Accretion geometry and spectral evolution in 1A 1118-61: a comparison of the 2009 and 2026 outbursts
Abstract
We present a detailed spectro-temporal study of the Be X-ray binary pulsar 1A 1118-61 during its brightest recorded outburst in 2026, using Swift and NuSTAR observations, and compare its properties with the 2009 outburst. Coherent pulsations at 400 s are detected throughout the outburst, with pulse profiles evolving strongly with energy and luminosity, indicating changes in emission geometry. A transient quasi-periodic oscillation (QPO) at 0.11 Hz is observed during the rising phase. The luminosity dependence of the QPO frequency during the current and previous outbursts suggests an origin associated with instabilities near the magnetospheric radius. The broadband spectra are well described by thermal Comptonization and show clear spectral hardening at higher luminosities. A cyclotron line is detected in the two NuSTAR observations, with its energy remaining nearly constant despite a factor of 25 change in luminosity. Long-term monitoring reveals that the 2026 outburst is systematically harder and brighter, suggesting significant difference in the accretion structure and emission regions between the two outbursts.
Turn this paper into a full lesson
ArcXiv compiles a staged curriculum from this paper: 8-12 lessons across beginner → advanced, synthesised section guides, visuals, flashcards, a quiz, exercises, and on-demand deep dives per section. Grounded in the abstract, never invented.