LIGO- G050143-00-Z March 23, LLO 1 The pulsar upper limits are already interesting! Ben Owen.

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Presentation transcript:

LIGO- G Z March 23, LLO 1 The pulsar upper limits are already interesting! Ben Owen

LIGO- G Z March 23, LLO 2 How bumpy can neutron stars be? Ellipticity  = (I xx – I yy )/I zz ~ Q 22 /I zz Elastic deformations »Solid matter folded, spindled, and mutilated »Max determined by breaking strain, shear modulus »Traditional answer:  max ~ few x (LIGO-S1 PRD 2004) »New crazy answer:  max ~ few x (Owen astro-ph/ ) »New not-so-crazy answer:  max ~ (Owen astro-ph/ ) Hydromagnetic deformations »Accreting matter (maybe not solid) bottled by magnetic field »Max determined by field strength, matter conductivity (flow-thru) »New answer:  max ~ (Melatos & Payne astro-ph/ )

LIGO- G Z March 23, LLO 3 Elastic deformations Solid crust (all stars) »Ushomirsky et al MNRAS (2000) »Neutron-rich nuclei »Conservative physics Solid core (hybrid star) »Glendenning PRD (1992) »Gradual phase transition »(-) quark droplets in (+) baryonic background »Up to 8km solid core »Not-so-crazy physics All-solid (strange quark) star »Xu ApJL (2003) »s quark clustering »Crazy physics

LIGO- G Z March 23, LLO 4 Hydromagnetic deformations Melatos & Phinney PASP (2000) Accreting ms pulsars only Accreted matter funnels towards magnetic pole Matter crosses field lines slowly (Ohmic diffusion) Depends on conductivity of matter at low density Field lines hold up mountain that would collapse under its own weight

LIGO- G Z March 23, LLO 5 Good news for searches S2 known pulsars »9 pulsars  < few x (solid strange star) – mildly interesting »(These have no competing spindown upper limit) S5 known pulsars »(Extrapolating SRD sensitivity and 1yr integration time) »9 “original” pulsars  < (hybrid star) – interesting! »O(10) more have  < and O(100) have  < few x S5 all-sky »Solid strange star  max visible in most of galaxy (beyond core) »Hybrid star  max visible to few kpc (Gould belt, not galactic core) Detection:  too big for normal star Many non-detections: render a model unlikely

LIGO- G Z March 23, LLO 6 Don’t party just yet… Many radio pulsars have  < from spindown (probably even in globular clusters) How to get to  max ? How to keep at  max ? Stars with big  don’t last long in the LIGO band Hydromagnetic: accreting millisecond pulsars in LMXBs have  ~ from x-ray flux and torque balance; have we seen them all?

LIGO- G Z March 23, LLO 7 Conclusions Limits on  < (S2) are already (mildly) interesting Limits on  < (S5) get us to where we might detect something in a reasonable theory Enough non-detections will let us confront, though not rule out, some theories of dense matter