CSIRO PUBLISHING Publications of the Astronomical Society of Australia, 2009, 26, 168–175 www.publish.csiro.au/journals/pasa Extra-Mixing in Luminous Cool Red Giants: Hints from Evolved Stars With and Without Li R. GuandaliniA,B,D, S. PalmeriniA,B, M. BussoA,B, and S. UttenthalerC A Dipartimento di Fisica, Università degli Studi di Perugia, via Pascoli, 06123 Perugia, Italy B INFN Sezione di Perugia, via Pascoli, 06123 Perugia, Italy C Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200D, 3000 Leuven, Belgium D Corresponding author. Email: guandalini@fisica.unipg.it Received 2008 December 8, accepted 2009 May 25 Abstract: We present an analysis of Li abundances in low mass stars (LMS) during the Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB) stages, based on a new determination of their luminosities and evolutionary status. By applying recently suggested models for extra-mixing, induced by magnetic buoy- ancy, we show that both Li-rich and Li-poor stars can be accounted for. The simplest scenario implies the development of fast instabilities on the RGB, where Li is produced. When the fields increase in strength, buoyancy slows down and Li is destroyed. 3He is consumed, at variable rates. The process continues on the AGB, where however moderate mass circulation rates have little effect on Li due to the short time available. O-rich and C-rich stars show different histories of Li production/destruction, possibly indicative of different masses. More complex transport schemes are allowed by magnetic buoyancy, with larger effects on Li, but most normal LMS seem to show only the range of Li variation discussed here. Keywords: nuclear reactions, nucleosynthesis, abundances — stars: AGB — stars: evolution — stars: red giants 1 Introduction in the luminosity function. This is the so-called ‘L-bump Most K-type giants are depleted in lithium. For low- phase’. metallicity objects an upper limit on the Li content was Any slow mixing process occurring at or after the L- set by Gratton et al. (2000), stating that field, metal-poor bump would further reduce not only Li, but also 9Be 3 (hence low-mass) stars on the upper RGB have log εLi ≤ 0. and He (Sackmann & Boothroyd 1999), as confirmed Mixing processes on the Main Sequence and up to by observations (Castilho 2000). However, a few red the first dredge-up imply that Li be gradually carried giants (about 2%) show enhanced Li abundances, at levels down from the photosphere to regions of high tempera- sometimes higher than in the present interstellar medium 7 ture and destroyed, while any amount of Be produced (log εLi 3.3). Various explanations have been attempted, by H burning burns ‘on the flight’ and new Li is not pro- the most common assumption being that some form of duced. The observations of Li-poor red giants are therefore fast extra-mixing might transport 7Be from above the well understood. It was further established three decades H-burning shell to the envelope at a speed sufficient to ago (Sweigart & Mengel 1979) and supported by many overcome the rate of p-captures; this is the so-called observations (e.g. Gilroy 1989; Gilroy & Brown 1991; Cameron–Fowler mechanism (Cameron & Fowler 1971). Kraft 1994) that, after the first dredge-up, low mass stars Further production of 7Be along the path can also occur must experience other mixing episodes, sufficiently slow (Sackmann & Boothroyd 1999). Very often, the cause of to gradually carry to the surface a considerable amount such extra-mixing was looked after in the stellar rotation, of 13C, so that the 12C/13C ratio decreases from 25–30 at inducing shear instabilities, meridional circulation and the first dredge-up, down to 12–15 (in Population I stars) diffusion phenomena (Charbonnel 1994; Charbonnel & or to 4–8 (in Population II red giants). The occurrence of Do Nascimiento 1998; Denissenkov & VandenBerg 2003; these mixing phenomena is made easy by the fact that, Palacios et al. 2003). These possibilities were frustrated by after dredge-up, the H-burning shell advances in a homo- the understanding that the stellar structure reacts to rota- geneous region, so that the natural barrier opposed to mass tional distortions too quickly to induce significant mixing transport by a chemical stratification is not present. The on long time scales (Palacios et al. 2006). onset of this phase is accompanied by a local decrease in Recently, two old ideas on mass transport have been the luminosity, followed by a new rise, so that the same revisited, looking for alternative causes of deep circulation regions in the H–R diagram are crossed repeatedly and the in stars. Both attribute mass transport to the presence, in points representing coeval stars pile up, producing a bump deep layers, of materials lighter than in the envelope. The © Astronomical Society of Australia 2009 10.1071/AS08063 1323-3580/09/03168 Downloaded from https://www.cambridge.org/core. IP address: 170.106.34.90, on 01 Oct 2021 at 06:22:11, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1071/AS08063 Extra-Mixing in Luminous Cool Red Giants 169 first mechanism (thermohaline diffusion) attributes this to the activation of the reaction 3He + 3He → 4He + 2p (Eggleton, Dearborn & Lattanzio 2006), reducing the molecular weight. The second process is the buoyancy of magnetized H-burning ashes (Busso et al. 2007a; Wasserburg & Busso 2008; Nordhaus et al. 2008), based on the fact that magnetic bubbles are lighter than the envi- ronment, due to the unbalance generated by magnetic pres- sure (B2/8π). This requires a magnetic dynamo to occur in red giants, as indeed observed (Andrews et al. 1988). Triggering these mechanisms requires specific condi- tions: the first one needs a suitable molecular weight inver- sion; the second is possible if strong magnetic fields exist. The two processes might be complementary and even occur together (Denissenkov, Pinsonneault & MacGregor Figure 1 The bolometric correction for C stars, as a function of 2009). However, while thermohaline mixing implies a the infrared color K-[12.5]. diffusive, slow transport, magnetic buoyancy can occur at different speeds, depending on the amount of heat exchange with the environment (Denissenkov et al. 2009). Therefore, a possibility of understanding which mech- anism is at play might be provided by observations of nuclei, like Li, for which the production and destruction are sensitive to the mixing velocity. Such a test requires an accurate calibration of the lumi- nosity of Li-bearing stars, in order to attribute them to the proper evolutionary stage. Therefore, we here apply bolometric corrections for evolved stars, as derived in our recent work, to infer the absolute HR diagram of red giants showing Li in their spectrum. This helps in setting constraints on where extra-mixing is active. In Sec- tion 2 we present a sample of cool red giants showing highly dispersed Li abundances, ranging from very Li- rich to very Li-poor, and we determine for them absolute magnitudes with the help of our bolometric corrections Figure 2 The bolometric correction for O-rich stars, derived from and of recent distance estimates. In Section 3 we com- MS- and S-type red giants, as a function of the infrared color pare the inferred magnitudes with the Li content, as taken K-[12.5]. from the literature and we present results of nucleosynthe- sis and mixing calculations, using the transport velocities parameters, thus offering calibrating tools to evolution- suggested by magnetic buoyancy. Finally, in Section 4 ary models. In this framework, large samples of C-rich, preliminary conclusions are illustrated. S-type and M-type AGB stars were collected and stud- ied. The first results were published for carbon-rich and 2 Bolometric Corrections and Li Abundances S-type stars in Guandalini & Busso (2008); Busso et al. in Red Giants (2007b); Guandalini et al. (2006). In Figures 1 and 2 we Any growth in our understanding of AGB stars is today present the bolometric corrections we derived for samples bound to improvements on two crucial parameters: lumi- of galactic C-rich and O-rich (S-type) stars, respectively. nosities and mass loss rates. For both, determinations are The techniques adopted and the source properties are hampered by the large distance uncertainties; both are also described in Guandalini et al. (2006) and in Guandalini & affected by the fact that most of the radiation emitted by Busso (2008). these sources can be observed only at infrared wavelengths For the purposes of the present work we use the bolo- and therefore depends on space-borne facilities, or maybe metric corrections of Figures 1 and 2, applying them on the exploitation of special ground-based locations, like to a sample of AGB stars showing highly dispersed Li Antarctica (Guandalini, Tosti & Busso 2008). abundances (from Li-rich to Li-poor). For these sources In the last years we performed an extensive analy- we determine the apparent bolometric magnitude and we sis of the photometric properties of AGB stars, using use the recent revision of the Hipparcos catalogue (van available infrared data from the ISO and MSX experi- Leeuwen 2007), to infer the absolute magnitude. TheAGB ments and looking for relations between their luminosities stars considered, their magnitudes and their Li abundances and their main chemical and physical parameters. The are shown in Table 1. In Table 2 we present a second aim of this work was to put constraints on basic stellar sample, made of RGB stars. The bolometric magnitudes Downloaded from https://www.cambridge.org/core. IP address: 170.106.34.90, on 01 Oct 2021 at 06:22:11, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms.