Broadband spectroscopy of the eclipsing high mass X-ray binary 4U 1700-37 with Suzaku

TL;DR

This study uses Suzaku broadband spectroscopy to analyze the high mass X-ray binary 4U 1700-37, revealing flux variability, a cyclotron line indicating magnetic field strength, and wind accretion effects causing flux changes.

Contribution

First broadband spectral analysis of 4U 1700-37 with detection of a cyclotron line and wind accretion effects, providing insights into the source's magnetic field and flux variability.

Findings

Detected a cyclotron absorption line at ~39 keV.

Observed flux variability linked to wind accretion and an accretion wake.

Estimated neutron star magnetic field to be ~3.4×10^12 Gauss.

Abstract

We present the results obtained from broadband spectroscopy of the high mass X-ray binary 4U 1700-37 using data from a Suzaku observation in 2006 September 13-14 covering 0.29-0.72 orbital phase range. The light curves showed significant and rapid variation in source flux during entire observation. We did not find any signature of pulsations in the light curves. However, a quasi-periodic oscillation at ~20 mHz was detected in the power density spectrum of the source. The 1-70 keV spectrum was fitted with various continuum models. However, we found that the partially absorbed high energy cutoff power-law and Negative and Positive power-law with Exponential cutoff (NPEX) models described the source spectrum well. Iron emission lines at 6.4 keV and 7.1 keV were detected in the source spectrum. An absorption like feature at ~39 keV was detected in the residuals while fitting the data with NPEX model. Considering the feature as cyclotron absorption line, the surface magnetic field of the neutron star was estimated to be ~3.4 times 10^12 Gauss. To understand the cause of rapid variation in the source flux, time-resolved spectroscopy was carried out by dividing the observation into 20 narrow segments. The results obtained from the time-resolved spectroscopy are interpreted as the accretion of inhomogeneously distributed matter in the stellar wind of the supergiant companion star as the cause of observed flux variation in 4U 1700-37. A sharp increase in column density after ~0.63 orbital phase indicates the presence of an accretion wake that blocks the continuum and produces the eclipse like low-flux segment.