Stellar triples on the edge - Comprehensive overview of the evolution of destabilised triples leading to stellar and binary exotica

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Volume 661 (May 2022)

A&A, 661 (2022) A61

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Table 1.

Distributions of the initial stellar masses, rotation, and orbital parameters.

Parameter	Range	Model OBin	Model T14⁽¹⁾	Model E09⁽²⁾
Mass of primary m₁	1–7.5 M_⊙	Kroupa IMF⁽³⁾	Kroupa IMF⁽³⁾	Kroupa IMF⁽³⁾
2*Mass ratio	0 − 1 ^(*)	2*Uniform^{(4, 5, 6)}	2*Uniform^{(4, 5, 6)}	2*Model E09⁽²⁾
	m₂, m₃ > 0.008 M_⊙
Stellar rotation		Hurley rotation⁽⁷⁾	Hurley rotation⁽⁷⁾	Hurley rotation⁽⁷⁾
Orbital separation	5 − 5 ⋅ 10⁶ R_⊙^(**)	Uniform in log(a)^(8, 9)	Log-normal ^(***)^{, (1, 4, 11)}	Model E09⁽²⁾
Eccentricity	0 − 1	Thermal distribution⁽¹⁰⁾	Thermal distribution⁽¹⁰⁾	Thermal distribution⁽¹⁰⁾
Inclination	0 − π	Uniform in cos(i)⁽¹²⁾	Uniform in cos(i)⁽¹²⁾	Uniform in cos(i)⁽¹²⁾
Argument of pericentre	–π − π	Uniform	Uniform	Uniform

Notes. See also Fig. 1–3 in Toonen et al. (2020) for a graphical representation of these parameters.

^(*)

Except for the outer mass ratio q_out in model E09;

^(**)

Formally the maximum orbital separation for Model T14 is 10¹² R_⊙. Due to the shape of the log-normal distribution, the contribution from systems with a_out ≳ 5 ⋅ 10⁷ R_⊙ is negligible;

^(***)

A log-normal distribution with periods in days, mean μ = 5 and dispersion σ = 2.3.

References. ⁽¹⁾Tokovinin (2014); ⁽²⁾Eggleton (2009); ⁽³⁾Kroupa et al. (1993); ⁽⁴⁾Raghavan et al. (2010); ⁽⁵⁾Duchêne & Kraus (2013); ⁽⁶⁾Sana et al. (2012); ⁽⁷⁾Hurley et al. (2000); ⁽⁸⁾Abt (1983); ⁽⁹⁾Kouwenhoven et al. (2007); ⁽¹⁰⁾Heggie (1975); ⁽¹¹⁾Duquennoy & Mayor (1991); ⁽¹²⁾Tokovinin (2017).

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