{ "id": "2209.06662", "version": "v1", "published": "2022-09-14T14:16:42.000Z", "updated": "2022-09-14T14:16:42.000Z", "title": "Detection of a quasi-periodic oscillation at $\\sim$40 mHz in Cen X-3 with Insight-HXMT", "authors": [ "Q. Liu", "W. Wang", "X. Chen", "W. Yang", "F. J. Lu", "L. M. Song", "J. L. Qu", "S. Zhang", "S. N. Zhang" ], "comment": "9 pages, MNRAS in press", "categories": [ "astro-ph.HE", "astro-ph.SR" ], "abstract": "We investigated the quasi-periodic oscillation (QPO) features in the accretion-powered X-ray pulsar Cen X-3 observed by Insight-HXMT. For two observations in 2020 when Cen X-3 was in an extremely soft state, the power density spectrum revealed the presence of obvious QPO features at $\\sim$40 mHz with an averaged fractional rms amplitude of $\\sim9\\%$. We study the mHz QPO frequency and rms amplitude over orbital phases, and find that the QPO frequency is $\\sim$33-39 mHz at the orbital phase of 0.1-0.4, increasing to $\\sim$37-43 mHz in the orbital phase of 0.4-0.8, but has no strong dependence on X-ray intensity. We also carried out an energy-dependent QPO analysis, the rms amplitude of the mHz QPOs have a decreasing trend as the energy increases from 2 to 20 keV. In addition, the QPO time-lag analysis shows that the time delay is $\\sim 20$ ms (a hard lag) in the range of $\\sim$5-10 keV, and becomes negative (time lag of $-(20-70)$ ms) above $\\sim 10$ keV. The different QPO theoretical models are summarized and discussed. In the end, we suggest that these energy-dependent timing features as well as the origin of mHz QPOs in Cen X-3 may be ascribed to an instability when the accretion disk is truncated near the corotation radius.", "revisions": [ { "version": "v1", "updated": "2022-09-14T14:16:42.000Z" } ], "analyses": { "keywords": [ "quasi-periodic oscillation", "orbital phase", "insight-hxmt", "energy-dependent qpo analysis", "qpo time-lag analysis" ], "note": { "typesetting": "TeX", "pages": 9, "language": "en", "license": "arXiv", "status": "editable" } } }