The XMM-Newton view of radio-quiet and X-ray dim isolated neutron stars

Abstract

(shortened) As part of the guaranteed time, guest observer and calibration programs, XMM-Newton extensively observed a group of six thermally emitting, isolated neutron stars which are neither connected with a supernova remnant nor show pulsed radio emission. Four of the six sources are now well established as X-ray pulsars: The 11.37 s period of RX J0806.4-4123 was confirmed in a second XMM-Newton observation. In the case of the X-ray faintest of the six stars, RX J0420.0-5022, the period marginally indicated in ROSAT data was not seen in the EPIC data, instead a 3.45 s pulse period was clearly detected. Spectral variations with pulse phase were discovered for the known 8.39 s pulsar RX J0720.4-3125 and also RBS1223. For the latter EPIC data revealed a double-peaked pulse profile for a neutron star spin period of 10.31 s. The X-ray continuum spectra of all six objects are consistent with a Planckian energy distribution with black-body temperatures kT between 40 eV and 100 eV. EPIC data of the pulsars RBS1223 and RX J0720.4-3125 revealed a broad absorption feature in their spectra at energies of 100-300 eV and ~260 eV, respectively. The depth of this feature varies with pulse phase and may be caused by cyclotron resonance scattering of protons or heavy ions in a strong magnetic field. In such a picture the inferred field strength exceeds 10^13 Gauss, in the case of RX J0720.4-3125 consistent with the value estimated from its pulse period derivative. A similar absorption feature in the RGS and EPIC spectra of RX J1605.3+3249 was reported recently.