MMCOCOS December 2 – 6 , 2013

1. Long Time Evolutionary Simulations in Supernova until SNR phase Included the Uncertainties of CSMs MMCOCOS December 2 – 6 , 2013 Y. Matsuo A), M. Hashimoto A), M. Ono A), S. Nagataki B), K. Kotake C), S. Yamada D) , K. Yamashita E) A :Kyushu universityB : RIKENC : Fukuoka universityD : Waseda universityE : Yamanashi university

2. Cassiopeia A (Cas A) • Distance：3.4kpc( Reed et al. 1995) • Age：~330yr( Fesen 2006) • Forward shock --- 2.5 ±0.2 pc • Reverse shock --- 1.6 ±0.2 pc (Gothelf 2001) • Progenitor: 20～35 M(Chevalier & Oishi 2003; Yong et al. 2006; Fesen & Becker 1991) • Type IIb supernova ( krause et al. 2008 ) • The progenitor has less H-envelop • There is the emission line of Fe. • It is likey that Fe exists outside Si in Cas A (Vink et al. 2004, Badenes 2010) . Hwang et al. 2004 This indicates the mixing between Si- and Fe-rich matters during the expansion. Badences 2010

3. Motivation • From the observations, … • There is the emission line of Fe in Cas A. • It is likely that Fe exist outside the Si. • Nobody have simulated the evolution of the elements from the onset of SNexplosion to SNR phase. • So we try to simulate the SN shock expansion and trace the elements (in particular H,He,O,Si,Fe) from the onset of the explosion to SNR phase (330 yr). • In this study, we investigate whether Fe collides with the reverse shock at which the fluid instability develops.

4. Initial models • Progenitors • 6 M He core model (Hashimoto 1995) and 3.8M CO core model • Circumstellar mediums (CSMs) • We assumed that CSM consists of RSG wind and/or WR wind. • We adopted the several wind parameters ( for details, please see my poster) Density profiles of the CSM models Density profiles of the progenitor models

5. Results 3.8M CO core and slow wind (TWR= 4000 yr) 6.0M He core and slow wind (TWR= 4000 yr) • In the case of 6M He core models, Fe does not collide with the reverse shock in most CSM models. • In the case of 3.8MCO core models, Fe collides with the reverse shock in slow wind models. Red: H, green:He, blue:O, pink:Si, aqua:Fe Fe would be mixed because the fluid instability develops around the reverse shock region.

6. The position of shocks and Fe Fe ～ 1.2 pc

7. 2D results of the slow wind model Slow wind model ( TWR = 8000yr) RTI develops around the O-rich region. But Fe –rich matter are not mixed because … 1) the mixing time of Fe are not enough to mix 2) Fe are not mixed in the star before the shock pass through the stellar surface. The expansion velocity of Fe is too slow.

8. How do we need the expansion velocity of Fe ? • From the observations, Fe reaches at the reverse shock ( r = 1.6 pc ) • 1.6pc / 330yr = 4740 km/s ~ 5000km/s • So, we need that the Fe-velocity is about 5000 km/s at least. • Now, VFein our models is 3000-3500 km/s at most. • We need to increase the expansion velocity of Fe by a factor of ~ 1.5 at least. • Fe need to be mixed up to the O-rich layers when the shock pass through the stellar surface.

9. Fluid element velocity (slow RSG wind) Red: H, green:He, blue:O, pink:Si, aqua:Fe • The ejecta expand at constant velocity after the ejecta reach the stellar surface. • Expansion velocities of … • O ~ 4000 – 6000 km/s • Si ~ 3500 – 4000 km/s • Fe ~ 3000 – 3500 km/s

10. How do we need the expansion velocity of Fe ? • From the observation, Fe reach at the reverse shock ( r = 1.6 pc ) • 1.6pc / 330yr = 4740 km/s ~ 5000km/s • So, we need that the Fe-velocity is about 5000 km/s • Now, VFein our models is 3000-3500 km/s. • We need to increase the expansion velocity of Fe by a factor of ~ 1.5 at least. • Fe need to be mixed up to the O-rich layers when the shock pass through the stellar surface.

11. Summary • We try to simulate the formation of SNR from onset of SN explosion and compare the results and the observation of Cas A. • From the observation, Fe reaches at reverse shock and it is likely that Fe and SI mixed during the explosion. • In all our models, Si and Fe are not mixed because the mixing between SI and Fe at SN explosion are not enough that Fe collides with the reverse shock. • We find that expansion velocity of Fe need to be increased by a factor of ~ 1.5 at least and this problem is not solved if CSM distribution are changed. • We should the estimate of growth rate of RTI to investigate the reason why Fe are not mixed in the star. • So, we will try to mix Fe to O-shell artificially and investigate the possibilities that Fe would exist outside the Si.