1. The AE Aqr Multi-wavelength Campaigns Zach Ioannou (SQU) BELISSIMA Conference 18-21 September 2012

2. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012

3. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012

4. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Patterson (1979): Oblique Rotator WKH (1997): Diamagnetic BlobsTerada et al. (2008): Cosmic Ray Accelerator E&H (1996), WHG (1998), Meintjes et al. (2000): Magnetic propeller

5. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 The 2005 Campaign ★ : CBA & AAVSO

6. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 The 2012 Campaign ★ : CBA & AAVSO KVA Vidojevica

7. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 2005 Campaign2012 Campaign 1. C.W. Mauche (LLNL, USA) 2. M. Abada-Simon (Obs. Paris, France)2. Rubén López-Coto (IFAE, Spain) 3. J.-F. Desmus (OAN, Spain)3. Z. Ioannou (SQU, Oman) 4. Z. Ioannou (Crete, Greece)4. M. Bogoslavljevic (AOB, Serbia) 5. M.J. Dulude (SDSU, USA)5. E. Lindfors (Tuorla, Finland) 6. W.F. Welsh (SDSU, USA)6. A. Henden (AAVSO) 7. J.D. Neil (Caltech, USA) 8. N. Sidro (IFAE, Spain) 9. A. Price (AAVSO)

8. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Sep 2 Sep 1 Aug 31 Aug 30 Aug 292005UT Chandra GALEX SWIFT VLA HESS MAGIC SALT Skinakas WHT Laguna The 2005 Campaign

9. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 The 2012 Campaign Observations consist of just a 30 min window per day

10. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Z. Ioannou W. F. Welsh M. J. Dulude M. Abada-Simon J.-F. Desmurs CBA AAVSO A. Price 1530 Å 2270 Å C. W. Mauche J. D. Neill Correlated flares and the 33 s white dwarf spin pulse are observed in the optical through X-ray wavebands The radio light curve is uncorrelated with the other wavebands, implying that the radio flux is due to indepen- dent processes

11. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Spin phase offset variations correspond to a pulse time delay of a sini = 2.17±0.48 s* Phase offset relative to the de Jager et al. spin ephemeris of 0.237 ± 0.010 cycles  X-ray source follows the motion of the white dwarf around the binary center of mass  White dwarf is spinning down at a rate that is slightly less than that predicted by the de Jager et al. (1994) quadratic ephemeris *de Jager (1995) derived a sini = 2.04±0.13 s

12. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Spectrum is reasonably well fit by a Gaussian emission measure distribution with a peak at log T(K) = 7.16, a width σ = 0.48, Fe/Fe  = 0.44, other metals Z/Z  = 0.76, EM = 8 x 10 53 cm -3, and L x = 1 x 10 31 (d/100 pc) 2 erg s -1 Mauche (2009, ApJ, 706, 130)

13. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Radial velocities don’t appear to vary on the white dwarf orbit phase! Radial velocities vary on the white dwarf 33 s spin phase, with two oscillations per cycle (b) composite line profile technique (c) cross-correlation technique (d) boot-strapped cross-correlation technique (a) composite line profile technique  X-ray plasma is trapped on, and rotates with, the white dwarf’s dipolar magnetic field  This is an unexpected result, but differs from the predicted radial velocity of the white dwarf (gray shading) by only 2.3σ

14. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 AE Aqr was observed with the 17 m MAGIC telescope on 4 consecutive nights in 2005 August 29−September 1, and for 24 nights in 2012 at zenith angles of 30 0 −50 0, for a total of >30 hr.  Analysis of each of the nights: no steady excess emission.  Analysis of the sum of the nights: no steady excess emission.  Periodic analysis of each night, using (a) the Rayleigh test on frequencies around the pulse frequency ν 0 and 2ν 0 and (b) phase-folding on frequencies near ν 0 and 2ν 0 : no excess emission.

15. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 Suggesting the possibility that, contrary to previous claims and common belief, AE Aqr is not a TeV gamma-ray source *Lang et al. (1998, Astroparticle Physics, 9, #3, 203) No detections on the sum of the 4 nights from 2005: * F(E>E 0 ) [10 -11 cm -2 s -1 ] Whipple*

16. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 The (pulsating component of the) source of X-rays in AE Aqr follows the motion of the white dwarf around the binary center of mass. Contrary to the conclusions of Itoh et al. (2006), the majority of the plasma in AE Aqr has a density n e >10 11 cm -3, hence its spatial extent is orders of magnitude less than their estimate of 5x10 10 cm. The radial velocity of the X-ray emission lines varies on the white dwarf 33 s spin phase, with two oscillations cycle and an amplitude K ≈ 160 km s -1, broadly consistent with plasma tapped, and rotating with, the white dwarf’s dipolar magnetic field. These results are inconsistent with recent models* of an extended, low- density source of X-rays in AE Aqr, but instead support earlier models in which the dominant source of X-rays is of high density and/or in close proximity to the white dwarf. AE Aqr is not a TeV gamma-ray source. *Meintjes (2000); Itoh et al. (2006); Ikshanov (2006); Venter & Meintjes (2007)

17. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 2005 Campaign: (18) Optical Telescopes (2) γ-ray (1) Radio (3) Satellites 2012 Campaign: (7) Optical Telescopes (1) γ-ray (1) Satellite ★ : CBA & AAVSO ★ : CBA & AAVSO

18. The AE Aqr Multi-wavelength Campaigns Belgrade, 20 th September 2012 We can vastly improve: –Telescope time allocation –Faster data analysis –Focus on science (not data collection) Robotic Telescope Networks –Dynamic (re)scheduling –Reduction Pipelines –Intelligent Systems –Minimize human input