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Niharika Sravan Midwest Relativity Meeting October 27, 2013

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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  1. Importance of Tidesfor Periastron Precession in Eccentric Neutron Star - White Dwarf Binaries Niharika Sravan Midwest Relativity Meeting October 27, 2013

  2. Once Upon A Time…

  3. And then came the GW observer

  4. 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

  5. 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

  6. Is GR enough to place correct constraints on the WD mass? Importance of Tides and rotation in J1141-6545

  7. Tides dominate in 380 Myr GR Rotation Tides Total

  8. Galactic NS-WD binaries

  9. 0.5 Gyr 13.8 Gyr

  10. How bad can NOT accounting for tides be? Our Method

  11. 0.5 Gyr 13.8 Gyr

  12. “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?”

  13. Once again

  14. Facilitating mass extraction: k2RWD5 vs. MWD Use it well.

  15. 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

  16. Questions?

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