The Very Soft X-Ray Spectrum of the Double Pulsar System J0737-3039

Abstract

We present the results of an 80 ks Chandra ACIS-S observation of the double pulsar system J0737-3039. Furthermore, we report on spectral, spatial and timing analysis of the combined X-ray observations performed so far for this system. Fitting a total of ~1100 photons, we show that the X-ray spectrum of the J0737-3039 system is very soft, and not satisfactorily modeled by a simple blackbody or an atmospheric model. However, it is not possible yet to discriminate between a predominantly nonthermal and a predominantly thermal origin for the X-ray emission. Adopting a simple power-law emission model, the photon index (Γ = 3.7 +/- 0.4, 90% confidence interval) and the implied conversion efficiency of the rotational energy of PSR J0737-3039A into X-ray emission (4.1 +/- 0.5 × 10^-4, for a distance to the source of 500 pc) are compatible with the X-ray photons being emitted in the magnetosphere of PSR J0737-3039A. This hypothesis is also supported by the absence of detectable X-ray orbital modulation (up to ~20%, 3 σ) or any X-ray nebular emission and it is in agreement with the high (gtrsim75%) X-ray pulsed fraction of PSR J0737-3039A. A two blackbody or a Comptonized blackbody model also reproduce the data, and the upper limit to the value of the hydrogen column density, N_Hlesssim 1 × 10²⁰ cm^-2, is in better agreement (with respect to the power-law model) with the Galactic N_H in that direction and at that distance. For the two blackbody model the implied emission radii and temperatures are also compatible with those seen in other recycled pulsars, calling for the bulk of the X-ray photons being originated from heated regions at the surface of pulsar A. On the other hand, in the Comptonized blackbody model, the electron temperature seems to be significantly smaller than in other similar objects.