Common envelope evolution /

Common envelope evolution is the most important phase in the lives of many significant classes of binary stars. During a common envelope phase, the stars temporarily share the same outer layers, with the cores of both stars orbiting inside the same common envelope. This common envelope is sometimes...

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Detalles Bibliográficos
Clasificación:Libro Electrónico
Autores principales: Ivanova, Natalia (astrophysicist) (Autor), Justham, Stephen (astrophysicist) (Autor), Ricker, Paul M. (Autor)
Formato: Electrónico eBook
Idioma:Inglés
Publicado: Bristol [England] (Temple Circus, Temple Way, Bristol BS1 6HG, UK) : IOP Publishing, [2020]
Colección:IOP (Series). Release 21.
AAS-IOP astronomy. 2021 collection.
Temas:
Double stars > Evolution.
Galaxies & stars.
SCIENCE / Physics / Astrophysics.
Acceso en línea:Texto completo
Tabla de Contenidos:
  • 1. Introduction
  • 1.1. Why do we think common-envelope evolution happens?
  • 1.2. Why is common-envelope evolution broadly important?
  • 1.3. Why is modeling common-envelope evolution difficult?
  • 2. Main phases
  • 2.1. Characteristic timescales
  • 2.2. Phase I : the loss of orbital stability and the onset of the common envelope
  • 2.3. Phase II : the plunge-in
  • 2.4. Phase III : the slow spiral-in
  • 2.5. Phase IV : termination of the slow spiral-in phase
  • 2.6. Phase V : post-CE evolution
  • 3. The energy budget
  • 3.1. The energy formalism
  • 3.2. The energy of the envelope
  • 3.3. Extra energy sources
  • 3.4. Ways in which the energy reservoirs may be used
  • 3.5. Energy losses : radiation
  • 3.6. The complete energy budget
  • 3.7. A brief guide to the energy components
  • 4. The codes that do the job
  • 4.1. Physics of common-envelope evolution
  • 4.2. Numerical methods
  • 4.3. What can we trust?
  • 5. The onset of the common envelope
  • 5.1. Tides and pre-CEE
  • 5.2. Darwin instability
  • 5.3. Onset induced by a tertiary companion
  • 5.4. Orbital evolution due to mass loss
  • 5.5. Increased mass loss before the RLOF
  • 5.6. Roche-lobe overflow and L1 mass transfer
  • 5.7. Mass loss via outer Lagrangian points
  • 5.8. The Onset of double-core common-envelope
  • 5.9. The effects of pre-plunge-in evolution on ce evolution
  • 6. The plunge-in
  • 6.1. The start of the plunge-in and the initial conditions
  • 6.2. The plunge itself : overview of three-dimensional numerical results
  • 6.3. The end of the plunge-in phase
  • 6.4. Plunge-in and 1D considerations
  • 7. The slow spiral-in
  • 7.1. How should we identify the slow spiral-in in simulations?
  • 7.2. Which processes are important?
  • 7.3. Transition from the plunge to the slow spiral-in
  • 7.4. What have we learned from one-dimensional simulations?
  • 8. Mechanisms of mass ejection
  • 8.1. Initial ejection
  • 8.2. Dynamical plunge-in ejection
  • 8.3. Recombination outflows
  • 8.4. Shell-triggered ejections and delayed dynamical ejection
  • 9. The outcomes of CE simulations
  • 9.1. The mass of the initial and remnant core
  • 9.2. Properties of post-common-envelope binaries
  • 9.3. Characteristics of outflows
  • 9.4. Can angular momentum conservation be used to predict CEE outcomes?
  • 10. Linking with observations
  • 10.1. Overview
  • 10.2. Post-common-envelope binary properties
  • 10.3. Post-common-envelope planetary nebulae
  • 10.4. Presumed post-merger stars and their nebulae
  • 10.5. Transients from CEE and stellar mergers
  • 10.6. Stars undergoing a common-envelope phase.

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