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Alberto Buzzoni INAF – Oss. Astronomico di Bologna, Italy

Stellar AGB evolution and its impact on galaxy spectrophotometric properties at low and high redshift: an updated view. Alberto Buzzoni INAF – Oss. Astronomico di Bologna, Italy. UV evolutionary paths for (old) low-mass stars. Renzini & Buzzoni (1986). Core mass.

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Alberto Buzzoni INAF – Oss. Astronomico di Bologna, Italy

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  1. Stellar AGB evolutionand its impact on galaxy spectrophotometric properties at low and high redshift: an updated view Alberto Buzzoni INAF – Oss. Astronomico di Bologna, Italy

  2. UV evolutionary paths for (old) low-mass stars Renzini & Buzzoni (1986) Core mass Dorman et al. (1993)

  3. EHB stars Castellani et al. (2006) Buson et al. (2006) (high-mass) MS Vassiliadis & Wood ‘94 Low Z High Z Dorman et al. ‘93 Brown et al. (1999)

  4. Back-in-time HB evolution HBtemperaturedistribution Buzzoni (1989) Brown et al. (2000)

  5. The puzzling problem of Planetary Nebulae Buzzoni, Arnaboldi & Corradi (2006) Weidemann (2000)

  6. PNe and galaxy environment UV enhanced UV poor

  7. Probing AGB extension

  8. Mass loss & SB magnitudes Reimers’s law 

  9. “Unconventional” fates

  10. AGB deployment and UV upturn(when infrared speaks to ultraviolet) No PNe No PNe Buzzoni & Gonzàlez-Lòpezlira (2007) data compilation from Cantiello et al. (2003)

  11. Toward a unitary picture? Globular clusters AGB ~ RGB [Fe/H]  lowest (« -0.5 dex) η highest (0.4-0.5) Core mass  low (~0.54 Mo) HB  blue PN  poor rate Metal-rich GCs & dE’s AGB >> RGB [Fe/H]  intermediate (< 0.0 dex) η lowest (0.0-0.1 ?) Core mass  highest (~0.65 Mo) HB  red PN  yes “standard” rate Ellipticals AGB > RGB [Fe/H]  highest (> 0.0 dex) η low (0.1-0.3 ?) Core mass  lowest (<0.52 Mo) HB  blue due to metal-rich PN  poor rate UV enhanced Spiral galaxies AGB >> RGB η VERY high (»1.5 ?) Core mass  highest (0.7-0.8 Mo) HB  red PN  yes “standard” rate UV enhanced?  yes but due to young Metal poor Metal rich UV poor O’Connell (1999)

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