The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
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| Format: | Preprint |
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2024
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| author | Ferrari, Lucía Folatelli, Gastón Kuncarayakti, Hanindyo Stritzinger, Maximilian Maeda, Keiichi Bersten, Melina Aguilar, Lili M. Román 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 Bravo, Tomás E. Müller Mattila, Seppo Nicholl, Matt Pignata, Giuliano Sollerman, Jesper Srivastav, Shubham Young, David R. |
| author_facet | Ferrari, Lucía Folatelli, Gastón Kuncarayakti, Hanindyo Stritzinger, Maximilian Maeda, Keiichi Bersten, Melina Aguilar, Lili M. Román 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 Bravo, Tomás E. Müller Mattila, Seppo Nicholl, Matt Pignata, Giuliano Sollerman, Jesper Srivastav, Shubham Young, David R. |
| contents | 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 Hα 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 {\times} 10^{15} cm. The Hα 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. Assuming a steady mass-loss, the estimated mass-loss rate from the luminosity of the Hα line is ~3-7 {\times} 10^{-5} M_\odot yr^{-1}. From hydrodynamical modelling and analysis of the nebular spectra, we find a progenitor He-core mass of 3-4 M{_\odot}, which would imply an initial mass of 13-15 M{_\odot}. 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_15052 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The metamorphosis of the Type Ib SN 2019yvr: late-time interaction Ferrari, Lucía Folatelli, Gastón Kuncarayakti, Hanindyo Stritzinger, Maximilian Maeda, Keiichi Bersten, Melina Aguilar, Lili M. Román 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 Bravo, Tomás E. Müller Mattila, Seppo Nicholl, Matt Pignata, Giuliano Sollerman, Jesper Srivastav, Shubham Young, David R. High Energy Astrophysical Phenomena 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 Hα 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 {\times} 10^{15} cm. The Hα 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. Assuming a steady mass-loss, the estimated mass-loss rate from the luminosity of the Hα line is ~3-7 {\times} 10^{-5} M_\odot yr^{-1}. From hydrodynamical modelling and analysis of the nebular spectra, we find a progenitor He-core mass of 3-4 M{_\odot}, which would imply an initial mass of 13-15 M{_\odot}. 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. |
| title | The metamorphosis of the Type Ib SN 2019yvr: late-time interaction |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2401.15052 |