Neutron Star Normal Modes lsc meeting, Baton Rouge, March 2004 ligo-g040141-00-z b. S. Sathyaprakash and Bernard Schutz


НазваNeutron Star Normal Modes lsc meeting, Baton Rouge, March 2004 ligo-g040141-00-z b. S. Sathyaprakash and Bernard Schutz
Дата конвертації06.06.2013
Розмір519 b.
ТипПрезентации


Neutron Star Normal Modes LSC Meeting, Baton Rouge, March 2004 LIGO-G040141-00-Z

  • B.S. Sathyaprakash and Bernard Schutz

  • Cardiff University and AEI


Neutron Stars

  • Great interest in detecting radiation: physics of such stars is poorly understood.

    • After 35 years we still don’t know what makes pulsars pulse or glitch.
    • Interior properties not understood: equation of state, superfluidity, superconductivity, solid core, source of magnetic field.
    • May not even be neutron stars: could be made of strange matter!


Gravitational Waves from Pulsating Neutron Stars



Stellar Modes

  • G-modes or gravity-modes: buoyancy is the main restoring force

  • P-modes or pressure-modes: main restoring force is the pressure

  • F-mode or fundamental-mode: (surface waves) has an intermediate character of p- and g-mode

  • W-modes: pure space-time modes (only in GR, space-time curvature is the restoring agent)

  • Inertial modes (r-mode) : main restoring force is the Coriolis force (σ~2Ω/3)

  • Superfluid modes: Deviation from chemical equilibrium provides the main restoring agent



Asteroseismology



Asteroseismology



Signal Strengths of Normal Modes

  • Glitch the energy

    • Crab/Vela glitches could deposit energy in normal modes as high as 10–12 Msun
  • Energy in normal modes when a neutron star forms could be as high as 10–8 Msun

  • Normal modes excited due to glitches in Vela will have an amplitude of 10–24

  • It is possible that a newly born NS can be observed in normal modes in our own Galaxy



F- and W- modes in Interferometers



Analysis Plan

  • Make a catalogue of potential sources of normal modes (T. Regimbau)

    • Glitches in radio pulsars, especially Crab and Vela
      • Set up collaborations with Radio, Gamma and X-ray Astronomers to set up time-windows to search for normal modes
    • Accretion onto neutron stars could produce seismic disturbances that could lead to intermittent emission of normal modes.
      • Should coordinate with X-ray/Gamma-ray observations
  • Use existing LAL codes to set up a search pipeline (R. Balasubramanian)

    • Add a piece to carry out triggered searches for NS modes
    • Explore if we can use the existing triggered search codes


Coordinated Searches with Radio Data

  • Why pulsars glitch

    • 3 decades after pulsars are discovered we don’t fully understand why pulsars pulse or glitch
    • Observing normal modes in neutron stars, combined with radio observations, could teach us about glitches, equation-of-state of high-density neutrons (or other matter)
  • Collaborate with Jodrell Bank

    • Jodrell and can provide glitch data on PSR B0833-45, The Vela Pulsar and PSR B0531+21, The Crab Pulsar
    • Jodrell also has unpublished data on pulsars showing peculiarities in pulse periods – could be looked in coincidence with GW data


Benefits from the study

  • Independent (maybe unique) estimation of stellar parameters (mass, radius, EOS, rotation)

  • Understanding of the microphysics in the early stages of NS formation

  • Discovering exotic EOS



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