Mixing fraction in classical novae

Guo, Yunlang; Wu, Chenjie; Wang, Bo

doi:10.1051/0004-6361/202142163

Cited by 8 publications

(5 citation statements)

References 56 publications

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“…There have been numerous MESA studies of various properties of classical nova systems (e.g., Denissenkov et al 2013;Wolf et al 2013;Denissenkov et al 2014;Wolf et al 2018;Chen et al 2019;Ginzburg & Quataert 2021;Leung & Siegert 2022;Guo et al 2022), but the present work is the first to use it to study hydrodynamical nova outflows. We outline our simulations in Section 2 and describe our results in Section 3.…”

Section: Introduction and The Physics Of Classical Nova Outburstsmentioning

confidence: 99%

Binary Interaction Dominates Mass Ejection in Classical Novae

Shen

Quataert

2022

ApJ

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Recent observations suggest our understanding of mass loss in classical novae is incomplete, motivating a new theoretical examination of the physical processes responsible for nova mass ejection. In this paper, we perform hydrodynamical simulations of classical nova outflows using the stellar evolution code MESA. We find that, when the binary companion is neglected, white dwarfs with masses ≳0.8 M ⊙ successfully launch radiation-pressure-driven optically thick winds that carry away most of the envelope. However, for most of the mass-loss phase, these winds are accelerated at radii beyond the white dwarf’s Roche radius assuming a typical cataclysmic variable donor. This means that, before a standard optically thick wind can be formed, mass loss will instead be initiated and shaped by binary interaction. An isotropic, optically thick wind is only successfully launched when the acceleration region recedes within the white dwarf’s Roche radius, which occurs after most of the envelope has already been ejected. The interaction between these two modes of outflow—a first phase of slow, binary-driven, equatorially focused mass loss encompassing most of the mass ejection and a second phase consisting of a fast, isotropic, optically thick wind—is consistent with observations of aspherical ejecta and signatures of multiple outflow components. We also find that isolated lower-mass white dwarfs ≲0.8 M ⊙ do not develop unbound optically thick winds at any stage, making it even more crucial to consider the effects of the binary companion on the resulting outburst.

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Section: Introduction and The Physics Of Classical Nova Outburstsmentioning

confidence: 99%

Binary Interaction Dominates Mass Ejection in Classical Novae

Shen

Quataert

2022

ApJ

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“…Imbriani et al 2004 ;LUNA Collaboration 2006 ). The exact composition of the ejecta depends on the degree of mixing between the accreted envelope and the white dwarf (Casanova et al 2011(Casanova et al , 2016Denissenkov et al 2013 ;Casanova, Jos é & Shore 2018;Guo, Wu & Wang 2022 ) as well as the white dwarf composition. To account for this, we let the abundances of the emitting plasma and the absorber intrinsic to the nova ejecta vary.…”

Section: Nustar Spectroscopymentioning

confidence: 99%

The multiwavelength view of shocks in the fastest nova V1674 Her

Sokolovsky

Johnson

Buson

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Classical novae are shock-powered multi-wavelength transients triggered by a thermonuclear runaway on an accreting white dwarf. V1674 Her is the fastest nova ever recorded (time to declined by two magnitudes is t2 = 1.1 d) that challenges our understanding of shock formation in novae. We investigate the physical mechanisms behind nova emission from GeV γ-rays to cm-band radio using coordinated Fermi-LAT, NuSTAR, Swift and VLA observations supported by optical photometry. Fermi-LAT detected short-lived (18 h) 0.1-100 GeV emission from V1674 Her that appeared 6 h after the eruption began; this was at a level of (1.6 ± 0.4) × 10−6 photons cm−2 s−1. Eleven days later, simultaneous NuSTAR and Swift X-ray observations revealed optically thin thermal plasma shock-heated to kTshock = 4 keV. The lack of a detectable 6.7 keV Fe Kα emission suggests super-solar CNO abundances. The radio emission from V1674 Her was consistent with thermal emission at early times and synchrotron at late times. The radio spectrum steeply rising with frequency may be a result of either free-free absorption of synchrotron and thermal emission by unshocked outer regions of the nova shell or the Razin-Tsytovich effect attenuating synchrotron emission in dense plasma. The development of the shock inside the ejecta is unaffected by the extraordinarily rapid evolution and the intermediate polar host of this nova.

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“…Imbriani et al 2004;LUNA Collaboration et al 2006). The exact composition of the ejecta depends on the degree of mixing between the accreted envelope and the white dwarf (Casanova et al 2011(Casanova et al , 2016(Casanova et al , 2018Denissenkov et al 2013;Guo et al 2022) as well as the white dwarf composition. To account for this, we let the abundances of the emitting plasma and the absorber intrinsic to the nova ejecta vary.…”

Section: Nustar Spectroscopymentioning

confidence: 99%

The multi-wavelength view of shocks in the fastest nova V1674 Her

Sokolovsky,

Johnson,

Buson

et al. 2023

Preprint

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Classical novae are shock-powered multi-wavelength transients triggered by a thermonuclear runaway on an accreting white dwarf. V1674 Her is the fastest nova ever recorded (time to declined by two magnitudes is 2 = 1.1 d) that challenges our understanding of shock formation in novae. We investigate the physical mechanisms behind nova emission from GeV -rays to cm-band radio using coordinated Fermi-LAT, NuSTAR, Swift and VLA observations supported by optical photometry. Fermi-LAT detected short-lived (18 h) 0.1-100 GeV emission from V1674 Her that appeared 6 h after the eruption began; this was at a level of (1.6 ± 0.4) × 10 −6 photons cm −2 s −1 . Eleven days later, simultaneous NuSTAR and Swift X-ray observations revealed optically thin thermal plasma shock-heated to k shock = 4 keV. The lack of a detectable 6.7 keV Fe K emission suggests supersolar CNO abundances. The radio emission from V1674 Her was consistent with thermal emission at early times and synchrotron at late times. The radio spectrum steeply rising with frequency may be a result of either free-free absorption of synchrotron and thermal emission by unshocked outer regions of the nova shell or the Razin-Tsytovich effect attenuating synchrotron emission in dense plasma. The development of the shock inside the ejecta is unaffected by the extraordinarily rapid evolution and the intermediate polar host of this nova.

show abstract

Mixing fraction in classical novae

Cited by 8 publications

References 56 publications

Binary Interaction Dominates Mass Ejection in Classical Novae

Binary Interaction Dominates Mass Ejection in Classical Novae

The multiwavelength view of shocks in the fastest nova V1674 Her

The multi-wavelength view of shocks in the fastest nova V1674 Her

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