Common Envelope Evolution of Massive Binary Stars

Taam, Ronald E.; Sandquist, Eric L.

doi:10.1146/annurev.astro.38.1.113

Cited by 283 publications

(249 citation statements)

References 133 publications

Supporting

Mentioning

242

Contrasting

Order By: Relevance

“…Chaty and Rahoui (2012) estimated the size of the infrared emitting disk to ∼ 70 R * . If the compact object orbits in the external regions of that disk, the system may end up in a BH/NS binary (Taam and Sandquist, 2000).…”

Section: Igr J16318-4848mentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

View full text Add to dashboard Cite

High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

show abstract

Section: Igr J16318-4848mentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

View full text Add to dashboard Cite

show abstract

“…Due to the close-to-spherical orbits, the system NN Ser provides a particularly strong case against a purely orbital change of pre-existing planets, while an eccentricity of 20% as in HU Aqr is potentially still compatible with semi-adiabatic orbital expansion (Portegies Zwart 2013). The CE model originally put forward by Paczynski (1976) is the central ingredient for the formation of many close binary systems, as discussed for instance by Meyer & MeyerHofmeister (1979), Iben & Livio (1993), Taam & Sandquist (2000), Webbink (2008) and Taam & Ricker (2010). A CE is defined as a structure where two stars share the envelope.…”

Section: Introductionmentioning

confidence: 99%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

View full text Add to dashboard Cite

Context. The close binary system NN Serpentis must have gone through a common envelope phase before the formation of its white dwarf. During this phase, a substantial amount of mass was lost from the envelope. The recently detected orbits of circumbinary planets are probably inconsistent with planet formation before the mass loss. Aims. We explore whether new planets may have formed from the ejecta of the common envelope and derive the expected planetary mass as a function of radius. Methods. We employed the Kashi & Soker model to estimate the amount of mass that is retained during the ejection event and inferred the properties of the resulting disk from the conservation of mass and angular momentum. The resulting planetary masses were estimated from models with and without radiative feedback. Results. We show that the observed planetary masses can be reproduced for appropriate model parameters. Photoheating can stabilize the disks in the interior, potentially explaining the observed planetary orbits on scales of a few AU. We compare the expected mass scale of planets for 11 additional systems with observational results and find hints of two populations, one consistent with planet formation from the ejecta of common envelopes and the other a separate population that may have formed earlier.Conclusions. The formation of the observed planets from the ejecta of common envelopes seems feasible. The model proposed here can be tested through refined observations of additional post-common envelope systems. While it appears observationally challenging to distinguish between the accretion on pre-existing planets and their growth from new fragments, it may be possible to further constrain the properties of the protoplanetary disk through additional observations of current planetary candidates and post-common envelope binary systems.

show abstract

“…Detailed treatment of the CE process with hydrodynamic models has been attempted (Bodenheimer & Taam 1984;Taam & Sandquist 2000;Ricker & Taam 2008;Podsiadlowski et al 2010), but has yet to produce a cohesive physical understanding of the entire process. Podiadlowski et al (2010) present an intriguing scenario which shows the simplicity of the α-formalism (Nelmans & Tout 2005).…”

Section: Population Synthesis Methodsmentioning

confidence: 99%

Accretion, ablation and propeller evolution in close millisecond pulsar binary systems

Kiel¹,

Taam²

2013

Astrophys Space Sci

Self Cite

View full text Add to dashboard Cite

A model for the formation and evolution of binary millisecond radio pulsars in systems with low mass companions (< 0.1 M ⊙ ) is investigated using a binary population synthesis technique. Taking into account the non conservative evolution of the system due to mass loss from an accretion disk as a result of propeller action and from the companion via ablation by the pulsar, the transition from the accretion powered to rotation powered phase is investigated. It is shown that the operation of the propeller and ablation mechanisms can be responsible for the formation and evolution of black widow millisecond pulsar systems from the low mass X-ray binary phase at an orbital period of ∼ 0.1 day. For a range of population synthesis input parameters, the results reveal that a population of black widow millisecond pulsars characterized by orbital periods as long as ∼ 0.4 days and companion masses as low as ∼ 0.005 M ⊙ can be produced. The orbital periods and minimum companion mass of this radio millisecond pulsar population critically depend on the thermal bloating of the semi-degenerate hydrogen mass losing component, with longer orbital periods for a greater degree of bloating. Provided that the radius of the companion is increased by about a factor of 2 relative to a fully degenerate, zero temperature configuration, an approximate agreement between observed long orbital periods and theoretical modeling of hydrogen rich donors can be achieved. We find no discrepancy between the estimated birth rates for LMXBs and black

show abstract

Common Envelope Evolution of Massive Binary Stars

Cited by 283 publications

References 133 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Planet formation from the ejecta of common envelopes

Accretion, ablation and propeller evolution in close millisecond pulsar binary systems

Contact Info

Product

Resources

About