the physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · magnetar activities from the cco in...
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![Page 1: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/1.jpg)
Thephysicsofmagnetar magnetosphere:understandingrecentmagnetar observationsfromthe
magnetospheric pointofview
H.Tong(仝号)2017.2
XinjiangAstronomicalObservatory,ChineseAcademyofSciences
Homepage:www.escience.cn/people/tonghao
For QCS 2017@YITP, Kyoto University
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Content
1. Introduction:what’smagnetars?2. Progressofisolatedmagnetars:
windbrakingofmagnetarsandmagnetarwindnebula
3. Accretingmagnetars
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1.Pulsarsandmagnetars(upto2017)1. Rotation-poweredpulsars2. Accretion-poweredpulsars3. Magnetars (?)
• AnomalousX-raypulsars• Softgamma-rayrepeaters
4. Thermal-powered• X-raydimisolatedneutrons(XDINSs)
5. ??• Rotatingradiotransients(RRATs)• CentralCompactObjects(CCOs)• ???,e.g.1987Apulsars
Magnetar is a special kind of pulsarswhy special? how special?
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Magnetarsmyfavorite!
updatedfromTong2016
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Τc"103 yr
106 yr
109 yr
Bc"10 10G
10 12G
10 14G
deathline
"!# magnetar$ XDINS! CCO
% RPP& RRAT' intermittent pulsar
&&
&
&&
&& && &
& &&& &
&
& &
&
&& &
&
&
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& &&
''
'
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''
$$$$$$
!!!!!!
""
"
"""
"
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"""
"
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"
#
###
10#3 10#2 10#1 100 10110#22
10#20
10#18
10#16
10#14
10#12
10#10
10#8
P"s#
dP!dt"s!s
#
![Page 5: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/5.jpg)
Traditionalmagnetar model(Mereghetti 2008)
Magnetar=1. youngNS(SNR&MSC)2. Bdip>BQED=4.4×1013 G(braking)3. Bmul=1014 -1015 G(burstandsuper-Eddington
luminosityandpersistentemission)
![Page 6: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/6.jpg)
Giantflaresofmagnetars(Mereghetti 2008):1.Spike+pulsatingtail(hundredsofseconds)
2.10^4timessuper-Eddingtonduringthetail(10^42ergs^-1)
Explanation:10^15Gmagneticfieldastheenergypowerandcauseofsuper-Eddingtonluminosity
![Page 7: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/7.jpg)
2.Recentprogressesofmagnetars
• 2010:“lowmagneticfield”magnetar(B<7.5*10^12G)Ferminon-detectionofmagnetars
• 2013:anti-glitch;Galacticcentermagnetar• 2014:accretingmagnetar• 2016:magnetarwindnebula;super-slowmagnetars;magnetaroutburstfromaradiopulsar
![Page 8: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/8.jpg)
Openquestions
Howmagnetars arespundown?• Whysomanytimingeventsinandonlyinmagnetars?
• Unifiedspindown mechanismofpulsarsandmagnetars
My answer: wind braking(Tong, Xu, Song, Qiao 2013, ApJ, 768, 144)
![Page 9: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/9.jpg)
Variousalternatives(Tong&Xu2014AN)
1.NS+twistedmagnetosphere(Thompsonetal.2002;Beloborodov 2009)(fornon-rotatingmagnetars)2.Windbrakingofmagnetars(Tongetal.2013)3.Coupledmagneticandthermalevolution (Vigano+2013)4.Fallbackdiskmodel(Alpar2001)5.Accretioninducedstarquakemodel(Xuetal.2006)
6.Quarknovaremnant(Ouyedetal.2007)7.AccretingWDmodel(Paczynski1990)
![Page 10: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/10.jpg)
Wingbrakingofmagnetars(Tong+2013)
• Insummary
• Magnetism-powered particlewind• WhenLp >>Edot,amuchlowermagneticfield(plushigherordereffects,magnetarcase)
工作3:
![Page 11: The physics of magnetar magnetosphereqcs2017/21/h_tong.pdf · Magnetar activities from the CCO in RCW 103 • Rea et al. arXiv:1607.04107; D’Ai et al. arXiv:1607.04264 (appear the](https://reader034.vdocuments.us/reader034/viewer/2022050422/5f90fea03f948a592d4f80b7/html5/thumbnails/11.jpg)
Subsequentworks(1)
• Variablespin-downofthesecondlow-Bmagnetar (Tong&2013RAA)
• Radioupperlimitsofonemagnetar (Tongetal.2014RAA)
• Anti-glitchinthewindbrakingmodel(Tong2014ApJ)
• Timingbehaviorofthegalacticcentermagnetar (Tong2015RAA)
• Magnetar windnebula(Tong2016RAA)
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Decreasing period derivative of the second low-B magnetar
Tong & Xu 2013 RAA
Scholz+ 2014
Decreasing Pdot a decresing particle wind
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Spindown behavior of the Galactic center magnetar, Kaspi+ 2014
1. Decreasing Lx2. Increasing spindown rate•negative correlation betweenLx and Pdot
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Changes of polar cap opensing angle, Tong 2015 RAA
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Anti-glitchofmagnetar1E2259+586
● Archibald+(2013)Anti-glitch
14 days interval
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Anti-glitchinthewindbrakingscenarioTong2014ApJ,citations:19
1.Duetoanenhancedparticlewind2.Anti-glitchalwaysaccompaniedbyradiativeevents
3.Noanti-glitch,butaperiodofenhancedspindown
● Futureanti-gltichwithoutradiativeeventoraverysmalltimescalecanruleoutthewindbrakingmodel
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Woods+ 2007
bursts
A period of enhanced spindown
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If…
• Anti-glitch:duetoastrongerparticlewind• ??????: aweakerparticlewind/theparticlewinddisappeared
Spindown behavior of intermittent pulsarsLi, Tong+ 2014 ApJ
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The first possible magnetar wind nebula (Younes et al. 2016)
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Younes et al. 2016
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My comments (Tong 2016 RAA)
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Openquestions
l 1967:discoveryofpulsars(Hewish,Belletal.)l ~1970:X-raypulsars(accretingneutronstarsinbinarysystems,Giacconietal.)
l 1982:millisecondpulsars(Backeretal.)RecycledneutronstarsvialowmassX-raybinaries
l 1990s:magnetar(Thompson/Duncan,Kouveliotouetal.)
– Whereareaccretingmagnetars?
3. accreting magnetar
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Spectraofmagnetars(Abdo etal.2010)
Cutoff?
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Mereghetti etal.(2015):comparisonbetweendifferentkindsofobjects
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Cuttoffat~130keVfor4U0142+61(Wang,Tong,Guo2014RAA;9yearsIntegraldata)
Conclusion:ultra-relativisticmodelscanberuledout!
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Thekeydifferencebetweenmagnetarsandrotation-poweredpulsars:multipole magneticfield!
Nottheirpositions ontheP-Pdot diagram(determined bythemagnetospheric torque)
Evidenceforstrongmultipole fieldinaccretingsystems(Tong&Wang2014):1.magnetar burst2.hardX-raytail3....
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10#3 10#2 10#1 100 10110#22
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SuperslowX-raypulsarmaynotbeaccretingmagnetars
(Tong&Wang2014)SuperslowX-raypulsarsin HMXBs
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Ultraluminous X-raysources(Feng &Soria 2011)
l X-raypointsourcesoffsetfromthenucleiofnearbygalaxies
l Lx=10^39-10^41ergs^-1l Intermediatemassblackhole(100-10000Msun)orsuper-Eddingtonaccretingstellarmassblackholeor...
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Pulsation (1.37s)modulatedBytheorbitalmotion (2.5day)
Bachetti etal.2014
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Bachetti etal.2014
Theneutronstarisspinning up!Pdot=-2*10^-10Typicalaccretion-powerX-raypulsars
Problem &Difficulity:Howtoexplainthesuper-Eddingtonluminosity (10^40ergs^-1)andspin-uprate?
Accretingmagnetar
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Models:accretingmagnetarl Observation:Bachetti etal.(arXiv:1410.3590)1. Eksi etal.(arXiv:1410.5205):accretingmagnetar,smallertorque
duringaccretionequilibrium2. Lyutikov (1410.8745):accretingmagnetar,super-Eddingtonaccretion3. Kluzniak &Lasota (1411.1005):ULXpulsar-->millisecondpulsar4. Tong(1411.3168):accretinglowmagneticfieldmagnetar5. Christodoulouetal.(1411.5434):accretingnormalneutronstar6. Dall'Osso etal.(1412.1834):accretingmagnetar7. Mushtukovetal.(1506.03600):maximumluminosityof10^40ergs^-
18. Guo etal.(1508.00390): massivepulsars(GRresponsibleforthesuper
Eddington luminosity)9. Panetal.(1510.08597):evolutionofaccretingmagnetars10. Fragos etal.(1501.02679),Shao&Li(1502.03905):formation
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Accretinglowmagneticfieldmagnetar
l Agedmagnetars aremoreliketobelowmagneticfieldmagnetars (10^6yrs old;consistentwithpopulationsynthesis)
l Super-Eddington luminosityduetothepresenceofstrongmultipole field(e.g.,10^14G)
l Rotationalbehaviorsduetotheinteractionofmuchlowerdipolefield(10^12G)withtheaccretionflow
工作4:吸积磁星
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Panetal.2015
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citations: 13
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subsequent support: Chen 2016, MNRAS
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CCO(1E1613)inRCW103(DeLuca+2006)
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Peculiarities
1. Variability2. Periodicity(6.6hour)Nature:magnetar!
Problem:P=6.6hr?Sol:fallbackdiskbrakingNewProblems:Accretionpowered?;Pdot?
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MagnetaractivitiesfromtheCCOinRCW103
• Reaetal.arXiv:1607.04107;D’Aietal.arXiv:1607.04264(appearthesamedayonthearXiv)
• burst:duration~10ms,spectra:BB,T~10keV• Timing:the6.6hrperiodisstillthere• spectra:2BB(Chandra)+PL(NuSTAR),PL
index~1.2(transienthardX-raycomponent,similartomagnetaroutburst)
• outburst:threeoutburstperiod,energyreleasecanbeashighas10^43erg
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Burst from the RCW 103 direction, Rea et al. 2016
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Outburst from the CCO in RCW 103, D’Ai et al. 2016
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NatureofCCOinRCW103
1. amagnetar!2. averyspecialmagnetar comparedwith
magnetars,CCOs,normalneutronsandaccretingneutrons:thelongestspinperiod!
3. amagnetar brakeddownbyafallbackdiskinthepast?
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3 weeks later (Aug 6th):
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Summary:magnetarsinastrophysics
1. AXP/SGR2. XDINSs:deadmagnetar3. CCO:magnetar-in-waiting/diskbrakeddown
magnetar4. HBPSR:magnetar activitiesalsoseen
(PSRJ1846-0258;andJ1119-6127)5. LowBSGR:magnetar activitiesinnormal
pulsarsinthefuture!6. Magnetars inbinarysystem?(LSI+61,
superslow X-raypulsars,ULXpulsarsetc)
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Thankyouverymuch!