PROGENITOR PULSATION-PHASE DEPENDENCE OF
TYPE IIP LIGHTCURVES (IN 1D)
Jared A. Goldberg* — Interacting Supernovae Contributed Talk
MIAPbP, 27 February 2023
*Flatiron Research Fellow @ CCA, Flatiron Institute, NY, USA
Email: goldberg@ucsb.edu
Web: jaredagoldberg.wordpress.com
Twitter: @aurimontem+2

3THE IMPORTANCE OF PROGENITOR RADIUS FOR IIP’S▸Measure L50, tp and MNi fromthe lightcurve▸Scaling laws yield families ofEjecta Masses and Explosion
Energies, as a function ofRSG Radius.
▸Expansion velocity on theplateau is degenerate withluminosity!
Lightcurve from Szalai et al 2019
Family of explosions from Goldberg & Bildsten 2020 ApJLLightcurve from Szalai et al 2019
Family of explosions from Goldberg & Bildsten 2020 ApJL4

LIGHTCURVE + PROGENITOR RADIUS à EXPLOSION PROPERTIES▸Given a progenitor radius constraint (e.g. HST pre-image), theexplosion energy ejecta mass can be inferred

Bolometric LC & velocities adopted from Szalai et al 2019

Adapted from Goldberg et al 2019, Goldberg & Bildsten 2020 ApJL5

PULSATING RED SUPERGIANTS OBSERVED IN NATURE▸ Wealth of observations: Kiss+2006, Soraisam+18, Yang+18, Ren+19,Chatys+19 and more show RSG pulsations up to ~30% of their radius withperiods of 100s – 1000s days

▸ It only takes a day for a corecollapse explosion: density
structure should be “lockedin” at time of death▸ The explosion should have nopreferred pulsation phase, but
the phase could affect the SNemission (though see slides
from Philipp Podsiadlowski’s
talk in Week 2 for a different
kind of pulsation)

M31: Soraisam et al 2018

6MODELING THE STRUCTURAL EFFECTS OF PULSATIONS (MESA)
Goldberg, Bildsten, & Paxton 2020

▸ At end of core C burning,calculate eigenmodes
using GYRE*

GYRE Pulsation period: 533.7 days
Peak-to-peak:535 days

▸ Inject the velocity

eigenmode into thestellar model at different
times, and allow the starto ring for evolution until
core-collapse▸ Proceed with explosion &SN modeling withMESA**+STELLA****Townsend & Teitler (2013), Townsend+(2018)**Paxton et al (2011, 2013, 2015, 2018, 2019)***Blinnikov+(2004), Baklanov+(2005), Blinnikov+(2006)

MZAMS = 18M☉, Z=0.02

EXPLODING FUNDAMENTAL MODE PULSATORS: BIGGER = BRIGHTER

7‣ Density profile changes with the displacement, but on the plateau, explosions offundamental mode pulsators agree with scaling relations, for fixed Mej and Eexpand varying R with some scatter‣ Differences from the unperturbed model are more extreme at early times and lessextreme at late times (corresponding to the magnitude of the perturbation).

112

Goldberg, Bildsten, & Paxton
2020

760 R☉0 R☉

8OVERTONE VS FUNDAMENTAL‣ Overtone exploded near max will be brighter initially and decline more
rapidly compared to a fundamental pulsation at the same radius‣ Density structure matters!

Goldberg, Bildsten, & Paxton 2020

9“...it just seems like you are focusing on the hippo in the room instead ofthe elephant, and while it's good to take note of the hippo, you should probably
acknowledge and discuss the elephant (although, truth be told, where both co-exist,
the hippo is the more dangerous) -- but, independent of their relative lethality, it is
odd not to discuss the other large mammal in the room.”

REGARDING THE ELEPHANT…

10‣ (Caveat: We do not include the lowest-density material below 10-10 g/cm3)‣ With that (potentially huge) caveat, we do not reproduce the rapid early-timerise with these pulsating structures

From Azalee Boestrom for one of theobjects she’s studying now

C0NCLUSIONS‣ For RSG pulsations primarily in the fundamental mode,the plateau luminosity of the SN scales simply withradius‣ Variability studies are important in determining how
much of an uncertainty this adds to progenitor radiimeasurements from HST pre-imaging‣ Due to the caveats of the existing treatment, interesting
work remains to be done on how pulsation phase
impacts shock breakout and shock-cooling( … in 1D and 3D)11