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From Progenitor to Afterlife

From Progenitor to Afterlife. Roger Chevalier. SN 1987A. HST/SINS. Core Collapse Supernova Types. IIP (plateau light curve) IIL (linear light curve) Ib (no H, He present) Ic (no H, no He) IIb (H early; like Ib or Ic late) IIn (narrow line) IIpec (peculiar, e.g., SN 1987A). Wheeler 1990.

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From Progenitor to Afterlife

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  1. From Progenitor to Afterlife Roger Chevalier SN 1987A HST/SINS

  2. Core Collapse Supernova Types • IIP (plateau light curve) • IIL (linear light curve) • Ib (no H, He present) • Ic (no H, no He) • IIb (H early; like Ib or Ic late) • IIn (narrow line) • IIpec (peculiar, e.g., SN 1987A) Wheeler 1990

  3. Progenitor stars • IIP (plateau) • Red supergiant • IIb, IIn (narrow line), IIL (linear) • Red, or cool, supergiant • Ib, Ic • Wolf-Rayet star • SN 1987A – like • Blue supergiant

  4. Single massive star evolution Heger et al. 2003

  5. Fractional frequency of SN Types(Cappellaro,….) • Type IIP 0.3 • Types IIL, IIn, IIb 0.3 • Types Ib,Ic 0.25 • SN 1987A – like 0.15 (upper limit) • High incidence of Type IIL/n/b and Ib/c indicates that binary evolution is important

  6. Element mixing by instabilities during explosion Kifonidis et al. 03

  7. Supernova density profile Break at velocity vbr ~ (E/M)1/2 vbr ~ 3000 km/sec for E=1051 ergs and M =10 M Maximum velocity limited by radiation (Matzner & McKee 99)

  8. Afterlife properties that depend on SN type • Composition structure • Maximum velocity • Photoionizing radiation at shock breakout • Core (neutron star/black hole) mass • Fallback of matter to central core • Density structure (on E and M)

  9. Reverse shock Freely expanding ejecta Forward shock cs wind

  10. Blondin, RAC

  11. Cas A radio NRAO/AUI

  12. Model with synchrotron self-absorption and interaction of outer steep power law profile with a wind n-1.0 spectrum, R~t0.9 Type Ic SN 1994I in M51 Data from Weiler, Stockdale,….

  13. Type Ib/c, no GRB Type Ib/c, GRB Type IIb Type IIP Type IIL Type IIn

  14. Type Ib/c, GRB Relativistic H env. – 0 M Type Ib/c, no GRB H env. - 0 M Type IIb – WR H env. - 0.01 M Type IIb – RSG H env. - 0.1 M Type IIL H env. - 1 M Type IIP H env. - 10 M

  15. SN 1987A – delayed radio increase optically thin optically thick Data from Ball

  16. X-ray Chandra Immler et al. 02 SN 1994I at 7 years

  17. Model radio – X-ray spectrum of SN Ic Photosphere Inverse Compton Synchrotron Fransson/RAC

  18. X-ray emission • Type II • Thermal • Type Ib, Ic • Synchrotron • Inverse Compton near maximum light

  19. Mass loss • IIP (plateau) • ~10-6-10-5 M/yr (vw=10 km/sec) • IIb, IIn (narrow line), IIL (linear) • ~10-5-10-3 M/yr (vw=10 km/sec) • Ib, Ic, some IIb • ~10-6-10-4 M/yr (vw=1000 km/sec) if magnetic amplification efficient

  20. Long duration gamma-ray bursts • Associated with SNe Ib/c, ~1/200 the rate • Afterglow theory well-developed, but generally indicates interaction with a constant density medium

  21. Synchrotron emission Spherical relativistic blast wave early Jet effects late Sari et al. 98 Zhang & Woosley

  22. Shocked wind bubble a possibility, but termination shock radius too large, transition not seen,…

  23. SN 1987A 1/3 pc scale HST/SINS Light echo – dense wind to ~5 pc

  24. Extended mass loss • Fast wind during main sequence phase gives extended bubble • Slow RSG wind extends to • During possible Wolf-Rayet phase, dense wind can be swept out by the fast wind

  25. Inner and outer interaction Shock in ejecta Reverse shock Forward shock Pulsar wind termination shock Blondin, RAC, Frierson 01

  26. Possible IIP - Crab • No outer interaction observed • Crab has low velocity hydrogen • Crab abundances imply progenitor mass ~10 M

  27. G21.5-0.9 – initially pure pulsar nebula Radio Chandra – X-ray Becker & Szymkowiak 1981 Matheson & Safi-Harb 2005

  28. 0540-69, Kes 75, MSH 15-52 • Radii 9-20 pc • Average velocity >~10,000 km/sec • Seem to have crossed “wind bubble” • Not IIL/n/b • Probably Ib, Ic; irregular shell may be RSG wind swept out by WR star wind Kes 75, X-ray Helfand et al. 03

  29. Young PWNe .

  30. Wind interaction model for Cas A- likely IIL/n/b • Expansion rate of bright shell and forward shock consistent with wind (r~r-2) interaction model • Wind density: dM/dt ~3x10-5 M/year for vw=10 km/sec • Contains a quiet, compact object RAC & Oishi 03 NASA/SAO/CXC

  31. Summary • Properties of young remnants can be related to supernova properties; mass loss environment deduced from interaction generally consistent with evolutionary expectations (not the case for GRBs) • Present data do not show a correlation of pulsar/neutron star properties with supernova type

  32. Reverse shock in Cas A(Fesen,Morse,RAC…)

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