Where are the double-degenerate progenitors of Type Ia supernovae?
| Autor: | Valeriya Korol, Alberto Rebassa-Mansergas, Santiago Torres, Silvia Toonen |
|---|---|
| Přispěvatelé: | Low Energy Astrophysics (API, FNWI), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica |
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
Astrophysics::High Energy Astrophysical Phenomena
Population Estels binaris FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Double stars 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics education 010303 astronomy & astrophysics Chandrasekhar limit Astrophysics::Galaxy Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Physics education.field_of_study Supernoves 010308 nuclear & particles physics Degenerate energy levels White dwarfs White dwarf Supernovae - general Astronomy and Astrophysics Estels nans Binaries - spectroscopic Galaxy Supernova Supernovae Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Física::Astronomia i astrofísica [Àrees temàtiques de la UPC] White dwarf stars |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, 482(3), 3656-3668. Oxford University Press Monthly Notices of the RAS (0035-8711) Monthly Notices of the RAS (0035-8711), 482(3), 3656-3668 UPCommons. Portal del coneixement obert de la UPC Universitat Politècnica de Catalunya (UPC) Recercat. Dipósit de la Recerca de Catalunya instname |
| ISSN: | 0035-8711 3656-3668 |
| Popis: | Double white dwarf binaries with merger timescales smaller than the Hubble time and with a total mass near the Chandrasekhar limit (i.e. classical Chandrasekhar population) or with high-mass primaries (i.e. sub-Chandrasekhar population) are potential supernova type Ia (SNIa) progenitors. However, we have not yet unambiguously confirmed the existence of these objects observationally, a fact that has been often used to criticise the relevance of double white dwarfs for producing SNIa. We analyse whether this lack of detections is due to observational effects. To that end we simulate the double white dwarf binary population in the Galaxy and obtain synthetic spectra for the SNIa progenitors. We demonstrate that their identification, based on the detection of Halpha double-lined profiles arising from the two white dwarfs in the synthetic spectra, is extremely challenging due to their intrinsic faintness. This translates into an observational probability of finding double white dwarf SNIa progenitors in the Galaxy of (2.1+-1.0)x10^{-5} and (0.8+-0.4)x10^{-5} for the classical Chandrasekhar and the sub-Chandrasekhar progenitor populations, respectively. Eclipsing double white dwarf SNIa progenitors are found to suffer from the same observational effect. The next generation of large-aperture telescopes are expected to help in increasing the probability for detection by ~1 order of magnitude. However, it is only with forthcoming observations such as those provided by LISA that we expect to unambiguously confirm or disprove the existence of double white dwarf SNIa progenitors and to test their importance for producing SNIa. Comment: Re-submitted to MNRAS after applying all referee's suggestions |
| Databáze: | OpenAIRE |
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