Prof. Ludwig Jost, For. Mem. R. S

Weiss, F. E.

doi:10.1038/159701b0

Cited by 4 publications

(6 citation statements)

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“…Social support from family and friends was measured by an 1 1-item scale, developed by the first author. The items were based on Weiss's (1974) conceptualization of the functions of social relationships: sharing of concerns, intimacy, opportunity for nurturance, reassurance of worth, and assistance/guidance. Sample items include: "The people important to me accept me as I am" and "When I need someone to help me out, I can usually find someone."…”

Section: Methodsmentioning

confidence: 99%

Work-family strains and gains among two-earner couples

Marshall

Barnett

1993

J. Community Psychol.

224

183

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This paper investigates the sources of work‐family strains and gains in a sample of 300 two‐earner couples. Although most men and women report work‐family gains, not all individuals experienced work‐family strains. Workload and the quality of experiences at work and at home were major predictors of work‐family strains. Experiences at work and at home, social support, and sex‐role attitudes were major predictors of work‐family gains.

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Section: Methodsmentioning

confidence: 99%

Work-family strains and gains among two-earner couples

Marshall

Barnett

1993

J. Community Psychol.

224

183

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“…Although the µ-inversion that we find is somewhat above the main part of the H-burning shell, it is not far above and we can expect some modest processing of 12 C to 13 C and 14 N. According to (18), it appears to be necessary for some extra mixing to take place beyond the point on the RGB where the SCZ has penetrated most deeply; that is exactly the point where our mechanism should start to operate. In (18,19,20,21) it was suggested that rotation in the region between the SCZ and the hydrogen-burning shell might be responsible for the required mixing. We do 9 not dispute the possible importance of rotation; however we emphasise that the mechanism we have discovered is not ad hoc, but simply arises naturally when the modeling is done in 3D.…”

mentioning

confidence: 89%

Deep Mixing of ³ He: Reconciling Big Bang and Stellar Nucleosynthesis

Eggleton

Dearborn

Lattanzio

2006

Science

229

246

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“…Our model 7 makes this very likely. Although the µ-inversion that we find is somewhat above the main part of the H-burning shell, it is not far above and we can expect some modest processing of 12 C to 13 C and 14 N. According to Weiss & Charbonnel (2004), it appears to be necessary for some extra mixing to take place beyond the point on the FGB where the SCZ has penetrated most deeply; that is exactly the point where our mechanism should start to operate.…”

Section: Rayleigh-taylor Instabilitymentioning

confidence: 51%

The destruction of ³He by Rayleigh-Taylor instability on the first giant branch

2006

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Abstract. Low-mass stars, ∼ 1 − 2 solar masses, near the Main Sequence are efficient at producing 3 He, which they mix into the convective envelope on the giant branch and distribute into the Galaxy by way of envelope loss. This process is so efficient that it is difficult to reconcile the observed cosmic abundance of 3 He with the predictions of Big Bang nucleosynthesis. In this paper we find, by modeling a red giant with a fully three-dimensional hydrodynamic code and a full nucleosynthetic network, that mixing arises in the supposedly stable and radiative zone between the hydrogen-burning shell and the base of the convective envelope. This mixing is due to Rayleigh-Taylor instability within a zone just above the hydrogen-burning shell. In this zone the burning of the 3 He left behind by the retreating convective envelope is predominantly by the reaction 3 He + 3 He → 4 He + 1 H + 1 H, a reaction which, untypically for stellar nuclear reactions, lowers the mean molecular weight, leading to a local minimum. This local minimum leads to Rayleigh-Taylor instability, and turbulent motion is generated which will continue ultimately up into the normal convective envelope. Consequently material from the envelope is dragged down sufficiently close to the burning shell that the 3 He in it is progressively destroyed. Thus we are able to remove the threat that 3 He production in low-mass stars poses to the Big Bang nucleosynthesis of 3 He. Some slow mixing mechanism has long been suspected, that connects the convective envelope of a red giant to the burning shell. It appears to be necessary to account for progressive changes in the 12 C/ 13 C and 14 N/ 12 C ratios on the First Giant Branch. We suggest that these phenomena are also due to the Rayleigh-Taylor-unstable character of the 3 He-burning region.

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Prof. Ludwig Jost, For. Mem. R. S

Cited by 4 publications

References 0 publications

Work-family strains and gains among two-earner couples

Work-family strains and gains among two-earner couples

Deep Mixing of ³ He: Reconciling Big Bang and Stellar Nucleosynthesis

The destruction of ³He by Rayleigh-Taylor instability on the first giant branch

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Prof. Ludwig Jost, For. Mem. R. S

Cited by 4 publications

References 0 publications

Work-family strains and gains among two-earner couples

Work-family strains and gains among two-earner couples

Deep Mixing of 3 He: Reconciling Big Bang and Stellar Nucleosynthesis

The destruction of 3He by Rayleigh-Taylor instability on the first giant branch

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Product

Resources

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Deep Mixing of ³ He: Reconciling Big Bang and Stellar Nucleosynthesis

The destruction of ³He by Rayleigh-Taylor instability on the first giant branch