TY - JOUR
T1 - Radiative Acceleration of Dense Circumstellar Material in Interacting Supernovae
AU - Tsuna, Daichi
AU - Murase, Kohta
AU - Moriya, Takashi J.
N1 - Funding Information:
The authors are deeply indebted to Viktoriya Morozova for early contributions and support in running the SNEC code, and many valuable discussions. The authors also thank the anonymous referee for the insightful comments. D.T. thanks the Pennsylvania State University and YITP at Kyoto University for their hospitality, where this work was mainly done. This work was supported by the JSPS Overseas Challenge Program for Young Researchers, JSPS KAKENHI grant No. JP19J21578, MEXT, Japan, and the Sherman Fairchild Postdoctoral Fellowship at Caltech (D.T.). The work was partly supported by the NSF grant Nos. AST-1908689, AST-2108466, and ST-2108467, and KAKENHI grant Nos. 20H01901 and 20H05852 (K.M.)
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/8/1
Y1 - 2023/8/1
N2 - Early-time light curves/spectra of some hydrogen-rich supernovae (SNe) provide solid evidence of the existence of confined, dense circumstellar matter (CSM) surrounding dying massive stars. We numerically and analytically study the radiative acceleration of CSM in such systems, where the radiation is mainly powered by the interaction between the SN ejecta and the CSM. We find that the acceleration of the unshocked dense CSM ahead of the shock is larger for massive and compact CSM, with velocities reaching up to ∼103 km s−1 for a CSM of order 0.1 M ⊙ confined within ∼1015 cm. We show that the dependence of the acceleration on the CSM density helps us explain the diversity of the CSM velocity inferred from the early spectra of some Type II SNe. For explosions in even denser CSM, radiative acceleration can affect the dissipation of strong collisionless shocks formed after the shock breakout, which would affect early nonthermal emission expected from particle acceleration.
AB - Early-time light curves/spectra of some hydrogen-rich supernovae (SNe) provide solid evidence of the existence of confined, dense circumstellar matter (CSM) surrounding dying massive stars. We numerically and analytically study the radiative acceleration of CSM in such systems, where the radiation is mainly powered by the interaction between the SN ejecta and the CSM. We find that the acceleration of the unshocked dense CSM ahead of the shock is larger for massive and compact CSM, with velocities reaching up to ∼103 km s−1 for a CSM of order 0.1 M ⊙ confined within ∼1015 cm. We show that the dependence of the acceleration on the CSM density helps us explain the diversity of the CSM velocity inferred from the early spectra of some Type II SNe. For explosions in even denser CSM, radiative acceleration can affect the dissipation of strong collisionless shocks formed after the shock breakout, which would affect early nonthermal emission expected from particle acceleration.
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U2 - 10.3847/1538-4357/acdb71
DO - 10.3847/1538-4357/acdb71
M3 - Article
AN - SCOPUS:85166076633
SN - 0004-637X
VL - 952
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 115
ER -