Abstract We study the timing and spectral properties of Be/X-ray binary pulsar EXO 2030+375 using a Suzaku observation taken on 2012 May 23, during a less intense Type I outburst. Pulsations were clearly detected in the X-ray light curves at a barycentric period of 41.2852 s, which suggest that the pulsar is spinning-up. The pulse profiles were found to be peculiar, e.g. unlike those obtained from the earlier Suzaku observation acquired on 2007 May 14. A single-peaked narrow profile at soft X-rays (0.5–10 keV range) changed to a double-peaked broad profile in the 12–55 keV energy range and again reverted back to a smooth single-peaked profile at hard X-rays (55–70 keV range). The 1.0–100.0 keV broadband spectrum of the pulsar was found to be well described by three continuum models described as (i) a partial covering high energy cut-off power-law model, (ii) a partially absorbed power-law with high-energy exponential rolloff and (iii) a partial covering Negative and Positive power law with EXponential (NPEX) continuum model. Unlike the earlier Suzaku observation during which several low energy emission lines were detected, a weak and narrow Iron Kα emission line at 6.4 keV was only present in the pulsar spectrum during the 2012 May outburst. Non-detection of any absorption like feature in the 1–100 keV energy range supports the claim of the absence of the cyclotron resonance scattering feature in EXO 2030+375 from the earlier Suzaku observation. Pulse-phase resolved spectroscopy revealed the presence of additional dense matter causing the absence of a second peak from the soft X-ray pulse profiles. The details of the results are described in the paper.

Keywords pulsars: individual (EXO 2030+375) — stars: neutron — X-rays: stars

https://doi.org/10.1088/1674–4527/15/4/007