A Generalized Analytical Model For Thermal And Bulk Comptonization In Accretion-Powered X-Ray Pulsars

TL;DR

This paper introduces a comprehensive analytical model for the X-ray spectra of accretion-powered pulsars, incorporating advanced geometrical and physical features to better match observed spectral variations across different luminosities.

Contribution

The authors develop a generalized, exact series solution-based model that extends previous work by including conical geometry, separate wall and top emissions, and realistic velocity profiles.

Findings

Model successfully simulates spectra of Her X-1 and X Per.

Spectral hardness increase linked to decreased impact velocity in Her X-1.

Model accommodates a wide range of accretion rates.

Abstract

We develop a new theoretical model describing the formation of the radiation spectrum in accretion-powered X-ray pulsars as a result of bulk and thermal Comptonization of photons in the accretion column. The new model extends the previous model developed by the authors in four ways: (1) we utilize a conical rather than cylindrical geometry; (2) the radiation components emitted from the column wall and the column top are computed separately; (3) the model allows for a non-zero impact velocity at the stellar surface; and (4) the velocity profile of the gas merges with Newtonian free-fall far from the star. We show that these extensions allow the new model to simulate sources over a wide range of accretion rates. The model is based on a rigorous mathematical approach in which we obtain an exact series solution for the Green's function describing the reprocessing of monochromatic seed photons. Emergent spectra are then computed by convolving the Green's function with bremsstrahlung, cyclotron, and blackbody photon sources. The range of the new model is demonstrated via applications to the high-luminosity source Her X-1, and the low-luminosity source X Per. The new model suggests that the observed increase in spectral hardness associated with increasing luminosity in Her X-1 may be due to a decrease in the surface impact velocity, which increases the $P$d$V$ work done on the radiation field by the gas.