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Progress and Application of The Initial-Final Mass Relation

Published online by Cambridge University Press:  08 August 2017

Jeffrey D. Cummings
Jeffrey D. Cummings*
Affiliation:
Center for Astrophysical Sciences, Johns Hopkins University, 3400 N Charles Street Baltimore, MD 21218, USA email: jcummi19@jhu.edu
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Abstract

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The stellar life cycle is dominated by phases such as the hydrogen-burning stage and the remnant white dwarf cooling phase. However, between these two stages, stars dramatically transform themselves by losing the bulk of their mass. Planetary nebulae (PNe) provide a powerful clue to the processes involved in this transformation, but they are very complex. Over the past 15 years, a new wave of imaging and spectroscopy programs have uncovered the remnants of PNe, white dwarfs, in a wide range of well-measured environments. With this we can map the masses and temperatures of the stellar remnants to the properties of their progenitors. This work has now led to the first uniform mapping of the initial-final mass relation from 1.5 to 7 M⊙. The resulting relation is a fundamental input to our understanding of stellar evolution for low and intermediate-mass stars that produce PNe and has a wide range of applications.

Keywords

White DwarfsAGB and post-AGBPlanetary NebulaMass Loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 157 - 164
Copyright
Copyright © International Astronomical Union 2017 

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