Green's electron function in a quantized plane wave field

Khokhlov, I. A.

doi:10.1007/bf00898886

Cited by 2 publications

(2 citation statements)

References 3 publications

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“…The burning of C and O under degenerate conditions can be described by three stages. First, C is consumed producing reaction products close to Mg. Then O is consumed along with the ashes of C burning, which produces a mixture of silicon group and light elements that is in a statistical quasi-equilibrium [59,60,61]. Finally the silicon-group nuclei are converted to IGEs, reaching full nuclear statistical equilibrium (NSE).…”

Section: Simulation Instrumentmentioning

confidence: 99%

Cosmic Chandlery with Thermonuclear Supernovae

Calder¹,

Krueger²,

Jackson³

et al. 2017

J. Phys.: Conf. Ser.

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Thermonuclear (Type Ia) supernovae are bright stellar explosions, the light curves of which can be calibrated to allow for use as "standard candles" for measuring cosmological distances. Contemporary research investigates how the brightness of an event may be influenced by properties of the progenitor system that follow from properties of the host galaxy such as composition and age. The goals are to better understand systematic effects and to assess the intrinsic scatter in the brightness, thereby reducing uncertainties in cosmological studies. We present the results from ensembles of simulations in the single-degenerate paradigm addressing the influence of age and metallicity on the brightness of an event and compare our results to observed variations of brightness that correlate with properties of the host galaxy. We also present results from "hybrid" progenitor models that incorporate recent advances in stellar evolution.

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Section: Simulation Instrumentmentioning

confidence: 99%

Cosmic Chandlery with Thermonuclear Supernovae

Calder¹,

Krueger²,

Jackson³

et al. 2017

J. Phys.: Conf. Ser.

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“…The nuclear processing can be well-approximated as a three stage process: initially C is consumed, followed by O, which creates a mixture of Si group and light elements that is in quasi-statistical equilibrium, also known as nuclear statistical quasi-equilibrium (NSQE) [236][237][238][239][240]); finally the Si-group nuclei are converted to Fe group, reaching full nuclear statistical equilibrium, NSE. In both of these equilibrium states, the capture and creation of light elements (via photodisintegration) is balanced, so that energy release can continue by changing the relative abundance of light (low nuclear binding energy) and heavy (high nuclear binding energy) nuclides, an action that releases energy as buoyant burned material rises and expands.…”

Section: Flame Modelmentioning

confidence: 99%

The influence of chemical composition on models of Type Ia supernovae

et al. 2013

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Type Ia supernovae are bright stellar explosions distinguished by standardizable light curves that allow for their use as distance indicators for cosmological studies. Despite the highly successful use of these events in this capacity, many fundamental questions remain. Contemporary research investigates how properties of the progenitor system that follow from the host galaxy such as composition and age influence the brightness of an event with the goal of better understanding and assessing the intrinsic scatter in the brightness. We provide an overview of these supernovae and proposed progenitor systems, all of which involve one or more compact stars known as white dwarfs. We describe contemporary research investigating how the composition and structure of the progenitor white dwarf systematically influences the explosion outcome assuming the progenitor is a single white dwarf that has gained mass from a companion. We present results illustrating some of these systematic effects from our research.PACS numbers: 97.60. Bw,26.50.+x,97.20.Rp,95.30.Lz

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Green's electron function in a quantized plane wave field

Cited by 2 publications

References 3 publications

Cosmic Chandlery with Thermonuclear Supernovae

Cosmic Chandlery with Thermonuclear Supernovae

The influence of chemical composition on models of Type Ia supernovae

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