Nustar-FPMA image 3-50 kev in the energy range of all comments. The location of the source, SXP 138, is indicated by a circular area. Credit: arxiv (2025). Doi: 10.48550/arxiv.2504.07219
Using NASA’s atomic spectroscopic telescope, Indian astronomers have visited an X-ray binary system named SXP 138. Results of nustar comments, Published On 26 Marcharxiv The pre-print server gets important information about the behavior of this system.
The X-ray binergies are made of a normal star or a white dwarf that transfers mass to the compact neutron star or black hole. Based on the mass of the fellow star, astronomers divided them into low-distance X-ray baynerizs (LMXBs) and high-mass X-ray binergies (HMXBS).
BE/X-Ray Binergies (BE/XRBS) are the largest subgroups of HMXBS. These systems include stars and, usually, neutron stars, including Pulsar. The comments have found that most of these systems demonstrate weak X-ray emissions that are interrupted by several weeks lasting outbreaks.
SXP 138 Small Magalanic Cloud (SMC) has A BE/XRB with a pulsar with a spin period of 138 seconds. The orbital period of the system was found to be around 125 days. In addition, previous comments have found that SXP 138 also displays a superbital duration of about 1,000 days, which can be caused by stochastic changes in the enhancement disc.
A team of astronomers led by Soham Praveen Sanyashiva of Indian Institute of Science Education and Research Kolkata used SXP 138 and used Nussar Hard X-ray Telescops-FPMA and FPMB on its periodicity.
The comments allowed Sanyashiv’s team to achieve more insight into the spin evolution, nature of the pulse profile and the spectral features of SXP 138.
By analyzing the light curve of SXP 138, it was revealed that the duration of Pulsar Spin increased from 140.69 to 140.85 seconds from August 2016 and August 2017. This suggests that the source is under the propeller regime that exceeds the magnetosferic radius corotation radius, which prevents efficient allocation on the neutron star.
The Pulse profile of SXP 138 displays a complex structure. In most comments, positives with negative generalized intensity and two high peaks with two secondary peaks are distinguished.
Astronomers indicate that high peaks indicate pencil beam emissions from asymmetric hotspots, while two secondary peaks indicate a complex radiation transfer.
The spectral analysis of the SXP 138 found that this requires both blackbody and power-law components.
“With enhanced enhancement, the blackbody temperature increases and the power-law index decreases, possibly internal disc heating and glory due to column formation,” Authors of the paper draw conclusions.
Scientists stated that the future comments of SXP 138 and similar binergies should be focused on keeping an eye on long -term spin variations and investigating spectral state infections. This can further enhance our knowledge about granship processes in such systems.
More information:
Soham Praveen Sanyashiv et al, X-ray binary Pulsar SXP 138: Non-Relative Spin-Down, Pulse and Spectral Features, arxiv (2025). Doi: 10.48550/arxiv.2504.07219
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Citation: Indian astronomers check the behavior of X-ray binary SXP 138 (2025, 18 April)
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