ti me introduce the effects of color superconductivity in the quark gluon pla sma to the framework of quarkyonic matter. In upcoming publications\, we w ill examine the impact of colour superconductivity in quarkyonic matter an d compare it to the Maxwell construction of the 1st order phase transition .

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