1 / 22

Understanding Hypernovae and Gamma-ray Bursts: Key Insights from SN 1998bw and Beyond

This document explores the dynamics of hypernovae and gamma-ray bursts, with a focus on SN 1998bw. It discusses the characteristics of hypernova candidates, their kinetic energy ranging from (5-10) × 10^51 ergs, and the spectral features of type Ic supernovae lacking hydrogen and strong helium. Key models, light curves, and nucleosynthesis processes are detailed, shedding light on massive stellar explosions and their implications for cosmic nucleosynthesis. The document also addresses the significance of aspherical explosions and the formation of black holes.

wilmet
Télécharger la présentation

Understanding Hypernovae and Gamma-ray Bursts: Key Insights from SN 1998bw and Beyond

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. Hypernovae and Gamma-ray Bursts K. Nomoto (U. Tokyo)

  2. SN 1998bw Hypernova CandidatesEkinetic > (5-10)×1051ergs GRB 980425

  3. Spectra of Supernovae & Hypernovae Ic: no H, no strong He, no strong Si SiII Ia O Ca He Ib Hypernovae： broad features blended lines 　　“Large mass at high velocities” Ic 94I 97ef Hyper-novae 98bw

  4. CO Star Models for SNeIc H-rich He ５６Fe C+O 56Co MC+O Si 56Ni Fe Collapse • ~ [dyn• diffusion]1/2 ~• 1/2  Mej R V R c Parameters [Mej, E, M(56Ni)] Light Curve Spectra E  Mej  ½Mej¾E -¼ ５６Ni E  Mej3

  5. Spectral Fitting: SN1997ef Iwamoto et al. 2000 Too Narrow Features Normal SN (E51=1) Small Mej Hypernova (E51=20) Large Mej at High Vel. Broad Features

  6. Light curves of Hypernovae & SNeIc log L (erg/s) Radioactive Decay 56Ni 56Co 56Fe 43 98bw&CO138 42 97ef&CO100 41 94I &CO21 0 50 100 t (days)

  7. Bolometric Light Curves SN 2003dh Mej=8M E=3.8×1052ergs M(56Ni)=0.35M SN 1998bw COMDH SN 2002ap SN 1997ef Mazzali et al (2003)

  8. Type II-P SN 1997D Very narrow lines. V < 1000 km s-1. EK=1-4×1050ergs. V~1000km s-1 2002gd, 1999br Faint M(56Ni)~2×10-3M (Turatto, Mazzali, Young, Nomoto 2002)

  9. Turatto, Mazzali, Young, Nomoto, Iwamoto et al. (1998) SNⅡ 1997D:Faint SN m－M=30.64 (NGC1536) 1987A LBOL 1997D Mms~20M M(56Ni) 0.07M 0.002M 1987A 1997D Mms~ 25－30MR ≤ 300R E~4×1050erg narrow lines

  10. Supernovae/Hypernovae Nomoto et al. (2003) EK Failed SN? 13M~15M

  11. M(56Ni)/M Nomoto et al. (2003) [/Fe]≫0

  12. SNe in Binary Systems Single M1~M2 ”Conservative” M1»M2 ”Non-Conservative” 2 1 2 1 Spiral-in RSG Rapid Rotator SNII Wolf Rayet (WN, WC) He, C+O Star SNIb/c ? SNIb/c Hypernovae?

  13. McWilliam, Ryan, Spite, Co Cr trend [Fe/H] [Fe/H] Mn Zn

  14. Hypernova Nucleosynthesis (1) M(Complete Si-burning) (Zn, Co)/Fe (Mn, Cr)/Fe Fe/(O, Si) (2) More ‐rich entropy Zn/Fe 64Ge Ti/Fe (3) More O burns (Si, S, Ca)/O Low energy High energy

  15. Jet-Induced Explosion Rotating Black Hole + Accretion Disk K. Maeda, 2003

  16. Collimated jets (Z) + Bow shock (All direction) M Lateral expansion Radial Velocity/c Hydrodynamics R/1010cm

  17. Jet-induced Explosion Maeda & Nomoto (2003), astro-ph/0304172 E51=10, MBH(final)=6M, M(56Ni)=0.1M, MCO=14M 0.04 0.04 0.7 s 1 Outflow Inflow (Fallback) 0 0 0 1.5 s R/1010cm

  18. [OI] 6300A 56Fe 16O Interpretation as an Aspherical explosion FeII] 5200A Observation Spherical 15 deg Aspherical Maeda et al. 2002

  19. Element Distribution Bipolar Explosion Model Zn Zn Zn Zn Mn

  20. Spherical 40M, E51=1 Jet 40M, E51=10 [Cr/Fe] [Mn/Fe] Jet 25M, E51=7 Spherical 25M, E51=1 [Co/Fe] [Zn/Fe]

  21. UN2003 Co Cr 15M, E51=1 25M, E51=30 (Hypernova) Mn Zn

  22. Origin of Hypernovae and Gamma-Ray Bursts Hypernovae • High Energy: E>1052erg • Massive: Mms>20-25M, typically 30-40M Black Hole forming Supernovae • Aspherical (Jet-induced) Explosions • Spectra, Light curves, Polarization Rotating Black Hole + Accretion Disk • Type Ic SNe: C+O stars Mergers in Binaries First Stars ? • Hypernova Nucleosynthesis Abundance Patterns of Extremely Metal-Poor Stars

More Related