The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs
Calcium-rich explosions are very faint ( M _B ∼ −15.5), type I supernovae (SNe) showing strong Ca lines, mostly observed in old stellar environments. Several models for such SNe have been explored and debated, but none were able to reproduce consistently the observed properties of Ca-rich SNe, nor t...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acaf65 |
| _version_ | 1797697278423597056 |
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| author | Yossef Zenati Hagai B. Perets Luc Dessart Wynn V. Jacobson-Galán Silvia Toonen Armin Rest |
| author_facet | Yossef Zenati Hagai B. Perets Luc Dessart Wynn V. Jacobson-Galán Silvia Toonen Armin Rest |
| author_sort | Yossef Zenati |
| collection | DOAJ |
| description | Calcium-rich explosions are very faint ( M _B ∼ −15.5), type I supernovae (SNe) showing strong Ca lines, mostly observed in old stellar environments. Several models for such SNe have been explored and debated, but none were able to reproduce consistently the observed properties of Ca-rich SNe, nor their rates and host-galaxy distributions. Here we show that the disruptions of low-mass carbon–oxygen (CO) white dwarfs (WDs) by hybrid helium–CO (HeCO) WDs during their merger could explain the origin and properties of such SNe. We make use of detailed multidimensional hydrodynamical-thermonuclear ( FLASH ) simulations to characterize such explosions. We find that the accretion of CO material onto an HeCO-WD heats its He shell and eventually leads to its “weak” detonation and ejection and the production of a sub-energetic ∼10 ^49 erg Ca-rich SN, while leaving the CO core of the HeCO-WD intact as a hot remnant WD, possibly giving rise to X-ray emission as it cools down. We model the detailed light curves and spectra of such explosions and find excellent agreement with the observations of Ia/c Ca-rich, and potentially Ib Ca-rich, SNe. We thereby provide a viable, consistent model for the origins of Ca-rich SNe. These findings can shed new light on the role of Ca-rich SNe in the chemical evolution of galaxies and the intracluster medium, and their contribution to the observed 511 Kev signal in the galaxy originating from positrons produced from ^44 Ti decay. Finally, the origins of such SNe points to the key role of HeCO-WDs as SN progenitors and their potential role as progenitors of other thermonuclear SNe including normal Ia. |
| first_indexed | 2024-03-12T03:38:03Z |
| format | Article |
| id | doaj.art-bbc99ef9a7ba49c78252fe28d47a2065 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:38:03Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-bbc99ef9a7ba49c78252fe28d47a20652023-09-03T13:07:59ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194412210.3847/1538-4357/acaf65The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White DwarfsYossef Zenati0https://orcid.org/0000-0002-0632-8897Hagai B. Perets1https://orcid.org/0000-0002-5004-199XLuc Dessart2https://orcid.org/0000-0003-0599-8407Wynn V. Jacobson-Galán3https://orcid.org/0000-0002-3934-2644Silvia Toonen4https://orcid.org/0000-0002-2998-7940Armin Rest5https://orcid.org/0000-0002-4410-5387Physics and Astronomy Department, Johns Hopkins University , Baltimore, MD, 21218, USA ; yzenati1@jhu.edu, hperets@physics.technion.ac.il; Technion—Israel Institute of Technology , Physics department, Haifa 3200002 IsraelTechnion—Israel Institute of Technology , Physics department, Haifa 3200002 IsraelInstitut d’Astrophysique de Paris, CNRS-Sorbonne Université , 98 bis boulevard Arago, F-75014 Paris, FranceDepartment of Astronomy and Astrophysics, University of California , Berkeley, CA, 94720, USAAnton Pannekoek Institute for Astronomy, University of Amsterdam , 1090 GE Amsterdam, The NetherlandsPhysics and Astronomy Department, Johns Hopkins University , Baltimore, MD, 21218, USA ; yzenati1@jhu.edu, hperets@physics.technion.ac.il; Space Telescope Science Institute , 3700 San Martin Dr., Baltimore, MD, 21218, USACalcium-rich explosions are very faint ( M _B ∼ −15.5), type I supernovae (SNe) showing strong Ca lines, mostly observed in old stellar environments. Several models for such SNe have been explored and debated, but none were able to reproduce consistently the observed properties of Ca-rich SNe, nor their rates and host-galaxy distributions. Here we show that the disruptions of low-mass carbon–oxygen (CO) white dwarfs (WDs) by hybrid helium–CO (HeCO) WDs during their merger could explain the origin and properties of such SNe. We make use of detailed multidimensional hydrodynamical-thermonuclear ( FLASH ) simulations to characterize such explosions. We find that the accretion of CO material onto an HeCO-WD heats its He shell and eventually leads to its “weak” detonation and ejection and the production of a sub-energetic ∼10 ^49 erg Ca-rich SN, while leaving the CO core of the HeCO-WD intact as a hot remnant WD, possibly giving rise to X-ray emission as it cools down. We model the detailed light curves and spectra of such explosions and find excellent agreement with the observations of Ia/c Ca-rich, and potentially Ib Ca-rich, SNe. We thereby provide a viable, consistent model for the origins of Ca-rich SNe. These findings can shed new light on the role of Ca-rich SNe in the chemical evolution of galaxies and the intracluster medium, and their contribution to the observed 511 Kev signal in the galaxy originating from positrons produced from ^44 Ti decay. Finally, the origins of such SNe points to the key role of HeCO-WDs as SN progenitors and their potential role as progenitors of other thermonuclear SNe including normal Ia.https://doi.org/10.3847/1538-4357/acaf65Type Ia supernovaeWhite dwarf starsHydrodynamical simulations |
| spellingShingle | Yossef Zenati Hagai B. Perets Luc Dessart Wynn V. Jacobson-Galán Silvia Toonen Armin Rest The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs The Astrophysical Journal Type Ia supernovae White dwarf stars Hydrodynamical simulations |
| title | The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs |
| title_full | The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs |
| title_fullStr | The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs |
| title_full_unstemmed | The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs |
| title_short | The Origins of Calcium-rich Supernovae From Disruptions of CO White Dwarfs by Hybrid He–CO White Dwarfs |
| title_sort | origins of calcium rich supernovae from disruptions of co white dwarfs by hybrid he co white dwarfs |
| topic | Type Ia supernovae White dwarf stars Hydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/acaf65 |
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