BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Talks.cam//talks.cam.ac.uk//
X-WR-CALNAME:Talks.cam
BEGIN:VEVENT
SUMMARY:Magnetic fields of neutron stars: simulations and observations - A
 ndrei Igoshev\, Newcastle University
DTSTART:20250612T150000Z
DTEND:20250612T160000Z
UID:TALK233026@talks.cam.ac.uk
CONTACT:Mor Rozner
DESCRIPTION:Neutron stars are the largest and the strongest magnets in the
  Universe. Their typical radius is around 10 km and their magnetic fiel
 ds could reach values of 1e15 G. Structurally\, the outer 1 km shell of 
 a neutron star is its solid crust\, while the inner part is its core. Ma
 gnetic fields shape observational properties of isolated and accreting neu
 tron stars. Strong magnetic fields play the crucial role in explaining tra
 nsient and persistent X-ray emission from Anomalous X-ray Pulsars and Soft
  Gamma Repeaters jointly known as magnetars. Magnetic fields are not const
 ant and expected to evolve over time. In the last years\, a significant pr
 ogress was made in modelling magneto-thermal evolution of neutron star cru
 st. Ohmic decay and Hall evolution explains multiple magnetar properties. 
  In this colloquium\, I summarise the main observational constrains curre
 ntly available on magnetic fields of neutron stars and confront them with 
 state-of-art numerical simulations. I will explain how current and future 
 observations help us to learn more about magnetic field evolution and its 
 structure. I also explain how the neutron star core can be modelled and sh
 ow preliminary results for field evolution in the core.
LOCATION:Hoyle Lecture Theatre\, Institute of Astronomy
END:VEVENT
END:VCALENDAR