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

• Published in: Monthly notices of the Royal Astronomical Society Vol. 529; no. 1; pp. L33 - L40
• Main Authors: 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, Kankare, Erkki, Müller Bravo, Tomás E, Mattila, Seppo, Nicholl, Matt, Pignata, Giuliano, Sollerman, Jesper, Srivastav, Shubham, Young, David R
• Format: Journal Article
• Language: English
• Published: Oxford University Press 2024; Oxford University Press (OUP): Policy P - Oxford Open Option A
• Subjects: Astrophysics; Physics; supernovae: general; supernovae: individual: SN 2019yvr; supernovae: general; supernovae: individual: SN 2019yvr
• DOI: 10.1093/mnrasl/slad195
• EISSN: 1745-3933; 1365-2966
• ISSN: 1745-3925; 0035-8711; 1745-3933

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.