Abstract
We present results from the first multi-epoch X-ray/IR fast-photometry
campaign on the black hole transient GX 339–4, during its 2015
outburst decay. We studied the evolution of the power spectral densities
finding strong differences between the two bands. The X-ray power
spectral density follows standard patterns of evolution, plausibly
reflecting changes in the accretion flow. The IR power spectral density
instead evolves very slowly, with a high-frequency break consistent with
remaining constant at 0.63 ± 0.03 Hz throughout the campaign. We
discuss this result in the context of the currently available models for
the IR emission in black hole transients. While all models will need to
be tested quantitatively against this unexpected constraint, we show
that an IR-emitting relativistic jet that filters out the
short-timescale fluctuations injected from the accretion inflow appears
as the most plausible scenario.
Original language | English (US) |
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Article number | L19 |
Journal | Astrophysical Journal Letters |
Volume | 887 |
Issue number | 1 |
DOIs | |
State | Published - Dec 10 2019 |
Keywords
- Stellar accretion disks
- Jets
- Black Hole physics
- Low-mass X-ray binary stars