1 / 21

Hayato Mikami (Chiba Univ.) Collaborators : Yuji Sato(Chiba Univ.), Tomoyuki Hanawa(Chiba Univ.),

Core Collapse And Supernova Explosion Of Massive Star Having Magnetic Field Inclined To The Rotation Axis. Hayato Mikami (Chiba Univ.) Collaborators : Yuji Sato(Chiba Univ.), Tomoyuki Hanawa(Chiba Univ.), and Tomoaki Matsumoto(Hosei Univ.). Introduction. Type-II supernovae

wendi
Download Presentation

Hayato Mikami (Chiba Univ.) Collaborators : Yuji Sato(Chiba Univ.), Tomoyuki Hanawa(Chiba Univ.),

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Core Collapse And Supernova Explosion Of Massive Star Having Magnetic Field Inclined To The Rotation Axis Hayato Mikami (Chiba Univ.) Collaborators: Yuji Sato(Chiba Univ.), Tomoyuki Hanawa(Chiba Univ.), and Tomoaki Matsumoto(Hosei Univ.)

  2. Introduction • Type-II supernovae • Asymmetric explosions • 2D MHD simulation(Sawai et al. 2004, Ardeljan et al. 2005) • The 3D effect by the magnetic field inclined to the core rotation axis • Magnetic field configuration • Direction of outflow • Dependence on the initial Ω and B

  3. Initial model • ρ0 = 6.8×109 g cm-3 • 15 Mo model (Woosley et al. 2002) 6000 km

  4. Initial model • ρ0 = 6.8×109 g cm-3 • Ω0 = 0.15 - 1.2 rad s-1 • Differential rotation

  5. Initial model • ρ0 = 6.8×109 g cm-3 • Ω0 = 0.15 - 1.2 rad s-1 • B0 = 0.25 - 4.0×1012 G • Dipole-like • Uniform near the central region

  6. Initial model • ρ0 = 6.8×109 g cm-3 • Ω0 = 0.15 - 1.2 rad s-1 • B0 = 0.25 - 4.0×1012 G • φ0 = 60° φ0

  7. Sawai et al Our work Parameters • Initial rotation Ω0 • Initial magnetic field B0

  8. The calculation method • Ideal MHD equations • EOS(Takahara & Sato, 1984) • The phenomenological parametric • P = Pthermal + Pcold • Pcold = KρΓ • Nested grid method • Roe method modified with the care for the Carbuncle instability • Numerical Viscosity to Care the Carbuncle Instability (Hanawa,11/3)

  9. Parameters

  10. Overview t=0 ms 230 ms

  11. Overview The next movie Core collapse (189 ms) After bounce (41 ms) Jets 206 ms

  12. 3D movie • The initial parameters • Ω0 = 1.22 s-1 • B0 = 3.04×1012 G 400 km Ω0 B0 lines - Magnetic fields - proto neutronstar ( ρ > 1014 cm s-1 ) - outflow ( vr > 109 cm s-1 ) 185 ms < t < 230 ms

  13. Time evolution of Energy (R<40 km) Eg Ecold Ethermal Ek Emag Jets

  14. Emagwas stored on R=10 & 60 km 206 ms Jets Enhanced by the core rotation 60 km NS 10 km Emag (erg)

  15. Jet launched at R=60 km 206 ms Jets 109 cm s-1 60 km NS 10 km

  16. 2D movie (187 < t < 230 ms) 187 ms Ω0 B0 B0 Ω0 200 km 40 km

  17. Layers of neutral sheets

  18. Jets launched from R=60 km

  19. Dependence on the initial Ω Fast Ω0 produced fast jet Fast Ω0model Faster Slow Ω0model

  20. Dependence on the initial B Strong B0 produced fast jet. Strong B0model Faster Weak B0model

  21. Conclusion • Neutral sheets: new feature in 3D • Emag is stored on the sphere of R=10 and 60 km. • Jets • Direction of jets is along the rotation axis. • Jets are launched from R=60 km. • Fast Ω0 produce fast jets. • Strong B0 produce fast jets.

More Related