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Braking Indexes of isolated pulsars. Arxiv: 1209.2478, 1209.2273, 1211.4689 reporter:Fu, Lei. O utline. 1. Background 2. Models 3. Recent works 4. Our work. Theories Background. Braking law. magnetic dipole model.

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Braking indexes of isolated pulsars
Braking Indexes of isolated pulsars

Arxiv: 1209.2478, 1209.2273, 1211.4689

reporter:Fu, Lei


O utline
Outline

  • 1.Background

  • 2.Models

  • 3.Recent works

  • 4.Our work


Theories background
Theories Background

Braking law

  • magnetic dipole model

Assume:1.pure magnetic dipole model2.constant magnetic field


Observations background
Observations Background

  • Lyne et al.(1993)

  • Crab B0531+21: n=2.51

  • Kaspi et al.(1994)

  • B1509-58 : n=2.91

  • Lyne et al.(1996)

  • Vela B0833-45 : n=1.4


Models
models

Magnetic field evolution

magnetic diople radiation: B≠constant

Braking law


Models1
models

Disk assisted spin down

  • oblique rotator, non-dipole field, pulsar wind, quadrapole gravitational radiation, varying of effective moment of inertia……


Observations
Observations

recent works


Arxiv 1209 2478
arxiv:1209.2478

recent works

  • S.-N. Zhang & Y. Xie 2012 ApJ, 757,153

  • magnetic evolution


arxiv:1209.2478

recent works

for young pulsars for old pulsars


Observations1
Observations

recent works

baby pulsars


For baby pulsar younger than 2000 yr
for baby pulsar younger than 2000 yr

recent works

  • for Crab pulsar: age=957 yr(AD1054)

  • this model only applicable for young and old pulsars



Observations2
Observations

recent works


Arxiv 1209 2273
arxiv:1209.2273

recent works

  • J.A. Pons, D. Viganò & U. Geppert 2012 A&A 547,9

  • Magnetic field evolution senarios

fallback burying

reemergence

SN

thermoelectric field generation

Hall drift

Ohmic decay


recent works

  • Thermoelectric field generation

    • only efficient for

    • <1000 yr (in standard cooling senario)

  • Field reemergence

    • accreted mass

  • Ohmic decay

    • timescale

    • σ depends on

    • dominant in and lead n> 3

    • after neutrino->photon cooling(105 yr) is slow


recent works

  • Hall drift oscillatory modes

    • timescale

    • significant for large B field

    • dipole field->smaller scale

    • toroidal field->dipole field



Hall drift oscillatory modes

recent works

Hall drift oscillatory modes


P 0 0 01s 8 pulsars 2 5 kyr

recent works

P0=0.01s8 pulsars2.5 kyr



Arxiv 1211 4689 ali kan u ertan m a alpar et al 2012

recent works

arXiv:1211.4689Ş. Çalişkan, U. Ertan, M. A. Alpar et al.(2012)

  • PSR J1734-3333

    • only pulsation at radio band


Disk assisted spin down

recent works

Disk assisted spin-down





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