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Is General Relativity correct theory of gravitation?

- Numerous tests of GR exist in weak fields
- Precession of orbit of Mercury
- Bending of star light at solar eclipse
- Gravitational lenses
- Binary Pulsar
- Frame dragging (LAGEOS, Gravity Probe B)
- New Test: Precession of orbit & emission of gravitational waves in OJ287
- Strong field -> Black holes

Unique solution of the timing problem

- Six well timed outburts
- Iterative code
- Astrophysical effects: disk bending, delay of radiation burst

Predictions for 2007 Sept no gravitational radiation: Oct 4

- OJ 287 timing models
- eccentricity
- 0.668 0.668 0.6667 0.655
- precession
- 37.0 36.9 37.0 39.2
- delay
- 0.75 0.70 0.75 1.0
- 1913.01
- 1956.27 1956.18 1956.24 1956.97
- 1963.74 1963.81 1963.69 1964.02
- 1972.97 1972.97 1972.97 1972.97
- 1984.15 1984.15 1984.15 1984.14
- 1994.66 1994.66 1994.65 1994.60
- 1995.85 1995.85 1995.85 1995.88
- 2005.78 2005.78 2005.77 2005.76
- 2007.68 2007.68 2007.69 2007.70
- Sept 5 Sept 5 Sept 9 Sept 13

OJ 287 optical variations

1. Jet wobble, 60 yr cycle + 12 yr steps

2. Tidal variations in jet flow, 12 yr cycle

3. Disk impacts, advance relative to the 12 year cycle due to precession

Complete solution of the problem: timing of 6 outbursts

.

No outburst in hard X-rays; outburst in soft X-rays

RADIO JET ORIENTATION AND THE PRECESSING BINARY BLACK HOLE

MODEL OF OJ287

M.J. VALTONEN, K.WIIK AND T.SAVOLAINEN

Department of Physics and Tuorla Observatory, University of Turku, Finland

Under preparation

The structure of the November 2005 outburst in OJ287 and the precessing binary black hole model

Mauri Valtonen1, Mark Kidger2,3, Harry Lehto4 & Gary Poyner5

After outburst light curve

- 1 time unit = 0.06 yr

Structure the same in 2005 as in 1983, but a factor of two slower

- 3 peak structure

The structure of the November 2005 outburst in OJ287 and the precessing binary black hole model[1]

Mauri Valtonen1,2, Mark Kidger3,4, Harry Lehto1,5 & Gary Poyner6

[1] Prepared in part with observations from the Bradford Robotic Telescope at the Instituto de Astrofísica de Canarias’s Teide Observatory.

2005 & 1983: same total energy

2005: 4 months; 1983: 2 months, 2x brighter

Overall properties of steady accretion rate disks

- Vertical structure

Mach number

These accretion disks are thin.

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