Abstract
The most massive stars, those with ZAMS masses above 50 M⊙, evolve into Luminous Blue Variables (LBVs) within 3 × 106 years (Langer et al. 1994) when they reach the empirical upper boundary in the Hertzsprung-Russell diagram (which is known as the Humphreys-Davidson limit; Humphreys & Davidson 1994). Winds with high mass-loss rates (~10−4 M⊙yr−1) and giant eruptions during the short (25,000 years) LBV phase lead to the formation of nebulae around these objects, the so-called LBV-nebulae (LBVN).
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References
Langer, N., Hamann, W.-R., Lennon, M., et al. (1994): AA 290, 819
Humphreys, R.M., Davidson, K. (1994): PASP 106, 1025
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© 1998 Springer-Verlag Berlin Heidelberg
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Weis, K., Duschl, W.J., Chu, YH. (1998). A Kinematic Study of the LBV Nebula around η Carinae. In: Kaper, L., Fullerton, A.W. (eds) Cyclical Variability in Stellar Winds. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-68597-5_24
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DOI: https://doi.org/10.1007/978-3-540-68597-5_24
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