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Evolution of Magnetar-Powered Supernovae

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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 1 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 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)?? (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 -> 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 Energy injection 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 × υ ] 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 logE [erg] 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. 17.
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