BEGIN:VCALENDAR VERSION:2.0 PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN BEGIN:VEVENT SUMMARY:Turbulence in Magnetised Neutron Stars DTSTART:20260423T143000Z DTEND:20260423T160000Z DTSTAMP:20260906T110955Z UID:7927deec-761e-4ea9-85f7-d2d1539ee685 SEQUENCE:1 CREATED:20260421T141058Z DESCRIPTION: The magnetic field configuration in the interior of Neutron S tars is an open problem and may be impacted by the influence of a turbulen t cascade within the star. Turbulent magnetic fields also play a key role in the evolution of Binary Neutron Star (BNS) mergers\, driving outflowing matter and launching ultrarelativistic jets. Modelling turbulent flow wit h numerical simulations either requires incredibly high resolution simulat ions\, or effective models to capture the impact of turbulence on large sc ales. In this talk I will firstly present a series of high resolution simu lations of magnetised isolated neutron stars\, to discuss the impact of th e magnetic field on turbulent flow in the star interior\, and the long ter m evolution of the magnetic field configuration. I will then discuss the i mpact of the end state of this magnetic field configuration on a BNS merge r\, and demonstrate the construction of a subgrid model to effectively inc orporate the impact of turbulence in such simulations. LAST-MODIFIED:20260421T141058Z LOCATION:DF Seminar Room (2-8.3)\, 2nd floor of Physics Building URL:http://df.vps.tecnico.ulisboa.pt/en/events/turbulence-in-magnetised-ne utron-stars/ X-ALT-DESC;FMTTYPE=text/html:

The magnetic field configuration in the interior of Neutron Stars is an open problem and may be impacted by the influence of a turbulent cascade within the star. Turb ulent magnetic fields also play a key role in the evolution of Binary Neut ron Star (BNS) mergers\, driving outflowing matter and launching ultrarela tivistic jets.

Modelling turbulent flow with numerical simulatio ns either requires incredibly high resolution simulations\, or effective m odels to capture the impact of turbulence on large scales. In this talk I will firstly present a series of high resolution simulations of magnetised isolated neutron stars\, to discuss the impact of the magnetic field on t urbulent flow in the star interior\, and the long term evolution of the ma gnetic field configuration.

I will then discuss the impact of th e end state of this magnetic field configuration on a BNS merger\, and dem onstrate the construction of a subgrid model to effectively incorporate th e impact of turbulence in such simulations.

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