Magnetars: wind braking

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Presentation transcript:

Magnetars: wind braking PAC2012, Xiangshan Magnetars: wind braking H. Tong Xinjiang Astronomical Observatory

Where are they?

Traditional magnetar model young NS (SNR & MSC) Bdip> BQED=4.4×1013 G (braking) Bmul=1014 -1015 G (burst and super- Eddington luminosity and persistent emission) 3

“Magnetic dipole braking” of normal pulsars Rotational energymagnetic dipole radiation+particle wind (rotation-powered) Effects: higher order modifications, e.g. braking index (Michel 1969; Manchester 1985; Xu & Qiao 2001; Contopoulos & Spitkovsky 2006; Wang+ 2012) timing noise (Lyne+ 2010; Liu+ 2011) +a rotation-powered PWN Exist: intermittent pulsars (Kramer+ 2006; Camilo+ 2012)

Intermittent pulsars B1931+24 (Kramer+ 2006)

Magnetic dipole braking is only a pedagogical model! Rotating dipole in vaccum! Only as first order approximation to the real case Normal pulsars braked down by a rotation- powered particle wind

Existence of a particle wind in magnetars Varying period derivative Higher level of timing noise (compared with HBPSRs) Magnetism-powered PWN Correlation between Lpwn and Lx Higher Lpwn/Edot

PSR J1622-4950 (Levin+ 2012)

Rotational energy loss rate In summary Magnetism-powered particle wind When Lp >> Edot, a much lower magnetic field (plus higher order effects, magnetar case)

Dipole magnetic field (1): magnetic dipole braking Polar magnetic field

Dipole magnetic field (2): wind braking Dipole magnetic field in the case of wind braking

Dipole B (case I)

Conclusions (1) Wind braking: Wind-aided spin down A lower surface dipole field Magnetars=NS+strong multipole field Explain challenging observations of magnetars Their SNe energies are of normal value Non-detection of magnetars by Fermi-LAT The problem of low-B SGRs The relation between magnetars and HBPSRs A decreasing Pdot during magnetar outburst Low luminosity mangetars more likely to have radio emissons Two predictions A magentism-powered PWN A braking index n<3

Conclusions (2): subsequent developments Magnetism-powered pulsar wind nebula around SGR Swift J1834.9-0846 (Younes et al. 2012) Geometrical effect during wind braking: small inclination angle--> higher B (Tong & Xu 2012)

A paradigm shift in the future? FAST: more radio-loud magnetars, HBPSRs, intermittent pulsars … “Pulsars are electromagnetic braking” For short Pulsars are wind braking