1 / 11

Observing Orbital Motion in Strongly Curved Spacetime

Observing Orbital Motion in Strongly Curved Spacetime. Gabriel Török. Institute of Physics, Silesian University in Opava. CZ.1.07/2.3.00/20.0071 Synergy , GAČR 209/12/P740 , 202/09/0772, SGS-01-201 3, www. physics.cz. Observing Orbital Motion in Strongly Curved Spacetime :.

omar-sexton
Télécharger la présentation

Observing Orbital Motion in Strongly Curved Spacetime

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Observing Orbital Motion in StronglyCurvedSpacetime Gabriel Török Institute ofPhysics, Silesian University in Opava CZ.1.07/2.3.00/20.0071Synergy , GAČR 209/12/P740, 202/09/0772,SGS-01-2013, www.physics.cz

  2. Observing Orbital Motion in StronglyCurvedSpacetime : Gabriel Török Institute ofPhysics, Silesian University in Opava CZ.1.07/2.3.00/20.0071Synergy , GAČR 209/12/P740, 202/09/0772,SGS-01-2010, www.physics.cz

  3. Timingsignaturesofaccretiondiscinhomogeneities Gabriel Török Institute ofPhysics, Silesian University in Opava CZ.1.07/2.3.00/20.0071Synergy , GAČR 209/12/P740, 202/09/0772,SGS-01-2013, www.physics.cz

  4. 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

  5. Comparing different orbital QPO models, RXTE and LOFT Response Matrices (Detector) Global Empirical Model of Variability and Spectra (GRS 1915+105, SPL State) TOTAL SOURCE FLUX MODEL + “DATA” Time and Spectral Distribution of Detected Counts RESULTS QPO MODEL TIMING ANALYSIS

  6. I. Small spots moving along slightly eccentric orbits close ISCO

  7. I. Small spots moving along slightly eccentric orbits close ISCO POWER POWER Left: RXTE Right: LOFT

  8. II. Toymodelsof double peakQPOsassumingpreferredorbits

  9. II. Toymodelsof double peakQPOsassumingpreferredorbits POWER Left: RXTE Right: LOFT

  10. III. Elongatedspotswith LOFT [LOFT YELLOW BOOK]

  11. CONCLUSIONS Ad SMALL SPOTS: The LOFT observationscouldeasily reveal the Keplerian frequency together with its firstand second harmonics when the strongest (but still veryweak) single signal is around the limits of the RXTE detectability. Ad ELONGATED SPOTS: The LOFT missioncould open a window to observetheepicyclicmotion. Ad SPOT vs. TORUS COMPARISON: We conclude that the abilityto recognize the harmonic content of the signal andfollowthe QPO evolutioncan help to distinguish between thedifferentproposedphysicalmodels.

More Related