11
Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy , GAČR 209/12/P740, 202/09/0772, SGS- 01-2013, www.physics.cz

Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

Embed Size (px)

Citation preview

Page 1: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

Observing Orbital Motion in Strongly Curved Spacetime

Institute of Physics, Silesian University in OpavaGabriel Török

CZ.1.07/2.3.00/20.0071 Synergy , GAČR 209/12/P740, 202/09/0772, SGS-01-2013, www.physics.cz

Page 2: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

Observing Orbital Motion in Strongly Curved Spacetime :

Institute of Physics, Silesian University in OpavaGabriel Török

CZ.1.07/2.3.00/20.0071 Synergy , GAČR 209/12/P740, 202/09/0772, SGS-01-2010, www.physics.cz

Page 3: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

Timing signatures of accretion disc inhomogeneities

Institute of Physics, Silesian University in OpavaGabriel Török

CZ.1.07/2.3.00/20.0071 Synergy , GAČR 209/12/P740, 202/09/0772, SGS-01-2013, www.physics.cz

Page 4: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

COLLABORATION:

Pavel Bakala, Didier Barret, Vladimír Karas, Michal Dovčiak, Martin Wildner, Dalibor Wzientek, Marek Abramowicz, Luigi Stella, Eva Šrámková, Kateřina Goluchová, Frederic Vincent, Grzegorz Mazur, Tomáš Pecháček

Page 5: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

Global EmpiricalModel of Variabilityand Spectra (GRS 1915+105, SPL State)

Response Matrices(Detector)

“DATA” Time and Spectral Distributionof Detected Counts

TIMINGANALYSIS

RESULTS

TOTA

L SO

URC

E FL

UX

MO

DEL

+

Comparing different orbital QPO models, RXTE and LOFT

QPO MODEL

Page 6: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

I. Small spots moving along slightly eccentric orbits close ISCO

Page 7: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

I. Small spots moving along slightly eccentric orbits close ISCO

Left: RXTE Right: LOFT

POW

ER

POW

ER

Page 8: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

II. Toy models of double peak QPOs assuming preferred orbits

Page 9: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

II. Toy models of double peak QPOs assuming preferred orbits

Left: RXTE Right: LOFT

POW

ER

Page 10: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

III. Elongated spots with LOFT

[LO

FT Y

ELLO

W B

OO

K]

Page 11: Observing Orbital Motion in Strongly Curved Spacetime Institute of Physics, Silesian University in Opava Gabriel Török CZ.1.07/2.3.00/20.0071 Synergy,

CONCLUSIONS

Ad SMALL SPOTS:The LOFT observations could easily reveal the Keplerian frequency together with its first and second harmonics when the strongest (but still very weak) single signal is around the limits of the RXTE detectability.

Ad ELONGATED SPOTS:The LOFT mission could open a window to observe the epicyclic motion.

Ad SPOT vs. TORUS COMPARISON:We conclude that the ability to recognize the harmonic content of the signal and follow the QPO evolution can help to distinguish between the different proposed physical models.