Evolution of Magnetar-Powered Supernovae

Evolution of magnetar-powered supernovae

Miyu Masuyama, RESCEU collaborator : Toshio Nakano, Toshikazu Shigeyama

RIKEN-RESCEU joint meeting 2016/07/25-27

• Neutron Stars (NS) • generated by core collapse supernovae • observed NS, a few hundreds

• Power sources of them • rotation energy • gravitational energy of accreting matters • thermal energy • magnetic field energy

2 1. Neutron stars

• Neutron Stars (NS) • generated by core collapse supernovae • observed NS, a few hundreds

• Power sources of them • rotation energy • gravitational energy of accreting matters • thermal energy • magnetic field energy

-> We focus on NS with strongest magnetic fields, “Magnetar”.

3 2. Magnetars

• NS with strong magnetic fields

-8 10 10 16 G

10-10 12 10 15 ( typical neutron stars : B~10 G ) G -12 • Spin down. Pdot > 0 10 10 14 G 1kyr • Radiate X-ray by using magnetic -14 10 35 10kyr 10 13 fields. Lx ~ 10 erg/s >> Lspin G 100kyr 10-16 -> rapidly spin & Highly 1Myr 10 12 G

magnetize at their birth. Period derivative(s/s) 10Myr 10-18 100Myr 10 11 G -20 -> The mechanism for growth of 10 Radio Pulsar Magnetar strong magnetic fields & what Binary 10-22 supernovae generate magnetars 0.001 0.01 0.1 1 10 100 have not been well understood. Period(1/s)(s) (ATNF pulsar catalog) 4 3. Previous works

• discovered magnetars : about 30 North West (NW) North east (NE) 506037010 ( ATNF pulsar catalog ) 506039010

• some associate with SNR XIS0,3 ( e.g. Kes 73, CTB 109 ) 1E 2259+586 1E 2259+586 (AXP) 404076010

• Observations of such SNR : XIS1 • Progenitors are very massive ( >30M◉) ( e.g. Figer +05, Kumar +12 ) 51 • ESNR ~ 10 erg ( e.g. Vink & Kuiper 06 ) South West (SW) South East (SE) 506038010 50604010 • Theoretical prediction※ : Suzaku X-ray image, 52 CTB109 (SNR) & 1E2259+586 (magnetar) • Erot ~ 10 erg are injected to stellar envelope by magnetic dipole radiation.

15 ※ Magnetars have very short spin periods (P0 < 3ms) and highly strong magnetic field (B0 > 10 G) at their birth (α-dynamo effect) (Duncan & Thompson 92). 52 Therefore they have Erot ~ 10 erg and inject its energy to stellar envelope.

5 4. Our work 2.1 何をやっていたのか ( 私の修論の復習 )

core collapse supernove supernove remnant of massive star t ~ 0 sec t ~ 100 days t ~ 10,000 yrs explosion expansion R ~ 1010 cm R ~ 1019 cm

52 51 Erot ~10 erg (A)?? (B)?? ESNR ~10 erg (C)??

(A). A mechanism without rapidly rotation 52 amplify a magnetic field of magnetar. -> Erot < 10 erg (B). Most of rotation energy is used for something (e.g. GW, binding energy). 51 (C). Underestimate energy of SNR associated with magnetars. -> ESNR > 10 erg

6 4. Our work 2.1 何をやっていたのか ( 私の修論の復習 )

core collapse supernove supernove remnant of massive star t ~ 0 sec t ~ 100 days t ~ 10,000 yrs explosion expansion R ~ 1010 cm R ~ 1019 cm

52 51 Erot ~10 erg (A)?? (B)?? ESNR ~10 erg (C)??

-> We perform 1D hydrodynamical simulations of evolutions of magnetars for 10,000 yrs

to investigate the relation between Erot and ESNR. 7 5. Set up for simulations

Energy Injection to stellar envelope Magnetar by magnetic dipole radiation

CSM ISM stellar envelope

WR star just before explosion ( Iwamoto et al. 1998 )

M~40M◉ density

10-24 g/cm3

106 cm 108 cm 1010 cm 5 pc 8 distance from the center 5. Set up for simulations

Energy Injection to stellar envelope Magnetar by magnetic dipole radiation

CSM ISM stellar envelope

WR star just before explosion ( Iwamoto et al. 1998 )

M~40M◉ density

Calculation region

10-24 g/cm3

106 cm 108 cm 1010 cm 5 pc 9 distance from the center 5. Set up for simulations

1D hydrodynamical simulation

Energycontinuity Injection equation to stellar envelope Magnetar by magnetic dipole radiation equation of motion CSM ISM stellar envelope =- energy equation + Q WR star just before explosion ( Iwamoto et al. 1998 )

L(t) injected from rotation energy of a magnetar Q = { @ inner most region M~40M◉ 0 @ the other region density

Calculation region

10-24 g/cm3

106 cm 108 cm 1010 cm 5 pc 10 distance from the center 6. Magnetars as a explosion engine

Magnetar 52 2 17 = 10 erg ~ lω B0=10 G Erot

1015 G inject energy to stellar envelope tp = 0.1 s by magnetic dipole radiation 1012 G

rot 103 s

Energyinjection rate[erg/s] 109 s

rot 0.01 102 106 108 1014 Energy injection time [s] 11 7. Time evolution of shock waves

reverse shock t = 4,000 yrs after explosion -23 ]

3 forward shock (a) -26

[g/cm CSM

density ρ

log -29 ejecta ISM 15.01.5 shock are formed 10.01.0 (b) by energy injection [cm/s] 7 from magnetar. velocity 10 5.0 ×

] 0.0 2 Initial proﬁle -8

(c) ρ ejecta [g/cm/s -11 log p pressure CSM ISM log -14 19 19 1.0×10 4.0×10 distance from the center distance from the center r [cm] 12 8. Energy of neutrino-heating

• ESNR ~ Erot + Eν,heating + Enuc + Ebind

-> The stalled shock is revived by depositing of a part of energy 1051 erg carried away by neutrino νe, ーνe.

※in the core νe νe + n -> p + e- ーνe ーνe + p -> n + e+

neutrino sphere stalled shock

51 • Eν,heating ~ 10 erg

13 9. Energy of nuclear reactions

• ESNR ~ Erot + Eν,heating + Enuc + Ebind • rough estimation of nuclear energy under assumption that the matter which exceed T > 5×109 K will be 56Ni.

10 -> P0 = 2 msec, energy is injected instantly 28Si -> 56Ni @ T > 5×109 K [K] max

16 P0 = 2 msec, B0 = 5×10 G log T magnetar • We should calculate hydrodynamical 9 simulations including nuclear reactions 2 3 4 5 and feedback to hydrodynamical simulations Mass [solar mass] for magnetar-powered supernovae.

14 10. Gravitational binding energy

• ESNR ~ Erot + Eν,heating + Enuc + Ebind

• Progenitors of magnetars are considered to be massive stars. ( e.g. Safi-Harb & Kumar 2012 ) Magnetar Progenitor mass

1E 1048.1-5937 (Gaensler+ 2005) 30-40 M◉

CXO J164710.2-455216 (Muno+ 2006) > 40 M◉

SGR1806-20 (Figer+ 2005) ~50 M◉

SGR 1900+14 (Davies+ 2009) 17 M◉

1E 1841–045 (Kumar+2014) >> 20 M◉

SGR 0526–66 (Uchida+2015) ~26 M◉

1E 2259+586 (Nakano PhD thesis) ~40 M◉

51 • Ebind ~ - 5 × 10 erg ( just before explosion )

in case that a progenitor mass is 40 M◉

15 11. Time evolution of energy

• ESNR ~ Erot + Eν,heating + Enuc + Ebind

52 51 51 51 ~ 10 + 10 + 10 - 5×10 ~ 1051 erg 52 Energy injection from magnetar Erot ~ 10 erg -> Most of the rotation energy 1e+5252 1052 erg is used to climb up the Internal energy, Ei 51 gravitational potential well of a ESNR ~ 10 erg massive star and the resultant 1e+5151

SNR possesses the rest of the 52 51 Kinetic energy, Ek energy ESNR ~ 10 erg. 1e+5050

ESNR log [erg] E Energy, Gravitational energy, -Eg

1e+4949 Einject 0.01 1 100 100002 5 1e+06 1e+08 1e+10 1e+12 r -2 0 2 4 6 8 10 12 Ebind Time after explosion, log t [sec]

16 12. Summary

• We perform 1D hydrodynamical simulations to investigate the relation between energy of magnetars at their birth Erot and energy of supernova remnants associated with magnetars ESNR.

• Most of the rotation energy is used to climb up the gravitational potential well of a massive star and the resultant supernova remnant 51 possesses the rest of the energy ESNR ~ 10 erg.

• We should carry out simulations including nuclear reactions and feedback to hydrodynamics.