Morpho-kinematics of the wind of asymptotic giant branch star L2 Pup

The Asymptotic Giant Branch

The Very Slow Wind from the Pulsating Semiregular Red Giant, L2 Pup

We have obtained 11.7 μm and 17.9 μm images at the Keck I telescope of the circumstellar dust emission from L2 Pup, one of the nearest (D = 61 pc) masslosing, pulsating, red giants that has a substantial infrared excess. We propose that the star is losing mass at a rate of ∼3 × 10 M⊙ yr . Given its relatively low luminosity (∼ 1500 L⊙), relatively high effective temperature (near 3400 K), relat...

On the asymptotic giant branch star origin of peculiar spinel grain OC 2

Context. Microscopic presolar grains extracted from primitive meteorites have extremely anomalous isotopic compositions revealing the stellar origin of these grains. Multiple elements in single presolar grains can be analysed with sensitive mass spectrometers, providing precise sets of isotopic compositions to be matched by theoretical models of stellar evolution and nucleosynthesis. Aims. The ...

Mass loss on the Asymptotic Giant Branch

Mass loss on the Asymptotic Giant Branch provides the origin of planetary nebulae. This paper reviews several relevant aspects of AGB evolution: pulsation properties, mass loss formalisms and time variable mass loss, evidence for asymmetries on the AGB, binarity, ISM interaction, and mass loss at low metallicity. There is growing evidence that mass loss on the AGB is already asymmetric, but wit...

Stellar evolution on the Asymptotic Giant Branch

Mass loss dominates the stellar evolution on the Asymptotic Giant Branch. The phase of highest mass-loss occurs during the last 1–10% of the AGB and includes the so-called Miras and OH/IR stars. In this review I will discuss the characteristics and evolution of especially Miras, and discuss how they are linked to the mass loss. There are indications that high mass-loss rates are only reached fo...