Georgios Vasilopoulos
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    Georgios Vasilopoulos
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      3. To beam or not to beam

      To beam or not to beam


      To beam or not to beam

      Ultra luminous X-ray pulsars are the believed to be the proof that super-Eddington accretion occurs. These systems host highly magnetized Neutron Stars that accrete way above the Eddington limit. A fundamental question is "how much more?". This is not a simple one as one needs to account for the structure of the accretion disk and possible beaming effects. In a series of articles we have tackled this problem and provide insights onto its nature, I will not spoil the answer.

      see relevant publications:

      A Bayesian approach for torque modelling of BeXRB pulsars with application to super-Eddington accretors

      Chandra Probes the X-Ray Variability of M51 ULX-7: Evidence of Propeller Transition and X-Ray Dips on Orbital Periods

      M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

      NGC 300 ULX1: spin evolution, super-Eddington accretion, and outflows

      Investigating ULX accretion flows and cyclotron resonance in NGC 300 ULX1

      NGC 300 ULX1: A test case for accretion torque theory

      The 2019 super-Eddington outburst of RX J0209.6-7427: detection of pulsations and constraints on the magnetic field strength

      ULX spectra revisited: Accreting, highly magnetized neutron stars as the engines of ultraluminous X-ray sources

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      ASTRAPE (funded by H.F.R.I)
      Hunting Be X-ray binary outbursts in the Magellanic Clouds
      X-ray binaries in the Large Magelanic Cloud
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