The metamorphosis of the Type Ib SN 2019yvr: late-time interaction

Ferrari, Lucía, Folatelli, Gastón, Kuncarayakti, Hanindyo, Stritzinger, Maximilian, Maeda, Keiichi, Bersten, Melina, Román Aguilar, Lili M., Sáez, M Manuela, Dessart, Luc, Lundqvist, Peter, Mazzali, Paolo, Nagao, Takashi, Ashall, Chris, Bose, Subhash, Brennan, Seán J., Cai, Yongzhi, Handberg, Rasmus, Holmbo, Simon, Karamehmetoglu, Emir, Pastorello, Andrea, Reguitti, Andrea, Anderson, Joseph, Chen, Ting-Wan, Galbany, Lluís, Gromadzki, Mariusz, Gutiérrez, Claudia P., Inserra, Cosimo ORCID: https://orcid.org/0000-0002-3968-4409, Kankare, Erkki, Müller Bravo, Tomás E., Mattila, Seppo, Nicholl, Matt, Pignata, Giuliano, Sollerman, Jesper, Srivastav, Shubham and Young, David R. 2024. The metamorphosis of the Type Ib SN 2019yvr: late-time interaction. Monthly Notices of the Royal Astronomical Society: Letters 529 (1) , L33–L40. 10.1093/mnrasl/slad195

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Abstract

We present observational evidence of late-time interaction between the ejecta of the hydrogen-poor Type Ib supernova (SN) 2019yvr and hydrogen-rich circumstellar material (CSM), similar to the Type Ib SN 2014C. A narrow H α emission line appears simultaneously with a break in the light-curve decline rate at around 80–100 d after explosion. From the interaction delay and the ejecta velocity, under the assumption that the CSM is detached from the progenitor, we estimate the CSM inner radius to be located at ∼6.5–9.1 × 1015 cm. The H α emission line persists throughout the nebular phase at least up to +420 d post-explosion, with a full width at half maximum of ∼2000 km s−1. Assuming a steady mass-loss, the estimated mass-loss rate from the luminosity of the H α line is ∼3–7 × 10−5 M⊙ yr−1. From hydrodynamical modelling and analysis of the nebular spectra, we find a progenitor He-core mass of 3–4 M⊙, which would imply an initial mass of 13–15 M⊙. Our result supports the case of a relatively low-mass progenitor possibly in a binary system as opposed to a higher mass single star undergoing a luminous blue variable phase.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Publisher:	Oxford University Press
ISSN:	1745-3925
Date of First Compliant Deposit:	26 January 2024
Date of Acceptance:	12 December 2023
Last Modified:	31 Jan 2024 10:01
URI:	https://orca.cardiff.ac.uk/id/eprint/165866

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