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

Result code in 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>

Result on the web

<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>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

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Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2025

Confidentiality

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

Name of the periodical

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

695

Issue of the periodical within the volume

March

Country of publishing house

FR - FRANCE

Number of pages

14

Pages from-to

A271

UT code for WoS article

001454467100002

EID of the result in the Scopus database

2-s2.0-105016480490