Evolution, nucleosynthesis and yields of low mass AGB stars

By S. Cristallo, O. Straniero, Roberto Gallino, L. Piersanti, I. Domínguez, M. Lederer. 2009

159 citations recorded by the source corpus.

INAF-Osservatorio Astronomico di Collurania, 64100 Teram o, Italy and R. Gallino2,3 Dipartimento di Fisica Generale, Universitá di Torino, 10 125 Torino, Italy Center for Stellar and Planetary Astrophysics, School of Ma thematical Sciences, Monash University, P.O. Box 28, Victoria 3800, Australia and L. Piersanti 1 INAF-Osservatorio Astronomico di Collurania, 64100 Teram o, Italy and I. Domı́nguez4 Departamento de Fı́sica Teórica y del Cosmos , Universidad de Granada, 18071 Granada, Spain and M.T. Lederer 5 Institut für Astronomie, Türkenschanzstraße 17, A-1180 Wien, Austria Received/ Accepted

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2483879dc2b6f0109a98f04e92bb83019e15d6a6

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Karakas
2. M. Lugaro
3. J. Lattanzio
4. A. Bressan
5. L. Girardi
6. S. Cristallo
7. A. Chieffi
8. M. Limongi

Citations in the corpus

• STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, methodology): “Similar considerations were also used by Cristallo et al. (2009) to calibrate the value of the free parameter β that controls the exponential decay of the velocity below the border of the convective envelope in their time-dependent description of overshoot.”
• Evolution of thermally pulsing asymptotic giant branch stars - I. The COLIBRI code (2013, background): “…of stellar structure with the aid of classical 1D stellar evolution codes, are becoming increasingly successful thanks to the speeding-up of modern processors, and to the particular care devoted to the nucleosynthesis (e.g. Ventura, D’Antona & Mazzitelli 2002; Cristallo et al. 2009; Karakas 2010).”
• Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “Cristallo et al. (2009, 2011, 2015a) have constructed evolutionary stellar models coupled to a full nuclear network including all the relevant isotopes, up to the termination point of the s-process path (Pb-Bi).”
• EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF AGB STARS AT DIFFERENT METALLICITIES. III. INTERMEDIATE-MASS MODELS, REVISED LOW-MASS MODELS, AND THE pH-FRUITY INTERFACE (2015, methodology): “This quantity takes into account the poisoning effect of 14N (via the14N(n,p)14C reaction) and, thus, provides a better estimate of the neutrons effectively contributing to the synthesis of heavy elements (see Cristallo et al. 2009).”
• ON THE SOURCE OF THE DUST EXTINCTION IN TYPE Ia SUPERNOVAE AND THE DISCOVERY OF ANOMALOUSLY STRONG Na i ABSORPTION (2013, background): “This is because of the formation of a 13C pocket, a necessary ingredient for the production of s-process elements (see e.g., Mowlavi 1999; Cristallo et al. 2009; Karakas 2010).”
• The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, methodology): “2M⊙, regardless of Z (see also Cristallo et al. 2009; Lugaro et al. 2012).”