Fitting XMM-Newton observations of the AXP 1RXS J170849.0−400910 with four magnetar surface emission models, and predictions for X-ray polarization observations with IXPE

Abstract

Context. Phase-resolved spectral and spectropolarimetric X-ray observations of magnetars present us with the opportunity to test models of the origin of the X-ray emission from these objects, and to constrain the properties of the neutron star surface and atmosphere. Aims. Our first aim is to use archival XMM-Newton observations of the magnetar 1RXS J170849.0−400910 to ascertain how well four emission models describe the phase-resolved XMM-Newton energy spectra. Our second aim is to evaluate the scientific potential of future spectropolarimetric observations of 1RXS J170849.0−400910 with the Imaging X-ray Polarimetry Explorer (IXPE) scheduled for launch in late 2021. The most salient questions are whether IXPE is able to distinguish between the different emission models, and whether IXPE can unambiguously detect the signatures of quantum electrodynamics (QED) effects in strong magnetic fields. Methods. We used numerical radiation transport calculations for a large number of different system parameters to predict the X-ray flux and polarization energy spectra of the source 1RXS J170849.0−400910. Based on the numerical results, we developed a new model to fit phase-resolved and phase-averaged X-ray spectral (i.e., XMM-Newton and IXPE) and spectropolarimetric (IXPE) data. In order to test the sensitivity of IXPE to strong-field QED effects, we fit a simulated IXPE observation with two versions of the model, i.e., with and without QED effects accounted for. Results. The fixed-ions condensed surface model gives the best description of the phase-resolved XMM-Newton spectra, followed by the blackbody and free-ions condensed surface models. The magnetized atmosphere model gives a poor description of the data and seems to be largely excluded. Simulations show that the IXPE observations of sources such as 1RXS J170849.0−400910 will allow us to cleanly distinguish between high-polarization (blackbody, magnetized atmosphere) and low-polarization (condensed surface) models. If the blackbody or magnetized atmosphere models apply, IXPE can easily prove QED effects based on ∼200 ksec observations as studied here; longer IXPE observation times will be needed for a clear detection in the case of the condensed surface models. Conclusions. The XMM-Newton data have such a good signal-to-noise ratio that they reveal some limitations of the theoretical models. Notwithstanding this caveat, the fits clearly favor the fixed-ions condensed surface and blackbody models over the free-ions condensed surface and magnetized atmosphere models. The IXPE polarization information will greatly help us to figure out how to improve the models. The first detection of strong-field QED effects in the signal from astrophysical sources seems possible if an adequate amount of time is dedicated to the observations.

A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910

“…The value of the period derivative, if interpreted as due to a rotating dipole in vacuum, yields a dipole magnetic field strength of ∼4-5 × 10 14 G. The source presents an erratic timing behavior, characterized by frequent glitching activity that interrupts periods of steady spin-down (Dib & Kaspi 2014). The X-ray spectrum has been fitted with an absorbed BB+PL model, with (slightly variable) photon index Γ ∼ 2.6, and BB temperature kT ∼ 0.45 keV (Rea et al 2003(Rea et al , 2007Krawczynski et al 2022). The source is radio-quiet.…”

X-ray spectra and polarization from magnetar candidates

“…This makes the external field non-potential, requiring that charged particles flow along the closed field lines to sustain the twist. Although it is more likely that the twist involves a small bundle of external field lines [66], with both electrons and positrons contributing to the magnetospheric currents [20], here we resort to a simplified model with a globallytwisted dipole field and currents made by electrons and ions lifted from the stellar surface, which nevertheless proved capable to explain the available spectral observations [21,67]. Under these assumptions, the polar components of the external field, (B r , B θ , B ϕ ), with θ and ϕ the magnetic colatitude and azimuth, respectively, can be written as [19,22,68]…”

X-ray Polarization from Magnetar Sources

“…This makes the external field non-potential, requiring that charged particles flow along the closed field lines to sustain the twist. Although it is more likely that the twist involves a small bundle of external field lines [66], with both electrons and positrons contributing to the magnetospheric currents [20], here we resort to a simplified model with a globally twisted dipole field and currents made by electrons and ions lifted from the stellar surface, which nevertheless prove capable to explain the available spectral observations [21,67]. Under these assumptions, the polar components of the external field, (B r , B θ , B ϕ ), with θ and ϕ the magnetic colatitude and azimuth, respectively, can be written as [19,22,68,69]…”