The outcome of explosive ignition of ONeMg cores - Supernovae, neutron stars, or 'iron' white dwarfs?

Isern, J.; Canal, R.; Labay, J.

doi:10.1086/186029

Cited by 76 publications

(89 citation statements)

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“…For these reasons we favor the scenario of WD0433+270 being a Fe-core white dwarf. The existence of white dwarfs with such core compositions could have important consequences for white dwarf formation models and also for the theories of core collapse and explosion of degenerate nuclei (Isern et al 1991).…”

Section: Current Status Of the Projectmentioning

confidence: 99%

Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

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A mis padres y hermana AgraïmentsEn primer lloc vull agrair als meus directors de tesi, Jordi Isern i Enrique García-Berro, que em donessin l'oportunitat de realitzar el doctorat a l'IEEC (al CSIC i a la UPC), així com que em proporcionessin tot el suport necessari. Crec que he après moltes coses importants en aquestsúltims anys, no només en la part científica, i això en partés una conseqüència d'haver treballat amb ells. Els vull donar les gràcies també pel suport i la confiança dipositada en mi, especialment durant aquestúltim any de feina.Durant tota aquestaèpoca he tingut la sort de tenir uns companys fantàstics que m'han fet molt més fàcil la feina. Primer vaig conèixer l'Alina, la meva companya de "fatigas" i després el Jose, el Pep i el Miquel. Més tard s'hi van afegir l'Ignasi, la Violeta, l'Anna C., l'Anna A., el Carlo, el Moi, el Nil, l'Anaïs. . . Tots els moments que hem compartit dins i fora de l'IEEC han estat molt importants per a mi i m'emporto un gran record de tota aquestaèpoca, primer al Nexus, després a la UAB i finalment a l'ETSE. Ara que tinc la oportunitat, els hi vull agrair als meus companys, o més ben dit, amics, tots elsànims i suport que m'han donat. També els hi vull donar les gràcies al personal d'administració i a la resta de companys que he tingut durant aquests anys.En especial, l'Ignasi es mereix un gran gràcies. . . Primer de tot, per venir a l'IEEC en un moment en que la meva feina necessitava d'un observador amb experiència. Per tenir la generositat de compartir els seus coneixements amb mi durant aquests anys, per acompanyar-me en les observacions, per tenir sempre tanta confiança en mi, molta més que jo mateixa i per ajudar-me sempre que se li presentés la oportunitat. Els seusànims i el seu suport han estat essencials per a que arribés aquest moment i per tant, només em queda donar-li el meu agraïment més sincer.También le debo un agradecimiento especial a Carlos Allende Prieto, que sin ni siquiera conocerme en persona aceptó acompañarme a observar al McDonald Observatory durante 10 días. Su ayuda y dedicación en la distancia, especialmente en el análisis de las compañeras de las enanas blancas, han sido también vitales para el desarrollo de esta tesis.Durante mi doctorado he tenido la oportunidad de disfrutar de estancias en otros centros. Le quiero dar las gracias a Inma Domínguez, Carlos Abia y Olga Zamora de la Universidad de Granada por la atención que me dispensaron cuando estuve allí. También quisiera dar las gracias a Roberto Silvotti y Juan Alcalá por la ayuda y el buen trato que me dieron durante el tiempo que pasé en el Osservatorio Astronomico di Capodimonte. Gracias también al resto de personas que trabajan en el Osservatorio y que hicieron mi estancia muy agradable.A mi profesor Manolo Segura le quiero agredecer que en su día me hiciera creer en mis posibilidades y despertara mi afán por intentar superarme poco a poco. Muchas gracias también por la "contingencia" y por la confianza dipositada en mí.En un momento para mí tan importante comoéste no me puedo olvi...

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Section: Current Status Of the Projectmentioning

confidence: 99%

Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

View full text Add to dashboard Cite

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“…Perhaps the most important works highlighting and addressing some of the questions surrounding the O deflagration phase in ECSNe and the AIC of ONe WDs are Nomoto & Kondo (1991), Isern et al (1991), Canal et al (1992) and Timmes & Woosley (1992). Nomoto & Kondo (1991) showed that for an ONe core with a central ignition density of 9.95×10 9 g cm −3 , the A72, page 2 of 11 distinction between core collapse and thermonuclear explosion lay with the speed of the convective or turbulent deflagration wave, for which a time-dependent formulation of mixing length theory (MLT) was used in their 1D models.…”

Section: Introductionmentioning

confidence: 99%

“…1). Isern et al (1991) also reported that if the O deflagration were to enter the turbulent burning regime, it could result in either the complete disruption of the ONe core/WD or in the partial ejection of material, leaving behind a bound remnant composed of O, Ne and Fe-group elements. Isern et al used the parameterisation suggested by Woosley (1986) for the speed of a turbulent flame as the propagation speed of the O deflagration, with the two free parameters set to the estimates given by Woosley (1986) together with the formula.…”

Section: Introductionmentioning

confidence: 99%

Do electron-capture supernovae make neutron stars?

Jones

Roepke

Pakmor

et al. 2016

A&A

130

207

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Context. In the classical picture, electron-capture supernovae and the accretion-induced collapse of oxygen-neon white dwarfs undergo an oxygen deflagration phase before gravitational collapse produces a neutron star. These types of core collapse events are postulated to explain several astronomical phenomena. In this work, the oxygen deflagration phase is simulated for the first time using multidimensional hydrodynamics. Aims. By simulating the oxygen deflagration with multidimensional hydrodynamics and a level-set-based flame approach, new insights can be gained into the explosive deaths of 8−10 M stars and oxygen-neon white dwarfs that accrete material from a binary companion star. The main aim is to determine whether these events are thermonuclear or core-collapse supernova explosions, and hence whether neutron stars are formed by such phenomena. Methods. The oxygen deflagration is simulated in oxygen-neon cores with three different central ignition densities. The intermediate density case is perhaps the most realistic, being based on recent nuclear physics calculations and 1D stellar models. The 3D hydrodynamic simulations presented in this work begin from a centrally confined flame structure using a level-set-based flame approach and are performed in 256 3 and 512 3 numerical resolutions. Results. In the simulations with intermediate and low ignition density, the cores do not appear to collapse into neutron stars. Instead, almost a solar mass of material becomes unbound from the cores, leaving bound remnants. These simulations represent the case in which semiconvective mixing during the electron-capture phase preceding the deflagration is inefficient. The masses of the bound remnants double when Coulomb corrections are included in the equation of state, however they still do not exceed the effective Chandrasekhar mass and, hence, would not collapse into neutron stars. The simulations with the highest ignition density (log 10 ρ c = 10.3), representing the case where semiconvective mixing is very efficient, show clear signs that the core will collapse into a neutron star.

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“…Miyaji et al 1980;Hillebrandt et al 1984;Ray et al 1984;Burrows & Lattimer 1985), and the field is still active (e.g. Isern et al 1991;Gutierrez et al 1996;Wanajo et al 2003). In the 80's, Nomoto and collaborators (Hillebrandt et al 1984;Nomoto 1984Nomoto , 1987Miyaji & Nomoto 1987;Hashimoto et al 1993) explored in more detail the mass range 9−12 M , investigating the evolution of 2.4 M and 2.6 M "helium balls" up to the first stages of core cooling after central carbon exhaustion and the evolution of a 2.2 M "helium ball" from central helium burning to the shock bounce following core collapse.…”

Section: Introductionmentioning

confidence: 99%

Evolution of massive AGB stars

Siess¹

2006

A&A

219

273

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We present new computations of the evolution of solar metallicity stars in the mass range 9−12 M . This first paper of a series focuses on the propagation of the carbon burning flame front and provides a detailed analysis of the structural evolution up to the formation of the neonoxygen core. Our calculations which do not include overshooting indicate that off-center carbon ignition is restricted to a small mass range between 9.0 and 11.3 M . The chemical imprints of the first and second dredge-ups on the surface composition are analyzed and compared to "standard" less massive stars. It results that, aside from being more luminous and slightly bluer in the HR diagram, massive AGB stars are almost indistinguishable from their lower mass counterparts, as far as the chemical composition is concerned. During the second dredge-up, we note however that the envelope penetrates deeper into the He burning shell than lower mass stars. Our simulations indicate that above ∼11.0 M , the depth of the second dredge up is considerably reduced, marking the transition between low and massive stars. We also investigate the effects of the nuclear uncertainties associated with 12 C + 12 C reactions and show that it has a little impact on the core composition. Finally we describe the nucleosynthesis and chemical structure of the newly formed neon-oxygen core.

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The outcome of explosive ignition of ONeMg cores - Supernovae, neutron stars, or 'iron' white dwarfs?

Cited by 76 publications

References 0 publications

Testing the Initial–Final Mass Relationship of White Dwarfs

Testing the Initial–Final Mass Relationship of White Dwarfs

Do electron-capture supernovae make neutron stars?

Evolution of massive AGB stars

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