Comprehensive analysis of AstroSat data shows a sign change in QPO time lags at ~2 Hz for high-inclination sources, consistent with a transition from elongated jet-like to compact corona.
A possible interpretation for the apparent differences in LFQPO types in microquasars
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abstract
In most microquasars, low-frequency quasi-periodic oscillations (LFQPO) have been classified into three types (A, B and C depending on the peak distribution in the PDS and the shape of the noise) but no explanation has been proposed yet. The accretion-ejection instability (AEI) was presented in 1999 as a possible explanation for the fast varying LFQPO that occur most often. Here we look at a possible generalization to explain the characteristics of the other two LFQPO types. It was recently shown that when the disk approaches its last stable orbit, the AEI is markedly affected by relativistic effects. We focus on the characteristics of the LFQPO that would result from the relativistic AEI and compare them with the different LFQPO types. The effects of relativity on the AEI seem to be able to explain most of the characteristics of the three types of LFQPO within one formalism.
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astro-ph.HE 1years
2026 1verdicts
UNVERDICTED 1representative citing papers
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Understanding corona and disk evolution in black hole X-ray binaries through a comprehensive study of their broadband variability and QPO characteristics
Comprehensive analysis of AstroSat data shows a sign change in QPO time lags at ~2 Hz for high-inclination sources, consistent with a transition from elongated jet-like to compact corona.