Analytical treatment of the two-body problem with slowly varying mass

Rahoma, U. Ali; El-Salam, F. A. Abd; Ahmed, M. K.

doi:10.1007/s12036-009-0012-y

Cited by 27 publications

(22 citation statements)

References 15 publications

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“…In our simulations we have made the common assumption that the wind mass loss is slow compared to the orbital period. Within this limit, the change in the orbit becomes adiabatic, and the system remains bound (see Rahoma et al 2009, for a review). If, on the other hand, the mass loss is a sudden event, it can lead to the disruption of the system, as discussed in the context of supernova explosions (e.g.…”

Section: Stellar Wind Mass Lossmentioning

confidence: 99%

The binarity of the local white dwarf population

Toonen

Hollands

Gänsicke

et al. 2017

A&A

174

194

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Context. As endpoints of stellar evolution, white dwarfs (WDs) are powerful tools to study the evolutionary history of the Galaxy. In particular, the multiplicity of WDs contains information regarding the formation and evolution of binary systems. Aims. Can we understand the multiplicity of the local WD sample from a theoretical point of view? Population synthesis methods are often applied to estimate stellar space densities and event rates, but how well are these estimates calibrated? This can be tested by a comparison with the 20 pc sample, which contains ≃ 100 stars and is minimally affected by selection biases. Methods. We model the formation and evolution of single stars and binaries within 20 pc with a population synthesis approach. We construct a model of the current sample of WDs and differentiate between WDs in different configurations, that is single WDs, and resolved and unresolved binaries containing a WD with either a main-sequence (MS) component or with a second WD. We also study the effect of different assumptions concerning the star formation history, binary evolution, and the initial distributions of binary parameters. We compile from the literature the available information on the sample of WDs within 20 pc, with a particular emphasis on their multiplicity, and compare this to the synthetic models. Results. The observed space densities of single and binary WDs are well reproduced by the models. The space densities of the most common WD systems (single WDs and unresolved WD-MS binaries) are consistent within a factor two with the observed value. We find a discrepancy only for the space density of resolved double WDs. We exclude that observational selection effects, fast stellar winds, or dynamical interactions with other objects in the Milky Way explain this discrepancy. We find that either the initial mass ratio distribution in the Solar neighbourhood is biased towards low mass-ratios, or more than ten resolved DWDs have been missed observationally in the 20 pc sample. Furthermore, we show that the low binary fraction of WD systems (∼25%) compared to Solartype MS-MS binaries (∼50%) is consistent with theory, and is mainly caused by mergers in binary systems, and to a lesser degree by WDs hiding in the glare of their companion stars. Lastly, Gaia will dramatically increase the size of the volume-limited WD sample, detecting the coolest and oldest WDs out to ≃ 50 pc. We provide a detailed estimate of the number of single and binary WDs in the Gaia sample.

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Section: Stellar Wind Mass Lossmentioning

confidence: 99%

The binarity of the local white dwarf population

Toonen

Hollands

Gänsicke

et al. 2017

A&A

174

194

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“…2 2 Rahoma, Abd El‐Salam & Ahmed (2009) provides a detailed summary of additional results from past papers, and Plastino & Muzzio (1992) summarizes the ‘use and abuse’ of using a force to model mass‐loss. …”

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confidence: 99%

The great escape: how exoplanets and smaller bodies desert dying stars

Veras

Wyatt

Mustill

et al. 2011

Monthly Notices of the Royal Astronomical Society

234

310

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Mounting discoveries of extrasolar planets orbiting post‐main‐sequence stars motivate studies to understand the fate of these planets. In the traditional ‘adiabatic’ approximation, a secondary’s eccentricity remains constant during stellar mass‐loss. Here, we remove this approximation, investigate the full two‐body point‐mass problem with isotropic mass‐loss, and illustrate the resulting dynamical evolution. The magnitude and duration of a star’s mass‐loss combined with a secondary’s initial orbital characteristics might provoke ejection, modest eccentricity pumping, or even circularization of the orbit. We conclude that Oort Clouds and wide‐separation planets may be dynamically ejected from 1–7 M⊙ parent stars during AGB evolution. The vast majority of planetary material that survives a supernova from a 7–20 M⊙ progenitor will be dynamically ejected from the system, placing limits on the existence of first‐generation pulsar planets. Planets around >20 M⊙ black hole progenitors may easily survive or readily be ejected depending on the core collapse and superwind models applied. Material ejected during stellar evolution might contribute significantly to the free‐floating planetary population.

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“…In addition, the mass loss rate will be varied depending on stellar evolutionary stage and the mechanism of mass loss. For more information about mass loss refer to Rahoma et al (2009) and the references therein.…”

Section: Star Mass Lossmentioning

confidence: 99%

Investigating Exoplanet Orbital Evolution Around Binary Star Systems with Mass Loss

Rahoma¹

2016

Journal of Astronomy and Space Sciences

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A planet revolving around binary star system is a familiar system. Studies of these systems are important because they provide precise knowledge of planet formation and orbit evolution. In this study, a method to determine the evolution of an exoplanet revolving around a binary star system using different rates of stellar mass loss will be introduced. Using a hierarchical triple body system, in which the outer body can be moved with the center of mass of the inner binary star as a two-body problem, the long period evolution of the exoplanet orbit is determined depending on a Hamiltonian formulation. The model is simulated by numerical integrations of the Hamiltonian equations for the system over a long time. As a conclusion, the behavior of the planet orbital elements is quite affected by the rate of the mass loss from the accompanying binary star.

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Analytical treatment of the two-body problem with slowly varying mass

Cited by 27 publications

References 15 publications

The binarity of the local white dwarf population

The binarity of the local white dwarf population

The great escape: how exoplanets and smaller bodies desert dying stars

Investigating Exoplanet Orbital Evolution Around Binary Star Systems with Mass Loss

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