The luminosity-core mass relation - Why and how

Tuchman, Y.; Glasner, Ariella; Barkat, Z.

doi:10.1086/160958

Cited by 17 publications

(20 citation statements)

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“…The increase in the luminosity with decreasing hydrogen mass fraction was also found in analytical studies by Tuchman et al (1983) and with numerical calculations of steady hydrogen burning on white dwarfs by Tuchman & Truran (1998). They studied the dependence of luminosity on the hydrogen mass fraction for a fixed metallicity (Z = 0.25) and for a constant He/H ratio (assumed to be solar, ≈0.1), and summarized their dependences by the relation L(L ) = 5.2 × 10 4 [M c /M − 0.205 − 0.5(X − Z)].…”

Section: Core Mass-luminosity Relationsupporting

confidence: 69%

Models for the soft X-ray emission of post-outburst classical novae

Sala

Hernanz

2005

A&A

120

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Abstract. We developed a hydrostatic and stationary white dwarf envelope model for the study of the post-outburst phases of classical novae and their soft X-ray emission. We considered several white dwarf masses and chemical compositions typical of classical novae. Our results show that the luminosity, maximum effective temperature, and envelope masses depend on the white dwarf mass and on the chemical composition. Envelope masses for which equilibrium solutions exist are pretty small (∼10 −7 −10 −6 M ), thus leading to a short duration of the soft X-ray emitting phase of classical novae, in agreement with most observations. The models we present provide a useful tool for the determination of the white dwarf properties from observable parameters in the X-ray range.

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Section: Core Mass-luminosity Relationsupporting

confidence: 69%

Models for the soft X-ray emission of post-outburst classical novae

Sala

Hernanz

2005

A&A

120

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“…As shown by Refsdal & Weigert (1970) and Tuchman et al (1983), the existence of an M c − L relation requires an inert transition region below the convective envelope where the luminosity remains constant and where the temperature, pressure, density, and radius present a steep dependence on the mass coordinate. In stars experiencing HBB, this transition region is absent because H burning extends into the convective envelope.…”

Section: The Interpulse Phasementioning

confidence: 95%

Evolution of massive AGB stars

Siess

2010

A&A

186

323

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Aims. We present the first simulations of the full evolution of super-AGB stars through the entire thermally pulsing AGB phase. We analyse their structural and evolutionary properties and determine the first SAGB yields.Methods. Stellar models of various initial masses and metallicities were computed using standard physical assumptions which prevents the third dredge-up from occurring. A postprocessing nucleosynthesis code was used to compute the SAGB yields, to quantify the effect of the third dredge-up (3DUP), and to assess the uncertainties associated with the treatment of convection.Results. Owing to their massive oxygen-neon core, SAGB stars suffer weak thermal pulses, have very short interpulse periods and develop very high temperatures at the base of their convective envelope (up to 140 × 10 8 K), leading to very efficient hot bottom burning. SAGB stars are consequently heavy manufacturers of 4 He, 13 C, and 14 N. They are also able to inject significant amounts of 7 Li, 17 O, 25 Mg, and 26,27 Al in the interstellar medium. The 3DUP mainly affects the CNO yields, especially in the lower metallicity models. Our post-processing simulations also indicate that changes in the temperature at the base of the convective envelope, which would result from a change in the efficiency of convective energy transport, have a dramatic impact on the yields and represent another major source of uncertainty.

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“…We see that the FST model achieves a maximum luminosity which is ∼70% larger than the corresponding value of the MLT17 model. This behaviour can be seen as an extreme case of the break-down of the core mass vs. luminosity relation which occurs when the hydrogen burning region is not detached from the convective region (Tuchman et al 1983;Blöcker & Schönberner 1991).…”

Section: The Influence Of the Convective Modelmentioning

confidence: 99%

Full computation of massive AGB evolution

Ventura

D’Antona

2005

A&A

201

235

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Abstract. It is well appreciated that the description of overadiabatic convection affects the structure of the envelopes of luminous asymptotic giant branch (AGB) stars in the phase of "hot bottom burning" (HBB). We stress that this important uncertainty in the modeling plays a role which is much more dramatic than the role which can be ascribed, e.g., to the uncertainty in the nuclear cross-sections. Due to the role tentatively attributed today to the HBB nucleosynthesis as the site of self-enrichment of Globular Clusters stars, it is necessary to explore the difference in nucleosynthesis obtained by different prescriptions for convection. We present results of detailed evolutionary calculations of the evolution of stars of intermediate mass during the AGB phase for the metallicity typical of the Globular Clusters that show the largest spread in CNO abundances (Z ∼ 10 −3 ). We follow carefully the nucleosynthesis at the base of the external convective region, showing that very different results can be obtained according to the presciption adopted to find out the temperature gradient within the instability regions. We discuss the uncertainties in the yields of the various chemical species and the role which these sources can play as polluters of the interstellar medium.

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The luminosity-core mass relation - Why and how

Cited by 17 publications

References 0 publications

Models for the soft X-ray emission of post-outburst classical novae

Models for the soft X-ray emission of post-outburst classical novae

Evolution of massive AGB stars

Full computation of massive AGB evolution

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