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Importance of Tides for Periastron Precession in Eccentric Neutron Star - White Dwarf Binaries. Niharika Sravan Midwest Relativity Meeting October 27, 2013. Once Upon A Time…. And then came the GW observer. Periastron Precession.

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importance of tides for periastron precession in eccentric neutron star white dwarf binaries

Importance of Tidesfor Periastron Precession in Eccentric Neutron Star - White Dwarf Binaries

Niharika Sravan

Midwest Relativity Meeting

October 27, 2013

periastron precession
Periastron Precession
  • Is driven by a combination of tidal, rotational and general relativistic effects

Companion Star/Satellite

The quadrupolarperiastron precession constant k2is a measure of the WD's central concentration

eccentric neutron star white dwarf binaries
Eccentric Neutron Star - White Dwarf binaries
  • Seen in the field as pulsars orbiting WDs
  • Serve as probes into compact object physics that are:
    • Clean
    • Testable
    • Abundant
tides dominate in 380 myr
Tides dominate in 380 Myr

GR

Rotation

Tides

Total

slide10

0.5 Gyr

13.8 Gyr

slide12

0.5 Gyr

13.8 Gyr

slide13
“Alright, alright!! I get it, tides are important. But how do you expect me to accurately interpret periastron precession rate if I know nothing about the internal structure of the WD?”
conclusions
Conclusions
  • Information about periastron precession rates can be used to place constraints on the properties of compact object binaries
  • Tides can be a significant driver of periastron precession
  • There is a simple relation that connects the WD structure parameters, governing periastron precession, to the WD mass