The bright, dusty aftermath of giant eruptions and H-rich supernovae: Late interaction of supernova shocks and dusty circumstellar shells created by 45, 50, and 60 M⊙ stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00619116" target="_blank" >RIV/67985815:_____/25:00619116 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0365892" target="_blank" >https://hdl.handle.net/11104/0365892</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202449717" target="_blank" >10.1051/0004-6361/202449717</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The bright, dusty aftermath of giant eruptions and H-rich supernovae: Late interaction of supernova shocks and dusty circumstellar shells created by 45, 50, and 60 M⊙ stars

Popis výsledku v původním jazyce

The late-stage evolution of massive stars is marked by periods of intense instability as they transit towards their final corecollapse. Within these periods, stellar eruptions stand out due to their hallmark of exceptionally high mass-loss rates, resulting in the formation of copious amounts of dust. However, the survival of these dust grains is threatened by the powerful shock waves generated when the progenitor star explodes as a supernova (SN). Aims. We aim to assess the impact of selected cases of hydrogen-rich SN explosions from progenitors of 45, 50, and 60 M-circle dot on dust grains formed after giant stellar eruptions, exploring late interactions with circumstellar shells that occur a few years to centuries after the eruption. Methods. We present 3D hydrodynamical simulations that follow the evolution of dust particles in a scenario that includes, for the first time, the progenitor's stellar wind, a giant stellar eruption, and the eventual SN explosion, while in line with the mass budget prescribed by stellar evolutionary models. Results. For a standard SN ejecta mass of 10 M-circle dot, kinetic energy of 10(51) erg, and a long 200-year eruption-SN gap, only 25% of the dust mass remains 250 years post-explosion in a spherical circumstellar medium (CSM), and only 2% a century after the explosion in a bipolar CSM. Conversely, a shorter gap of a dozen years preserves 75% of the dust mass after shock-processing for a standard explosion, while this drops to 20% for more massive (15-20 M-circle dot) ejecta with kinetic energy of 5 x 10(51) erg. Conclusions. The CSM geometry and an early SN remnant transition to a radiative phase impact dust survival. As the shock wave weakens from efficiently converting kinetic energy into thermal radiation (up to half of the injected kinetic energy), there is a greater potential for survival, not only for dust in the CSM but also for SN-condensed dust (due to a weaker SN reverse shock), and pre-existing dust in the ambient ISM. Against expectations, a larger fraction of the dust mass can survive if the SN occurs just a few years after the eruption event.

Název v anglickém jazyce

The bright, dusty aftermath of giant eruptions and H-rich supernovae: Late interaction of supernova shocks and dusty circumstellar shells created by 45, 50, and 60 M⊙ stars

Popis výsledku anglicky

The late-stage evolution of massive stars is marked by periods of intense instability as they transit towards their final corecollapse. Within these periods, stellar eruptions stand out due to their hallmark of exceptionally high mass-loss rates, resulting in the formation of copious amounts of dust. However, the survival of these dust grains is threatened by the powerful shock waves generated when the progenitor star explodes as a supernova (SN). Aims. We aim to assess the impact of selected cases of hydrogen-rich SN explosions from progenitors of 45, 50, and 60 M-circle dot on dust grains formed after giant stellar eruptions, exploring late interactions with circumstellar shells that occur a few years to centuries after the eruption. Methods. We present 3D hydrodynamical simulations that follow the evolution of dust particles in a scenario that includes, for the first time, the progenitor's stellar wind, a giant stellar eruption, and the eventual SN explosion, while in line with the mass budget prescribed by stellar evolutionary models. Results. For a standard SN ejecta mass of 10 M-circle dot, kinetic energy of 10(51) erg, and a long 200-year eruption-SN gap, only 25% of the dust mass remains 250 years post-explosion in a spherical circumstellar medium (CSM), and only 2% a century after the explosion in a bipolar CSM. Conversely, a shorter gap of a dozen years preserves 75% of the dust mass after shock-processing for a standard explosion, while this drops to 20% for more massive (15-20 M-circle dot) ejecta with kinetic energy of 5 x 10(51) erg. Conclusions. The CSM geometry and an early SN remnant transition to a radiative phase impact dust survival. As the shock wave weakens from efficiently converting kinetic energy into thermal radiation (up to half of the injected kinetic energy), there is a greater potential for survival, not only for dust in the CSM but also for SN-condensed dust (due to a weaker SN reverse shock), and pre-existing dust in the ambient ISM. Against expectations, a larger fraction of the dust mass can survive if the SN occurs just a few years after the eruption event.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

695

Číslo periodika v rámci svazku

March

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

14

Strana od-do

A271

Kód UT WoS článku

001454467100002

EID výsledku v databázi Scopus

2-s2.0-105016480490