X-ray observations and nuclear physics of GW-driven r-modes
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1 X-ray observations and nuclear physics of GW-driven r-modes Wynn Ho University of Southampton, UK Nils Andersson Ian Jones University of Southampton, UK Nathalie Degenaar University of Michigan, USA Bryn Haskell University of Melbourne, Australia Andersson, Jones, WH, 2014, MNRAS, 442, 1786 Haskell, Degenaar, WH, 2012, MNRAS, 424, 93 WH, Andersson, Haskell, 2011, PRL, 107, CompOSE and NewCompStar WG November 2014
2 Possible detection of r-mode oscillation in LMXBs Fluid oscillation in rotating stars with o inertial frequency (whole star variation): = (4/3) s o corotating frequency (hot spot modulation): = (2/3) s Oscillation observed in two LMXBs (Strohmayer & Mahmoodifar 2014a,b) o XTE J during accretion outburst = s ( s = 435 Hz) o 4U during nuclear superburst = s if r-mode ( s = 582 Hz) Owen+ Andersson, Jones, WH, MNRAS, 442, 1786 (2014): o Relativistic corrections to mode frequency (see also Idrisy, Jones+ 2014) o Observed oscillation amplitude ( ) and spin evolution (spin-up) inconsistent with r-mode theory for XTE J (and 4U ?)
3 LMXBs R-mode instability and emission of gravitational waves Fluid oscillation in rotating stars Generically unstable: GW emission drives r-mode growth (Andersson 1998; Friedman & Morsink 1998) Viscosity damps r-mode o shear viscosity at low temperature o bulk viscosity at high temperature R-mode (in)stability criterion: Owen+ Andersson & Kokkotas (2001) t gw ( s ) = t visc ( s, T)
4 Physics of r-mode (in)stability Unstable r-mode (good for GWs) o spin-temperature evolution limit cycle w/ short time in instability window (Levin 1999; Bondarescu et al 2007) o cannot produce high s Stable r-mode (bad for GWs) o crustal physics mode resonance with elastic crust (Levin & Ushomirsky 2001) o high viscosity at high T superfluid-suppressed hyperon bulk viscosity (Haskell & Andersson 2010) but pulsar spin-down vs. observed s = 716 Hz o superfluid mutual friction e - scatter off sf vortices (weak/strong gap) (Lindblom & Mendell 2000; Haskell+ 2009, 2014) extra friction from vortex-fluxtube interaction? o superfluid phonons (Manuel & Tolos 2013; Manuel, Tolos+ 2013) o magnetic field shortens VBL B > G to stabilize (Mendell 2001)
5 Physics of r-mode (in)stability Unstable r-mode (good for GWs) o spin-temperature evolution limit cycle w/ short time in instability window (Levin 1999; Bondarescu et al 2007) o cannot produce high s no crust Stable r-mode (bad for GWs) o crustal physics mode resonance with elastic crust (Levin & Ushomirsky 2001) o high viscosity at high T superfluid-suppressed hyperon bulk viscosity (Haskell & Andersson 2010) but pulsar spin-down vs. observed s = 716 Hz o superfluid mutual friction e - scatter off sf vortices (weak/strong gap) (Lindblom & Mendell 2000; Haskell+ 2009, 2014) extra friction from vortex-fluxtube interaction? o superfluid phonons (Manuel & Tolos 2013; Manuel, Tolos+ 2013) realistic crust rigid crust o magnetic field shortens VBL B > G to stabilize (Mendell 2001)
6 Physics of r-mode (in)stability Unstable r-mode (good for GWs) o spin-temperature evolution limit cycle w/ short time in instability window (Levin 1999; Bondarescu et al 2007) o cannot produce high s Stable r-mode (bad for GWs) o crustal physics mode resonance with elastic crust (Levin & Ushomirsky 2001) o high viscosity at high T superfluid-suppressed hyperon bulk viscosity (Haskell & Andersson 2010) but pulsar spin-down vs. observed s = 716 Hz o superfluid mutual friction e - scatter off sf vortices (weak/strong gap) (Lindblom & Mendell 2000; Haskell+ 2009, 2014) extra friction from vortex-fluxtube interaction? o superfluid phonons (Manuel & Tolos 2013; Manuel, Tolos+ 2013) o magnetic field shortens VBL B > G to stabilize (Mendell 2001)
7 Observations and physics of r-modes RXTE Oscillations (non-spin) observed in NSs LIGO R-mode/GW sources counter to expectations R-mode instability window is uncertain Rich nuclear physics arena o window shape: crust-core transition/elasticity superfluidity (critical temperature, hyperons, mutual friction, phonons) (see, e.g., recent works by Gusakov+) magnetic field (damping and strength) non-linearity and saturation EOS (see Vidana 2012; Wen+2012) exotica (strange matter, quarks) o core temperature estimates: envelope composition thermal conductivity neutrino emission Weber 2005
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