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Хохлов, А. В.; Хохлов, В. А.

doi:10.1023/a:1011665417591

Cited by 16 publications

(42 citation statements)

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“…This finding was interpreted as evidence that the initial deflagration flame proceeds in an asymmetric way, having an offset with respect to the explosion centre, in the context of a deflagration‐to‐detonation transition explosion scenario (Khokhlov 1991; Yamaoka et al 1992; Woosley & Weaver 1994; Iwamoto et al 1999; Röpke & Niemeyer 2007; Kasen et al 2009; Seitenzahl et al 2010). Although the details of the ignition process are not yet fully understood, theoretically, an off‐centre ignition may be a natural consequence of the convection within a progenitor white dwarf (Kuhlen, Woosley & Glatzmaier 2006).…”

Section: Asymmetry In Type Ia Snementioning

confidence: 98%

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Effects of the explosion asymmetry and viewing angle on the Type Ia supernova colour and luminosity calibration★

Maeda

Leloudas

Taubenberger

et al. 2011

Monthly Notices of the Royal Astronomical Society

126

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Phenomenological relations exist between the peak luminosity and other observables of type Ia supernovae (SNe Ia) that allow one to standardize their peak luminosities. However, several issues are yet to be clarified: SNe Ia show colour variations after the standardization. Also, individual SNe Ia can show residuals in their standardized peak absolute magnitude at the level of ∼0.15 mag. In this paper, we explore how the colour and luminosity residual are related to the wavelength shift of nebular emission lines observed at ≳150 d after the maximum light. A sample of 11 SNe Ia which likely suffer from little host extinction indicates a correlation (3.3σ) between the peak B−V colour and the late‐time emission‐line shift. Furthermore, a nearly identical relation applies for a larger sample in which only three SNe with B−V≳ 0.2 mag are excluded. Following the interpretation that the late‐time emission‐line shift is a tracer of the viewing direction from which an off‐centre explosion is observed, we suggest that the viewing direction is a dominant factor controlling the SN colour and that a large part of the colour variations is intrinsic, rather than due to the host extinction. We also investigate a relation between the peak luminosity residuals and the wavelength shift in nebular emission lines in a sample of 20 SNe. We thereby found a hint of a correlation (at ∼1.6σ level). The confirmation of this will require a future sample of SNe with more accurate distance estimates. Radiation transfer simulations for a toy explosion model where different viewing angles cause the late‐time emission‐line shift are presented, predicting a strong correlation between the colour and shift, and a weaker one for the luminosity residual.

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Section: Asymmetry In Type Ia Snementioning

confidence: 98%

“…3 3 In the deflagration‐to‐detonation transition scenario, the thermonuclear sparks first trigger the deflagration flames which travel subsonically and then the flames subsequently turn into a supersonic detonation flame (Khokhlov 1991). …”

mentioning

confidence: 99%

Effects of the explosion asymmetry and viewing angle on the Type Ia supernova colour and luminosity calibration★

Maeda

Leloudas

Taubenberger

et al. 2011

Monthly Notices of the Royal Astronomical Society

126

View full text Add to dashboard Cite

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“…INTRODUCTION After decades of study, the mechanism of the explosion of a white dwarf in a Type Ia supernova (SN Ia) remains uncertain (Hillebrandt & Niemeyer 2000). Several of the proposed theoretical models (Arnett 1969;Khokhlov 2001;Reinecke et al 2002) have failed to produce objects with the energetics and chemical composition compatible with observations (Höflich et al 2002). These two characteristics are best captured by the so-called delayed-detonation models (Khokhlov 1991;Gamezo et al 2004;Plewa et al 2004).…”

mentioning

confidence: 99%

“…Several of the proposed theoretical models (Arnett 1969;Khokhlov 2001;Reinecke et al 2002) have failed to produce objects with the energetics and chemical composition compatible with observations (Höflich et al 2002). These two characteristics are best captured by the so-called delayed-detonation models (Khokhlov 1991;Gamezo et al 2004;Plewa et al 2004). In such models, a mild ignition occurs near the center of the accreting, massive white dwarf and sparks a deflagration (subsonic flame).…”

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confidence: 99%

Spectral Signatures of Gravitationally Confined Thermonuclear Supernova Explosions

Kasen

Plewa

2005

ApJ

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We consider some of the spectral and polarimetric signatures of the gravitationally confined detonation scenario for Type Ia supernova explosions. In this model, material produced by an off-center deflagration (which itself fails to produce the explosion) forms a metal-rich atmosphere above the white dwarf surface. Using hydrodynamical simulations, we show that this atmosphere is compressed and accelerated during the subsequent interaction with the supernova ejecta. This leads ultimately to the formation of a high-velocity pancake of metal-rich material that is geometrically detached from the bulk of the ejecta. When observed at the epochs near maximum light, this absorbing pancake produces a highly blueshifted and polarized calcium IR triplet absorption feature similar to that observed in several Type Ia supernovae. We discuss the orientation effects present in our model and contrast them to those expected in other supernova explosion models. We propose that a large sample of spectropolarimetric observations can be used to critically evaluate the different theoretical scenarios.

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“…Paradoxically, both invoke a detonation, which is more violent than a deflagration, but in a lower‐density environment. Pulsational delayed detonation was proposed by Khokhlov (1991). According to this model, the white dwarf fails to explode following the initially slow propagation of the flame, experiencing instead a large pulsation.…”

Section: Introductionmentioning

confidence: 99%

The fate of CO white dwarfs that experience slow deflagrations

Bravo

Domı́nguez

Isern

1999

Monthly Notices of the Royal Astronomical Society

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It has been suggested that the differences among the observational Type Ia supernovae (SNIa) set can be accounted for by invoking two regimes of propagation of combustion. Normal SNIa should be produced by rapid deflagrations that rapidly propagate across a white dwarf, while dim SNIa should be a consequence of a detonation issued during the contraction phase of a pulsation induced by a very slow conductive deflagration. In this paper, we explore the observational consequences of deflagrations, the properties of which are in between both behaviours. Using different laws for the flame velocity as a function of flame radius, a number of different outcomes were found, including direct explosions ejecting small quantities of 56Ni, pulsations leading to recontraction and likely reignition of the flame, and a threshold explosion characterized by an extended gravitationally bound phase (several 103 s), in which most of the white dwarf matter was ejected by the energy input of radioactive isotopes.\ud \ud Not one of these strange supernovae has been detected up to now. Nevertheless, since they are very dim and, for nucleosynthesis reasons, very rare, their existence cannot be excluded. Furthermore, the computed light curve shows that these events mimic the behaviour of peculiar Type II supernovae (SNII), for which reasons there is always the possibility that they have been misclassified as peculiar SNII whose spectrum is lacking.Peer ReviewedPostprint (published version

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Cited by 16 publications

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Effects of the explosion asymmetry and viewing angle on the Type Ia supernova colour and luminosity calibration★

Effects of the explosion asymmetry and viewing angle on the Type Ia supernova colour and luminosity calibration★

Spectral Signatures of Gravitationally Confined Thermonuclear Supernova Explosions

The fate of CO white dwarfs that experience slow deflagrations

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