Light curves of Type II Supernovae: Metallicity Dependencies.
“Discussion is Welcome... And conclusions may change after discussion”. Cute.
First talk by a member of the Subaru generation. Lots of young energetic Japanese astronomers here.
Light curves of Type IIs... characterized by the envelope mass and pre-sn radius... also metallicity. Type I: by Mej, M Ni, and E. LC Plateu, brighter and longer for larger Menv....
Difference btw SN Ibc and SN II? MS mass? Single vs Binary? Metallicity? Mass loss uncertain.. Can these be constrained just with MColor LCs? Stella, radn hydrocode from Blinnikov et al. Type IIs have weak metal lines and close to BB. Large PreSN radius so Rad Trans important...
Using code, explore effects of Energy, MS mass, and Metallicity. Progenitor models from Umeda & Nomoto 2005, Explosions 1,5,10,20 FOE. MS mass, 13,15, 18,20,25,30, Metallicity ... missed it...
Higher energy makes shorter and brighter plateaus.
Larger MS mass makes brighter and longer plateaus. Some discussion of the difference between input KE and actual result KE. Plateaus seem long... all are above 100 d which is near the long end of observations... Perhaps KE is too low?
Metallicity... Zero metallicity star is compact, but the rest have similar structures... Envelope mass has complicated relation to metallicity... some discussion between those responsible for the input models... Metallicity results: zero metallicity star has 87A-like light curve, Otherwise the trend is relativity weak for metallicities. However colors change significantly. Higher metallicity sne are redder. Higher metallicity means larger photospheric radii (larger opacity). Same structure, but larger radius so cooler.
Looking at shock breakout. For larger PreSN radius, longer shock breakout, higher total energy, but fainter and cooler.
Energy: Higher energies are brighter and bluer.
MS Mass: Larger mass makes the peak longer and color redder. Lifan asks where is Ly Alpha.. Its ionized. Very hot (300K +)
Metallicity: All similar except metal free, spectra very similar as well.. (not surprising if ionization is very high and opacity low.)
Sensitivity for seeing these things in S-Cam on Subaru. 30 Msun at z=2 possible in 1 hr? NIR on JWST, 10 ks observations, 10 sigma.... Discussion of how to find these things...
“Discussion is Welcome... And conclusions may change after discussion”. Cute.
First talk by a member of the Subaru generation. Lots of young energetic Japanese astronomers here.
Light curves of Type IIs... characterized by the envelope mass and pre-sn radius... also metallicity. Type I: by Mej, M Ni, and E. LC Plateu, brighter and longer for larger Menv....
Difference btw SN Ibc and SN II? MS mass? Single vs Binary? Metallicity? Mass loss uncertain.. Can these be constrained just with MColor LCs? Stella, radn hydrocode from Blinnikov et al. Type IIs have weak metal lines and close to BB. Large PreSN radius so Rad Trans important...
Using code, explore effects of Energy, MS mass, and Metallicity. Progenitor models from Umeda & Nomoto 2005, Explosions 1,5,10,20 FOE. MS mass, 13,15, 18,20,25,30, Metallicity ... missed it...
Higher energy makes shorter and brighter plateaus.
Larger MS mass makes brighter and longer plateaus. Some discussion of the difference between input KE and actual result KE. Plateaus seem long... all are above 100 d which is near the long end of observations... Perhaps KE is too low?
Metallicity... Zero metallicity star is compact, but the rest have similar structures... Envelope mass has complicated relation to metallicity... some discussion between those responsible for the input models... Metallicity results: zero metallicity star has 87A-like light curve, Otherwise the trend is relativity weak for metallicities. However colors change significantly. Higher metallicity sne are redder. Higher metallicity means larger photospheric radii (larger opacity). Same structure, but larger radius so cooler.
Looking at shock breakout. For larger PreSN radius, longer shock breakout, higher total energy, but fainter and cooler.
Energy: Higher energies are brighter and bluer.
MS Mass: Larger mass makes the peak longer and color redder. Lifan asks where is Ly Alpha.. Its ionized. Very hot (300K +)
Metallicity: All similar except metal free, spectra very similar as well.. (not surprising if ionization is very high and opacity low.)
Sensitivity for seeing these things in S-Cam on Subaru. 30 Msun at z=2 possible in 1 hr? NIR on JWST, 10 ks observations, 10 sigma.... Discussion of how to find these things...
No comments:
Post a Comment