(Pulsational) Pair-instability
Supernovae
Rob Farmer - MPA
Pablo Marchant - KU Leuven
Mathieu Renzo - CCABound Mass

Example of dynamics during (P)PISN

Log time to final core-collapse

H-rich envelope vs. no envelope

Renzo et al. 2020b

What is a PPISN “pulse”?

What is a “pulse”? Option 1: spike in core T

Not really visible except asbursts of neutrinos,
butNo progenitors in the Local
UniverseRenzo et al. 2020b

What is a “pulse”? Option 2: radial expansion

He, init…but self-generated CSM
may be obscure thisandno progenitors in the Local
Universe

Large radial
oscillation of thebound material
Binary interactions?
Renzo et al. 2020b

Marchant et al. 2019

What is a “pulse”? Option 3: mass loss

M_ejected ≥ 1e-6 Mⵙ
Delta t_ej ≥ t_dynamical

Renzo et al. 2020b

Timing, velocity, and amplitude of pulses

Pulses time-delay

Many outbursts
weeks-months
timescaleRenzo et al. 2020b

Ejecta velocity typically ~1000 km/s

Renzo et al. 2020b

Mass lost per pulse

Renzo et al. 2020b

Renzo et al. 2020b

Nucleosynthesis

Big caveat: approx21.net

Renzo et al. 2020b

, see also Aguado et al. 2023

Connecting GW and EM predictions
and pitfalls in population synthesis implementations

Possible physical reason: time-dependent convection

Take home point:
During dynamical events, the treatment of the time-dependence ofconvection affects the energy budget of the pulse

Renzo et al. 2020a

Possible physical reason: final post-PPI CCSN

See Powell et al. 2021
Rahman et al. 2022The bump at M1~35Mⵙ

Powerlaw+peak fite.g. , Abbott et al. 2022

Hendricks, van Son, Renzo, Izzard (in prep.)Is the bump at ~35Mⵙ related to PPISN?

No Common envelope
evolution
Known non-PPI issueHendricks, van Son, Renzo, Izzard (in prep.)Is the bump at ~35Mⵙ related to PPISN?

No Common envelope
evolution

Is the bump at ~35Mⵙ related to PPISN?

Most massive BH
does not comefrom post-PPI
anymoreHendricks, van Son, Renzo, Izzard (in prep.)

Extra mass loss
is at odds with
3D CCSNesimulations:
M_ej < 3Msun
Powell et al. 2021, Rahman et al. 2021

Is the bump at ~35Msun related to PPISN?

Maybe if
shifting
the PISN
range by~15Msun

Hendricks, van Son, Renzo, Izzard (in prep.)Impact on the predicted SN-rate

Hendricks, van Son, Renzo, Izzard (in prep.)“Super-kilonovae” & Filling the PISN gap from above

Extrapolation of semianalytic long-GRB model

Siegel et al. (incl. Renzo) 2022

Semi-analytic 4-species nucleosynthesis

Siegel et al. (incl. Renzo) 2022

Based on GRMHD from Siegel et al.

Fraction of Keplerian rot. outer layers
Siegel et al. (incl. Renzo) 2022

GW190521
90%-interval

outer/inner boundary for rot. profile

GW signature of Super-kilonova: spiral arms in diskSa
as d tro
M_ mb
BH ongro e:
wsfdecrea

Siegel et al. (incl. Renzo) 2022

ses

Nucleosynthesis
Large ni56 & (light) r-process +Large ejecta masses

Long lasting red light curves

Siegel et al. (incl. Renzo) 2022

EM signature of Super-kilonova Assuming homogeneous ejecta composition

Detectability: Assuming a rate of ~10 /(Gpc^3 yr)
ROMAN: 1-20 superKN to z~1 in 5yr
Rubin/LSST: ~1Siegel et al. (incl. Renzo) 2022

Questions● Can and do binary interaction prevent (P)PISN?
○ And if yes…how?

● Phenomenology of PPI-driven binary interactions?
● Will EM and/or GW find direct evidence of (P)PISN?
○ Rubin/LSST + JWST follow-up○ Odd-even effect?

● Or does nature find a way to avoid (P)PISN?
○ Low-Z stars have little overshooting & swallow all envelope?
○ binary interactions strip too deep/don’t rejuvenate enough?

Spera & Mapelli 2019, di Carlo et al. 2019, 2020, Renzo et al. 2020c, Ballone et al. 2022, Costa et al. 2022

Avoid PPISN with exotic mergers
di Carlo et al. 2019, 2020
Renzo, Cantiello et al. 2020c
Costa et al. 2022
Ballone et al. 2022Fate of the envelope at core-collapse