Long-Period Variables in the Magellanic Clouds

Wood, P. R.; Moore, G. K. G.; Hughes, Shaun M. G.

doi:10.1007/978-94-011-3432-3_62

Cited by 9 publications

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References 34 publications

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“…Wood et al (1991) combine a theoretical pulsation equation with a theoretical AGB relation to obtain: M b ol = -1-57 log P+0.73 log z-2.45 log M-6.1 A+const:(1) log Teff = -O.10 log P-O.072 log z+0.013 log M+0.6lA+const: (2a) (J-K) = +0.50 log P+0.36 log z-0.065 log M-3.05A+const:(2b) (M = mass, z = metal abundance).…”

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confidence: 99%

What do Mira Variables Tell us About the Late Evolution of Low Mass Stars?

Feast

1992

Highlights astron.

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(1)Mira variables define the tip of the AGB for low mass stars (cf. Feast and Whitelock 1987 fig. 1).(2)The kinematics of Mira variables are a function of period (e.g. Feast 1989 and earlier references) and for Miras in globular clusters the period is a function of metallicity (e.g. Feast 1981). Hence the Mira period sequence is not an evolutionary sequence but represents the sequence of AGB tips for stars of different initial mass and/or chemical composition and/or age.(3)Mira are surrounded by circumstellar dust shells. The mass loss rates are a function of period and light amplitude (Whitelock et al. 1987, Whitelock et al. 1991, Whitelock 1990). The results suggest evolution with increasing pulsation amplitude and mass loss but little change in log P ((2) and (3) do not preclude some (small) change in log P during evolution nor possible phases of decreasing light amplitude and mass loss).

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confidence: 99%