Revisiting the common envelope evolution in binary stars: A new semianalytic model for 
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-body and population synthesis codes

Trani, Alessandro A.; Rieder, Steven; Tanikawa, Ataru; Iorio, Giuliano; Martini, Riccardo; Karelin, Georgii; Glanz, Hila; Zwart, Simon Portegies

doi:10.1103/physrevd.106.043014

Cited by 13 publications

(6 citation statements)

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“…If the system remains bound, the postcollapse orbital parameters are related to the precollapse parameters by (see, 5 Note, however, that population synthesis studies suggest that a sizable fraction of binaries might be eccentric as they enter the common envelope phase (Vigna-Gómez et al 2020), and recent common envelope modeling suggests that a fraction of these might still maintain some residual eccentricity post−common envelope (Trani et al 2022). We stress that while the assumption of e i = 0 in the present work significantly simplifies the expressions and provides clarity, it is by no means required, and that the most important results of the present work (such as the ultrafast merger time tail) are independent of this assumption.…”

Section: Bound Systemsmentioning

confidence: 99%

Ultrafast Compact Binary Mergers

Beniamini,

Piran

2024

ApJ

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The duration of orbital decay induced by gravitational waves (GWs) is often the bottleneck of the evolutionary phases going from star formation to a merger. We show here that kicks imparted to the newly born compact object during the second collapse generically result in a GW merger time distribution behaving like dN / d log t ∝ t 2 / 7 at short durations, leading to ultrafast mergers. Namely, a nonnegligible fraction of neutron star binaries, formed in this way, will merge on a timescale as short as 10 Myr, and a small fraction will merge even on a timescale less than 10 kyr. The results can be applied to different types of compact binaries. We discuss here the implications for binary neutron star mergers. These include unique short gamma-ray bursts (GRBs), eccentric and misaligned mergers, r-process enrichment in the very early Universe and in highly star-forming regions, and possible radio precursors. Interestingly, we conclude that among the few hundred short GRBs detected so far, a few must have formed via this ultrafast channel.

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Section: Bound Systemsmentioning

confidence: 99%

Ultrafast Compact Binary Mergers

Beniamini,

Piran

2024

ApJ

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“…During the rapid plunge-phase of the CEE the accretion flow is not in a steady state because the spiraling-in timescale  a a is on about the dynamical timescale of the giant star (e.g., Ohlmann et al 2016;Iaconi et al 2017b;Law-Smith et al 2020;Glanz & Perets 2021a, 2021bLau et al 2022aLau et al , 2022bGonzález-Bolívar et al 2022;Moreno et al 2022;Ondratschek et al 2022;Trani et al 2022;Roepke & De Marco 2023 for some recent papers and references to earlier studies therein). I take the plunge-in timescale as…”

Section: Timescalesmentioning

confidence: 99%

On the Nature of Jets from a Main Sequence Companion at the Onset of Common Envelope Evolution

Soker

2023

Res. Astron. Astrophys.

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I consider a flow structure by which main sequence companions that enter a common envelope evolution (CEE) with giant stars might launch jets even when the accreted gas has a sub-Keplerian specific angular momentum. I first show that after a main sequence star enters the envelope of a giant star the specific angular momentum of the accreted gas is sub-Keplerian but still sufficiently large for the accreted gas to avoid two conical-like openings along the two opposite polar directions. I suggest that the high-pressure zone that the accreted gas builds around the main sequence equatorial plane accelerates outflows along these polar opening. Most of the inflowing gas is deflected to the polar outflows, i.e., two oppositely-directed jets. The actual mass that the main sequence star accretes is only a small fraction, $\approx 0.1$, of the inflowing gas. However, the gravitational energy that this gas releases powers the inflow-outflow streaming of gas and adds energy to the common envelope ejection. This flow structure might take place during a grazing envelope evolution if it occurs, during the early CEE, and possibly in some post-CEE cases. This study increases the parameter space for main sequence stars to launch jets. Such jets might shape \add{ some morphological features in } planetary nebulae, add energy to mass removal in CEE, and power some intermediate luminosity optical transients.

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“…In isolated COBs several processes (e.g.,tidal interactions or dynamical friction during a common envelope phase) tend to circularise the orbit of the binary progenitor [e.g. [153][154][155][156][157], although some of the physical processes still partly unknown -like common envelope -could produce mildly eccentric binaries [158]. Conversely, the eccentricity distribution of dynamically assembled BBHs generally follows a thermal distribution, P(e)de ∼ 2e, which implies a probability of 50% to form a binary with eccentricity e > 0.7.…”

Section: Introductionmentioning

confidence: 99%

Quiescent and Active Galactic Nuclei as Factories of Merging Compact Objects in the Era of Gravitational Wave Astronomy

Sedda

Naoz

Kocsis³

2023

Universe

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Galactic nuclei harbouring a central supermassive black hole (SMBH), possibly surrounded by a dense nuclear cluster (NC), represent extreme environments that house a complex interplay of many physical processes that uniquely affect stellar formation, evolution, and dynamics. The discovery of gravitational waves (GWs) emitted by merging black holes (BHs) and neutron stars (NSs), funnelled a huge amount of work focused on understanding how compact object binaries (COBs) can pair up and merge together. Here, we review from a theoretical standpoint how different mechanisms concur with the formation, evolution, and merger of COBs around quiescent SMBHs and active galactic nuclei (AGNs), summarising the main predictions for current and future (GW) detections and outlining the possible features that can clearly mark a galactic nuclei origin.

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Revisiting the common envelope evolution in binary stars: A new semianalytic model for N -body and population synthesis codes

Cited by 13 publications

References 100 publications

Ultrafast Compact Binary Mergers

Ultrafast Compact Binary Mergers

On the Nature of Jets from a Main Sequence Companion at the Onset of Common Envelope Evolution

Quiescent and Active Galactic Nuclei as Factories of Merging Compact Objects in the Era of Gravitational Wave Astronomy

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