Evolutionary Processes in Binary and Multiple Stars

By P. Eggleton. 2006

324 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f7a4acfa69465915f981f4a50f85ff62f738a423

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Common envelope evolution: where we stand and how we can move forward (2012, unknown): “3.6 of Eggleton 2006).”
Comparative statistics and origin of triple and quadruple stars (2008, background): “Kozai cycles with tidal friction (KCTF, Eggleton 2006) can be viewed as yet another flavor of migration where the angular momentum is deposited into a tertiary component while the orbital energy is dissipated by tides.”
The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc (2015, background): “The threshold for stability of multiple systems is considered to be a separation ratio for the outer to inner pair of 5:1 (Eggleton 2006), suggesting that all the triple systems are likely stable.”
The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity (2018, background): “…studies of blue stragglers, chemically peculiar stars, cataclysmic variables, SNe Ia and Ib/c, X-ray binaries, mergers of compact objects, short gammaray bursts, and sources of gravitational waves (Hurley et al. 2002; Eggleton 2006; Belczynski et al. 2008; Sana et al. 2012; De Marco & Izzard 2017).”
FROM BINARIES TO MULTIPLES. II. HIERARCHICAL MULTIPLICITY OF F AND G DWARFS (2014, background): “This mechanism, known as Kozai cycles with tidal friction (KCTF, Eggleton 2006), works well when the period ratio PL/PS is not too high and the initial inner period PS is not too long.”
The helium star donor channel for the progenitors of Type Ia supernovae (2009, methodology): “2000; Han & Podsiadlowski 2004, 2006; Chen & Li 2007; Han 2008; Meng, Chen & Han 2009). Meanwhile, a CO WD may also accrete material from a He star companion to increase its mass to the Ch mass, a process known as the He star donor channel in this paper. The study of Iben & Tutukov (1994) showed tha”
ON THE TRIPLE ORIGIN OF BLUE STRAGGLERS (2009, methodology): “The companions of blue straggler The binary companions of long period BSSs could be MS stars in the triple scenario (see also Eggleton & Kisseleva-Eggleton (2006, 2008) for a related discussion, and possible observations of such cases), which could not be the case for long period BSS binaries…”
The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, background): “Two of the hierarchical systems within this study were found to have low period ratios, indicative of a dynamically unstable system (Eggleton 2006); a triple system consisting of a single primary and a wide pair in a tight orbit (HIP 44127 A-BC;ι UMa), and the widest binary component of a higher…”
Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “Kiseleva-Eggleton, Eggleton and Fabrycky & Tremaine further studied the Mazeh & Shaham effect for cases where the eccentricity modulation is large, which occurs when the relative angle between the two orbital planes of motion is larger than ∼ 40◦.”
Theoretical uncertainties of the Type Ia supernova rate (2014, methodology): “…to test the mass transfer rate calculated with our BPS code, as a next step a set of binary systems and their mass transfer rates were calculated with the our BPS code and witha detailed binary stellar evolution code (STARS, Eggleton 1971, 2006; Pols et al. 1995; Glebbeek et al. 2008) and compared.”
Young Massive Star Clusters (2010, background): “An upper limit on the dividing line between phase 1 and phase 2 is the time of the first supernovae in the cluster, some 3 Myr after formation (Eggleton 2006), since these expel any remaining gas not already ejected by winds and radiation from OB stars.”