Importance of tides for periastron precession in eccentric neutron star white dwarf binaries
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Niharika Sravan Midwest Relativity Meeting October 27, 2013 PowerPoint PPT Presentation


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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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Niharika Sravan Midwest Relativity Meeting October 27, 2013

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Importance of Tidesfor 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

  • 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

  • Seen in the field as pulsars orbiting WDs

  • Serve as probes into compact object physics that are:

    • Clean

    • Testable

    • Abundant


Is GR enough to place correct constraints on the WD mass?

Importance of Tides and rotation in J1141-6545


Tides dominate in 380 Myr

GR

Rotation

Tides

Total


Galactic NS-WD binaries


0.5 Gyr

13.8 Gyr


How bad can NOT accounting for tides be?

Our Method


0.5 Gyr

13.8 Gyr


“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?”


Once again


Facilitating mass extraction: k2RWD5 vs. MWD

Use it well.


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


Questions?


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