Common envelope evolution / Natalia Ivanova, Stephen Justham, Paul Ricker.

Format:

Book

Author/Creator:

Ivanova, Natalia (astrophysicist), author.

Justham, Stephen (astrophysicist), author.

Ricker, Paul M., author.

Contributor:

Institute of Physics (Great Britain), publisher.

Series:

AAS-IOP astronomy. 2021 collection.

AAS-IOP astronomy. [2021 collection], 2514-3433

Language:

English

Subjects (All):

Double stars--Evolution.

Double stars.

Physical Description:

1 online resource (various pagings)

Place of Publication:

Bristol [England] (Temple Circus, Temple Way, Bristol BS1 6HG, UK) : IOP Publishing, [2020]

System Details:

Mode of access: World Wide Web.

System requirements: Adobe Acrobat Reader, EPUB reader, or Kindle reader.

Biography/History:

Natalia Ivanova is Professor of theoretical and computational astrophysics within the Physics Department, University of Alberta. Her scientific interests include everything about the understanding of single, binary, multiple stars and clusters of them, stellar physics, and numerical codes that can create a star or many of them inside a computer. In 2010, she was appointed as Canada Research Chair in astronomy and astrophysics. Stephen Justham is currently based at the University of Amsterdam, where he is an acting group leader, on extended leave from a Professorship in the University of the Chinese Academy of Sciences. His research focuses on understanding the physics and consequences of stellar interactions, including how those help to explain the observed variety of stellar systems and explosive transients.

Summary:

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 ejected and helps to explain the formation of a wide variety of astrophysical phenomena, including cataclysmic variables, X-ray binaries, progenitors for type Ia supernovae, and gravitational-wave mergers. Modeling common envelope evolution is a challenging problem, and this important process has typically been described in evolutionary models using very approximate treatments. This book explains the physics of common envelope evolution and relates it to the approximations that are frequently used for modeling the onset, progression, and outcome of common envelope phases.

Contents:

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.

Notes:

"Version: 20201201"--Title page verso.

Includes bibliographical references.

Title from PDF title page (viewed on January 14, 2021).

ISBN:

9780750315623

0750315628

9780750315630

0750315636

OCLC:

1231597435