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Fast multi-wavelength broad-band and QPO variability in a black hole X-ray binary: accretion flow and/or a jet origin?

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2015

Publication Year

2020-10-22T10:40:14Z

Acceptance in OA@INAF

Fast multi-wavelength broad-band and QPO variability in a black hole X-ray binary: accretion flow and/or a jet origin?

Title

Kalamkar, M.; CASELLA, Piergiorgio; O'Brien, K.; Uttley, P.; Maccarone, T.

Authors

http://hdl.handle.net/20.500.12386/27916

(2)

1

Maithili Kalamkar

Fast multi-wavelength broad-band and QPO

variability in a black hole X-ray binary:

an accretion flow and/or a jet origin?

Rome Astronomical Observatory

P. Casella, P. Uttley, K. O'Brien, T. Maccarone,

F. Vincentelli, M. van der Klis

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2

Emission components of a black hole X-ray binary

Accretion flow Jet

Emission from various components:

Jet

Synchrotron emission: radio through optical-infra-red (OIR) and possibly in X-rays

Hot flow/corona

Comptonized emission: hard X-rays

also suggested to emit in OIR

Accretion disc

Thermal emission: inner disc soft X-rays outer disc to UV & op.

(4)

3

GX 339-4

Jet

Outburst in 2010

Simultaneous observations:

1. RXTE: X-rays 2-60 keV 2. XMM-Newton: X-rays 0.3-10 keV 3. XMM-Newton Optical monitor

U band (344 nm) 3.6 eV V band (543nm) 2.3 eV 4. VLT ISAAC: IR

K band (2.2 μm) 0.5 eV Hardness- Intensity Diagram

In

te

ns

ity

(5)

4

Power density spectra

In

te

ns

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5

Power density spectra

In te ns ity 0.164 +/- 0.003 Hz 0.161 +/- 0.003 Hz 0.080 +/- 0.001 Hz

(7)

6

Power density spectra

0.164 +/- 0.003 Hz 0.161 +/- 0.003 Hz

(8)

7

Cross correlation function

IR lags the X-rays by 111 ms

0.161 +/- 0.003 Hz 0.080 +/- 0.001 Hz

(9)

8

Origin of variable IR emission

(10)

9

Origin of variable IR emission

Intrinsic outer disc emission? Variability time scales are too fast

(11)

10

Origin of variable IR emission

Synchrotron emission from outer hot flow?

Intrinsic outer disc emission? Variability time scales are too fast Reprocessing of variable X-ray Too short CCF delay

emission incident on outer disc? Highly inclined disc and a highly asymmetric CCF required

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11

Origin of variable IR emission

Synchrotron emission from the jet?

Intrinsic outer disc emission? Variability time scales are too fast Reprocessing of variable X-ray Too short CCF delay

emission incident on outer disc? Highly inclined disc and a highly asymmetric CCF required

Synchrotron emission from outer Unlikely hot flow?

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12

Origin of variable IR emission

(14)

13

Origin of the IR QPO

(15)

14

Conclusions

●

First QPO detection in IR band in a black hole X-ray binary

●

The IR and optical QPO are at half the frequency of the X-

ray QPO

●

The variable IR emission (broad band) is most likely jet

emission

●

The IR emission variable on the QPO time scale could be

from Lense-Thirring precession of the hot flow – but this is

difficult to reconcile with the broad band variability

Riferimenti

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