The Energy Sources, the Physical Properties, and the Mass-loss History of SN 2017dio
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arXiv
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| Auteurs principaux: | , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866929341288415232 |
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| author | Shi, Deng-Wang Wang, Shan-Qin Gan, Wen-Pei Liang, En-Wei |
| author_facet | Shi, Deng-Wang Wang, Shan-Qin Gan, Wen-Pei Liang, En-Wei |
| contents | We study the energy sources, the physical properties of the ejecta and the circumstellar medium (CSM), as well as the mass-loss history of the progenitor of SN 2017dio which is a broad-lined Ic (Ic-BL) supernova (SN) having unusual light curves (LCs) and signatures of hydrogen-rich CSM in its early spectrum. We find that the temperature of SN 2017dio began to increase linearly about 20 days after the explosion. We use the $^{56}$Ni plus the ejecta-CSM interaction (CSI) model to fit the LCs of SN 2017dio, finding that the masses of the ejecta, the $^{56}$Ni, and the CSM are $\sim$ 12.41 M$_\odot$, $\sim$ 0.17 M$_\odot$, and $\sim$ 5.82 M$_\odot$, respectively. The early-time photosphere velocity and the kinetic energy of the SN are respectively {$\sim$ 1.89 $\times 10^4$ km s$^{-1}$} and $\sim$ 2.66 $\times 10^{52}$ erg, which are respectively comparable to those of SNe Ic-BL and hypernovae (HNe). We suggest that the CSM of SN 2017dio might be {from an luminous-blue-variable-like outburst or} pulsational pair instability $\sim$ 1.2$-$11.4 yr prior to the SN explosion{, or binary mass transfer}. {Moreover,} we find that its ejecta mass is larger than those of many SNe Ic-BL, and that its $^{56}$Ni mass ($M_{\rm Ni}$) is approximately equal to the mean (or median) value of $M_{\rm Ni}$ of SNe Ic-BL in the literature, but lower than $M_{\rm Ni}$ of prototype HNe (e.g., SN 1998bw and SN 2003dh). |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_07485 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Energy Sources, the Physical Properties, and the Mass-loss History of SN 2017dio Shi, Deng-Wang Wang, Shan-Qin Gan, Wen-Pei Liang, En-Wei High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We study the energy sources, the physical properties of the ejecta and the circumstellar medium (CSM), as well as the mass-loss history of the progenitor of SN 2017dio which is a broad-lined Ic (Ic-BL) supernova (SN) having unusual light curves (LCs) and signatures of hydrogen-rich CSM in its early spectrum. We find that the temperature of SN 2017dio began to increase linearly about 20 days after the explosion. We use the $^{56}$Ni plus the ejecta-CSM interaction (CSI) model to fit the LCs of SN 2017dio, finding that the masses of the ejecta, the $^{56}$Ni, and the CSM are $\sim$ 12.41 M$_\odot$, $\sim$ 0.17 M$_\odot$, and $\sim$ 5.82 M$_\odot$, respectively. The early-time photosphere velocity and the kinetic energy of the SN are respectively {$\sim$ 1.89 $\times 10^4$ km s$^{-1}$} and $\sim$ 2.66 $\times 10^{52}$ erg, which are respectively comparable to those of SNe Ic-BL and hypernovae (HNe). We suggest that the CSM of SN 2017dio might be {from an luminous-blue-variable-like outburst or} pulsational pair instability $\sim$ 1.2$-$11.4 yr prior to the SN explosion{, or binary mass transfer}. {Moreover,} we find that its ejecta mass is larger than those of many SNe Ic-BL, and that its $^{56}$Ni mass ($M_{\rm Ni}$) is approximately equal to the mean (or median) value of $M_{\rm Ni}$ of SNe Ic-BL in the literature, but lower than $M_{\rm Ni}$ of prototype HNe (e.g., SN 1998bw and SN 2003dh). |
| title | The Energy Sources, the Physical Properties, and the Mass-loss History of SN 2017dio |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2405.07485 |