An accretion model for the anomalous X-ray pulsar 4U 0142+61

TL;DR

This paper introduces an accretion-based model for the X-ray emission of the anomalous X-ray pulsar 4U 0142+61, explaining its spectral features and pulse profiles through fallback disk accretion and radiative shock processes.

Contribution

It presents a novel accretion model involving fan and polar beams to explain the spectral and pulse profile characteristics of 4U 0142+61, contrasting with magnetar-based explanations.

Findings

Successfully fits energy-dependent pulse profiles using beaming functions and gravitational bending.

Explains high polar cap temperatures as due to fan beam heating.

Provides estimates for inclination, magnetic, and shock parameters.

Abstract

We propose that the quiescent emission of AXPs/SGRs is powered by accretion from a fallback disk, requiring magnetic dipole fields in the range 10^{12}-10^{13} G, and that the luminous hard tails of their X-ray spectra are produced by bulk-motion Comptonization in the radiative shock near the bottom of the accretion column. This radiation escapes as a fan beam, which is partly absorbed by the polar cap photosphere, heating it up to relatively high temperatures. The scattered component and the thermal emission from the polar cap form a polar beam. We test our model on the well-studied AXP 4U 0142+61, whose energy-dependent pulse profiles show double peaks, which we ascribe to the fan and polar beams. The temperature of the photosphere (kT~0.4 keV) is explained by the heating effect. The scattered part forms a hard component in the polar beam. We suggest that the observed high temperatures of the polar caps of AXPs/SGRs, compared with other young neutron stars, are due to the heating by the fan beam. Using beaming functions for the fan beam and the polar beam and taking gravitational bending into account, we fit the energy-dependent pulse profiles and obtain the inclination angle and the angle between the spin axis and the magnetic dipole axis, as well as the height of the radiative shock above the stellar surface. We do not explain the high luminosity bursts, which may be produced by the classical magnetar mechanism operating in super-strong multipole fields.