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

The AE Aqr Multi-wavelength Campaigns

Zach Ioannou(SQU)

BELISSIMA Conference18-21 September 2012


Belgrade, 20th September 2012





Patterson (1979): Oblique Rotator

WKH (1997): Diamagnetic Blobs Terada et al. (2008): Cosmic Ray Accelerator

E&H (1996), WHG (1998), Meintjes et al. (2000): Magnetic propeller



The 2005 Campaign

★:CBA &AAVSO



The 2012 Campaign

★:CBA &AAVSO

KVA

Vidojevica



2005 Campaign 2012 Campaign

1. C.W. Mauche (LLNL, USA) 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)



Sep 2Sep 1Aug 31Aug 30Aug 292005 UT

Chandra

GALEX

SWIFT

VLA

HESS

MAGIC

SALT

Skinakas

WHT

Laguna

The 2005 Campaign



The 2012 Campaign

Observations consist of just a 30 min window per day



Z. IoannouW. F. WelshM. J. Dulude

M. Abada-SimonJ.-F. Desmurs

CBAAAVSOA. Price

1530 Å

2270 Å

C. W. Mauche

C. W. MaucheJ. D. Neill

Correlated flaresand the 33 s white dwarf spin pulseare observed in theoptical through X-ray wavebands

The radio light curveis uncorrelated withthe other wavebands,implying that the radio flux is due to indepen-dent processes



Spin phase offset variations correspond toa 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 whitedwarf around the binary center of mass

White dwarf is spinning down at a rate thatis 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



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 = 8x1053 cm-3, and Lx = 1x1031 (d/100 pc)2 erg s-1

Mauche (2009, ApJ, 706, 130)



Radial velocities don’t appear to vary on thewhite dwarf orbit phase!

Radial velocities vary on the white dwarf 33 sspin 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



• 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 300−500, 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 ν0 and 2ν0 and (b) phase-folding on frequencies near ν0 and 2ν0: no excess emission.



Suggesting the possibility that, contrary to previous claimsand 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)

[10-1

1 c

m-2s-1

]

Whipple*



• 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 plasmain AE Aqr has a density ne>1011 cm-3, hence its spatial extent is orders of magnitude less than their estimate of 5x1010 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)



• 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



•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

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

Documents

s slide

campaign slide

day slide

cba aavso slide

price aavso slide

magnetic propeller slide

cba aavso kva vidojevica

s spin phase