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The physics of accretion in X-ray binary pulsars - relativistic effects, pulse profiles, and emission properties

Subject Area Astrophysics and Astronomy
Term from 2014 to 2023
Project identifier Deutsche Forschungsgemeinschaft (DFG) - Project number 259364563
 
Final Report Year 2024

Final Report Abstract

Neutron stars can have very strong B-fields. In a binary system, matter can fall from the star onto the neutron star (“accretion”). During accretion a plasma is formed, which couples to the B-field about 1000 km from the neutron star and falls along the B-field lines with ∼30% of the speed of light onto the magnetic poles of the neutron star. On the hard surface of the neutron star an accretion column is formed, a roughly cylinder shaped object with a foot print of < 1 km2 , a height of a few km, and a luminosity of up to a few 10000 solar luminosities are created. We study the physics of the accretion column and of the interaction of the strong B-field of the neutron star with its surroundings. To study individual sources, observations of neutron stars with strong B-fields were performed with X-ray observatories and methods were developed that predict the emission of the acretion column. These include methods to model the shape of the cyclotron resonance line and methods permitting a direct comparison of theoretical models for the emission of the accretion column with observations, including relativistic light bending and models for the emission of the column at very low mass accretion rates, which agree with observations. The polarization predicted by these models agrees with observations with IXPE. The degree of polarization in these observations was larger than predicted by earlier models which ignored the effects of the quantum vacuum.

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