next up previous
Next: The iron abundances of Up: Introduction Previous: Metal line strengths in

Stellar evolution on the asymptotic giant branch: PAGB stars

The majority of stars in the Galaxy are low mass stars, with M tex2html_wrap_inline406 5M tex2html_wrap_inline302 . Unlike the higher mass stars, some aspects of which will be considered later, significant mass loss only occurs in the late stages of stellar evolution, serving to enrich the interstellar medium with the products of nucleosynthesis (He, C, N and O). Because low mass stars constitute such a large majority, knowledge of the last stages of their evolution is of great importance for the study of the evolution of the Galaxy and the interstellar medium (Trams et al. 1989).

On the exhaustion of core hydrogen in such a star, the core contracts and the temperature and pressure just outside the core are sufficiently high for shell hydrogen burning to start. Except for the least massive stars (M tex2html_wrap_inline406 2M tex2html_wrap_inline302 ) (Shu 1981) this takes place partly via the CNO cycle:

tex2html_wrap_inline344 C+ tex2html_wrap_inline306 H tex2html_wrap_inline310 tex2html_wrap_inline420 N+ tex2html_wrap_inline326
tex2html_wrap_inline420 N+ tex2html_wrap_inline426 tex2html_wrap_inline314 tex2html_wrap_inline310 tex2html_wrap_inline420 C+ tex2html_wrap_inline316
tex2html_wrap_inline420 C+ tex2html_wrap_inline306 H tex2html_wrap_inline310 tex2html_wrap_inline376 N+ tex2html_wrap_inline326
tex2html_wrap_inline376 N+ tex2html_wrap_inline306 H tex2html_wrap_inline310 tex2html_wrap_inline452 O+ tex2html_wrap_inline326
tex2html_wrap_inline452 O+ tex2html_wrap_inline426 tex2html_wrap_inline314 tex2html_wrap_inline310 tex2html_wrap_inline452 N+ tex2html_wrap_inline316
tex2html_wrap_inline452 N+ tex2html_wrap_inline306 H tex2html_wrap_inline310 tex2html_wrap_inline334 He+ tex2html_wrap_inline344 C

The star moves off the main sequence and on to the red giant branch (RGB). The stellar radius increases to typically 100 solar radii and the products of stellar nucleosynthesis (primarily He and N, as products of the CNO cycle) begin to appear at the stellar surface. This is the result of the extension of the star setting up a strong convection zone in the outer stellar envelope, which reaches down to the hydrogen burning shell. The surface abundances are modified as follows (Becker & Iben 1979, Trams et al. 1991);

This stage is known as the first dredge-up.

As the core mass increases, the core temperature rises until the onset of core helium burning. In the lower mass stars, this can occur in a violent process known as the helium flash (Zeilik et al. 1992). The star now leaves the RGB and settles on the horizontal branch (HB), in a relatively stable He-burning phase.

When the core helium is exhausted, the core contracts and the star becomes cooler, once again moving to the right on the HR diagram. The star is now on the asymptotic giant branch (AGB), and the outer envelope is strongly convective, leading to the mixing of He and N to the surface in the second dredge-up. Shell hydrogen burning persists and shell helium burning commences. The energy production of this shell is large, causing renewed expansion (Becker & Iben 1979). The helium shell is wholly converted to carbon, and shell hydrogen burning almost stops. The surface abundance changes are similar to those produced in the first dredge-up, with a further enhancement of tex2html_wrap_inline376 N and depletion of tex2html_wrap_inline344 C. Hence stars that have only passed the first dredge-up are not easily distinguished from those that have also undergone the second dredge-up (Trams et al. 1991). However, very low mass stars (M tex2html_wrap_inline406 2M tex2html_wrap_inline302 ) will not pass through a second dredge-up phase.

Hydrogen shell burning once again takes over the energy production of a star on the AGB, as the conditions at the outer boundary of the carbon/oxygen core are not extreme enough for efficient helium shell burning (Trams et al. 1991). Helium will burn sporadically (described as thermal pulsing) via the triple- tex2html_wrap_inline346 process (3 tex2html_wrap_inline334 He tex2html_wrap_inline310 tex2html_wrap_inline344 C+ tex2html_wrap_inline326 ). During these pulses, the star will expand and hydrogen shell burning ceases, while a strong convection zone is again produced bringing further products of nucleosynthesis to the stellar surface in the third dredge-up. The surface abundances are modified as follows:

Hence a star which has passed the third dredge-up should exhibit relative overabundances, with respect to the original chemical composition, of C, N and O, with carbon more abundant than oxygen as it is a direct product of helium burning. For heavier elements, one would expect a decreasing enrichment from tex2html_wrap_inline524 Ne to tex2html_wrap_inline526 S, as the tex2html_wrap_inline346 -capture reaction rates decrease (Lang 1980). Stars will now evolve from the AGB towards higher effective temperatures and are described as post-asymptotic giant branch (PAGB) stars. The majority of low and intermediate mass stars (M tex2html_wrap_inline378 1-8M tex2html_wrap_inline302 ) are believed to pass through this post-asymptotic giant branch stage on their way to becoming planetary nebulae (PNe). However, this brief transition phase (typically 10 tex2html_wrap_inline334  yr (Wood & Faulkner 1986; Schönberner 1983, 1987)) is one of the least well understood stages of stellar evolution and recently there has been renewed interest in spectroscopic studies of stars believed to be at this evolutionary stage.

Recent work has concentrated on cooler PAGB stars of spectral type A, F and G, which have been observed for some years, often in globular clusters (Renzini 1985, Luck 1993). However, the work in this thesis deals with hotter analogues to these stars, which are likely to be the immediate precursors of planetary nebulae (McCausland et al. 1992). These PAGB stars are of spectral type B, and typically show very large carbon depletions. In the most massive and luminous AGB stars, a fourth process, hot bottom burning (HBB) may occur (Becker & Iben 1980; Renzini & Voli 1981; Meatheringham et al. 1990), and may remove carbon produced via the triple- tex2html_wrap_inline346 process. During the interpulse phase, temperatures may be sufficiently high to cause CNO processing at the base of the convective envelope. Thus the entire stellar envelope may be cycled through CNO processing, with the conversion of tex2html_wrap_inline344 C to tex2html_wrap_inline376 N, which is convected to the surface. Alternatively, it is possible that such stars arrived at the AGB with carbon already depleted, as descendants of the rare weak G-band stars, giants which are thought to be carbon deficient owing to large scale diffusion in Ap stars during the main sequence phase (Lambert & Sawyer 1984). This highlights the difficulty that although PAGB stars will have had their surface abundances modified via convective processes, the observed abundances are also dependent on the original stellar metallicity and other processes. Therefore their chemical compositions may also mimic those of Population I objects. For example, many of the cool A, F and G PAGB stars reveal near solar abundances for several elements (Venn & Lambert 1990; Bond 1991).

The hotter B-type PAGB stars have only recently been identified. As mentioned above, high resolution spectroscopy is required to differentiate them from main sequence stars, on the basis of their modified chemical compositions. However, determination of the surface gravity is sufficient to distinguish them from subluminous stars such as subdwarfs, which are characterised by higher gravities (Lamontagne et al. 1985; Heber et al. 1986; Moehler et al. 1990). In addition, some PAGB stars emit a detectable excess of radiation in the infrared, which may indicate the presence of a dust shell surrounding the star (Kwok et al. 1987). In this thesis, several projects related to PAGB stars are discussed, and are introduced below.




next up previous
Next: The iron abundances of Up: Introduction Previous: Metal line strengths in

Tim kendall
Wed Dec 6 13:15:27 WET 2000