X-ray bounds on cooling, composition, and magnetic field of the Cassiopeia A neutron star and young central compact objects
Wynn C. G. Ho, Yue Zhao, C. O. Heinke, D. L. Kaplan, P. S. Shternin, M J P Wijngaarden
Abstract
ABSTRACT We present analysis of multiple Chandra and XMM–Newton spectra, separated by 9–19 yr, of four of the youngest central compact objects (CCOs) with ages <2500 yr: CXOU J232327.9+584842 (Cassiopeia A), CXOU J160103.1−513353 (G330.2+1.0), 1WGA J1713.4−3949 (G347.3−0.5), and XMMU J172054.5−372652 (G350.1−0.3). By fitting these spectra with thermal models, we attempt to constrain each CCO’s long-term cooling rate, composition, and magnetic field. For the CCO in Cassiopeia A, 14 measurements over 19 yr indicate a decreasing temperature at a 10-yr rate of 2.2 ± 0.2 or 2.8 ± 0.3 per cent (1σ error) for a constant or changing X-ray absorption, respectively. We obtain cooling rate upper limits of 17 per cent for CXOU J160103.1−513353 and 6 per cent for XMMU J172054.5−372652. For the oldest CCO, 1WGA J1713.4−3949, its temperature seems to have increased by 4 ± 2 per cent over a 10-yr period. Assuming each CCO’s preferred distance and an emission area that is a large fraction of the total stellar surface, a non-magnetic carbon atmosphere spectrum is a good fit to spectra of all four CCOs. If distances are larger and emission areas are somewhat smaller, then equally good spectral fits are obtained using a hydrogen atmosphere with B ≤ 7 × 1010 G or B ≥ 1012 G for CXOU J160103.1−513353 and B ≤ 1010 G or B ≥ 1012 G for XMMU J172054.5−372652 and non-magnetic hydrogen atmosphere for 1WGA J1713.4−3949. In a unified picture of CCO evolution, our results suggest most CCOs, and hence a sizable fraction of young neutron stars, have a surface magnetic field that is low early in their life but builds up over several thousand years.