Abstract
The bright star ε Aurigae, an eclipsing binary with the longest known orbital period and eclipse, has been slow to reveal it secrets. The most recent eclipse, 2009-2011, was monitored with an array of new and old astronomical techniques, leading to new evidence concerning the nature of the eclipsing body and its contents. While this has led to new insights about the state of the F superigant star and to more clues about the evolutionary state of the system and components, a high-mass versus low-mass model dilemma persists. This chapter examines some of the recent developments and attempts to place the system among the pantheon of binary types. It also offers suggestions for observational tests prior to the next eclipse in 2037.
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Notes
- 1.
The disk dimensions reported in that paper were based only on early eclipse phases, and should be used with caution.
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Stencel, R.E. (2015). ϵ Aurigae: A Two Century Long Dilemma Persists. In: Ake, T., Griffin, E. (eds) Giants of Eclipse: The ζ Aurigae Stars and Other Binary Systems. Astrophysics and Space Science Library, vol 408. Springer, Cham. https://doi.org/10.1007/978-3-319-09198-3_4
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