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Observations of compact binaries using XMM-Newton. Gavin Ramsay. What is a compact binary?. Two stars orbiting around each other on timescales less than ~few hrs. One star a white dwarf the other a star similar to the Sun but less massive. How compact are they?. The Sun!. - PowerPoint PPT Presentation
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Observations of compact binariesusing XMM-Newton
Gavin Ramsay
What is a compact binary?
Two stars orbiting around each other on timescales less than ~few hrsOne star a white dwarf the other a starsimilar to the Sun but less massive
How compact are they?
The Sun!
A compact binary with 2hr orbital period
Characteristics depend on the magneticfield of the white dwarf
B<10^4G
B~10^6G
B>10^7G
XMM-Newton
XMM-MSSL polar survey
Surprise was that so many were inlow accretion states: ~half of the systems
A survey of 40 strongly magnetic binary systems
Not there!Important input for population synthesis models
Ramsay et al (2004)
EP Dra - an eclipsing polar
EP Dra - accretion dip and eclipse
Ramsay et al (2004)
The X-ray spectra of polars
Long been the subject of greatcontroversy. Standard model suggestsL_soft/Lhard~1/2
Survey suggests that most polars showX-ray spectrum consistent to that predictedby standard model. However….
Ramsay & Cropper (2004)
EU UMa - shows very little hard X-ray flux
Some systems, however, showemission properties not predicted by the standard accretion model. One proposalis that dense blobs of materialare present in the accretionflow which do not generatehard X-rays. Not clear why some systems have blobs whileothers do not. Not related tomagnetic field strength.
Ramsay et al (2004)
B<10^4G
B~10^6G
B>10^7G
XMM-Newton observations of Intermediate Polars
FO Aqr: P_spin=20.9min, Porb=4.9hrs
Evans et al (2004)
FO Aqr: X-ray spectrum
Huge absorption dip due accretion ‘curtain’
Evans et al (2004)
B<10^4G
B~10^6G
B>10^7G
Disc accreting binaries
YZ Cnc: Porb~2.1hrs
Hakala et al (2004)
YZ Cnc: X-ray spectrum
Hakala et al (2004)
Evidence for jets?
Model with no-blue shift Model with blue shift of1200km/s
Hakala et al (2004)
ULTRA-compact binary: Porb<10min
Jupiter
Ultra-compactbinary
RX J1914+24: Porb 569 sec (9.5min)
Ramsay et al (2005)
Models fall into accretion and non-accreting model.
Accreting models predict it wouldspin down over time.
Non-accreting model suggests it would spin-up over time (the electricstar model).
RX J1914+24: spinning up
Ramsay et al (2005)
Spining up at a rate of 6.6x10^-12s/s
Ramsay et al (2005)
What is the electric star model?
Sounds far fetched - but!….
We know it operates on Jupiter
RX J1914+24: X-ray spectrum
Very odd!Ramsay et al (2005)
Both ultra-compacts have been discoveredin X-rays. Search for more!
Programme to search for ultra-compactsystems in XMM-Newton and Chandraarchives.
Have yet to find one but have discoveredlots of flare stars!
Trenholme, Ramsay & Foley (2004)