The central stars

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ALMA and the CSEs!! Iso-distance samples are very important !!M vs P(M MS )dN/dMM-starsC-starsM vs v expM-starsC-stars
ALMA and the CSEsSizes of the emitting regions:B CSE,d (p) ∝ p −1.4⎡θ CO ≈ 5 ⎣0.1 + 0.9sharply peaked at the centre, butextend much further thanmolecule-CSEs, and is opticallythin even at high mass-loss rates( ) ⎤ 0.7Ṁ⎦10 −6[ 1 kpcD]arcsphotodiss.radiusθ CO (8 kpc, 10 −6 M ⊙ /yr) ≈ 0.5 arcsθ CO (50 kpc, 10 −5 M ⊙ /yr) ≈ 0.5 arcsθ mol ≤ 0.1 θ COnormallysharplypeaked atthe centre
Page 1 and 2: ALMA and AGB starsHans OlofssonOnsa
Page 3 and 4: The importance of AGB stars- They a
Page 5 and 6: The stellar mass lossThe mass loss
Page 7 and 8: AGB stars are dynamical objectsThis
Page 9 and 10: ALMA and the central starsSize (ten
Page 11 and 12: ALMA and the CSEsM(t,θ,φ,M MS ,Z,
Page 13 and 14: ALMA and the CSEsNote thatS ∗ ∝
Page 15: ALMA and the CSEsObservational spac
Page 19 and 20: Circumstellar molecules∑ = 69 cir
Page 21 and 22: Circumstellar SiO abundance estimat
Page 23 and 24: Circumstellar isotope ratiosEven a
Page 25 and 26: ALMA and the circumstellar structur
Page 27 and 28: ALMA and the circumstellar structur
Page 29 and 30: Comparisons of gas and dust distrib
Page 31 and 32: Termination of the AGB phaseIRC+102
Page 33 and 34: Post-AGB circumstellar chemistry11

The central stars

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