Effects of mass loss on the late stages of stellar evolution |
| |
| Affiliation: | 1. Department of Aeronautical and Vehicle Engineering, KTH Royal Institute of Technology, SE-100 44 Stockholm, Sweden;2. Volvo Car Corporation, Dept. 93600/PVÖSN23, 405 31 Gothenburg, Sweden;1. Civil Engineering Research Laboratory, Biskra University, 07000, Biskra, Algeria;2. Faculty of Civil Engineering, Wroclaw University of Science and Technology, Wybrzeze Wyspianskiego 27, 50-370, Wroclaw, Poland;3. Faculty of Mechanical Engineering, Wroclaw University of Science and Technology, Wybrzeze Wyspianskiego 27, 50-370, Wroclaw, Poland;1. Appleton Institute for Behavioural Science, Central Queensland University, PO Box 42, Goodwood, South Australia 5032, Australia;2. Centre for Sleep Research, University of South Australia, GPO Box 2471, Adelaide, South Australia 5001, Australia;1. Division of Cardiology, University of California, San Francisco, Box 0124, San Francisco, CA 94143-0124, USA;2. Division of Cardiology, Johns Hopkins Ciccarone Center for the Prevention of Heart Disease, Johns Hopkins Hospital, Baltimore, MD, USA;3. Department of Biostatistics, University of Washington, Seattle, WA, USA;4. Division of Preventive Medicine, Department of Family and Preventive Medicine, University of California, San Diego, San Diego, CA, USA;5. Department of Epidemiology, Bloomberg School of Public Health, Johns Hopkins University, Baltimore, MD, USA;6. Division of Cardiology, University of California, Irvine, Irvine, CA, USA;7. Division of Cardiology, Los Angeles Biomedical Research Institute at Harbor-UCLA, Torrance, CA, USA;1. Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, Case 7011, 35 rue Hélène Brion, 75205 Paris Cedex 13, France;2. Institute of Planetary Research, German Aerospace Center (DLR), 6 Rutherfordstraße 2, 12489 Berlin, Germany;3. Institut de Minéralogie, de Physique des Matériaux, et de Cosmochimie (IMPMC), Sorbonne Universités – UPMC Univ Paris 06, UMR CNRS 7590, Muséum National d''Histoire Naturelle, IRD UMR 206, 4 Place Jussieu, F-75005 Paris, France |
| |
| Abstract: | Advances in the infrared and radio observational techniques in the last decade have led to a revolution in our understanding of the late stages of stellar evolution. Intermediate (1–8 M⊙) mass stars are found to be undergoing rapid mass loss in the form of a stellar wind during the asymptotic-giant-branch after the exhaustion of helium burning in the core. Significant fraction of the original stellar mass can be lost in short time scales of < 106 yr. The ejected mass constitutes the major component of matter returned by stars to the interstellar medium. Since such material has been heavily nuclear processed, they also represent the dominant mechanism of chemical enrichment of the Galaxy. The high rate of mass loss implies that the majority of Population I stars end their evolution as planetary nebulae and white dwarfs rather than superovae and neutron stars.In this review, we summarize recent observational methods in the determination of the mass loss rate and the associated physical parameters of the stellar wind. Since the observed mass loss rate greatly exceeds the nuclear burning rate, we also discuss the theoretical models on how such mass loss affects the asymptotic giant branch evolution. A scenario is presented on how red giants evolve into planetary nebulae, a process which has been very poorly understood until recently. Conjectures on how the current evolutionary “missing link” - the proto-planetary nebulae - could be identified are also considered. |
| |
| Keywords: | |
| 本文献已被 ScienceDirect 等数据库收录！ |
|
