Multi-scale observations of dense core G205.46-14.56-N2 show a quadruple protostellar system whose symmetry, outflows, and kinematics match simulations of rotational fragmentation, providing the first claimed evidence for this pathway in high-order multiples.
Stellar Multiplicity
4 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
Stellar multiplicity is an ubiquitous outcome of the star formation process. Characterizing the frequency and main characteristics of multiple systems and their dependencies on primary mass and environment is therefore a powerful tool to probe this process. While early attempts were fraught with selection biases and limited completeness, instrumentation breakthroughs in the last two decades now enable robust analyses. In this review, we summarize our current empirical knowledge of stellar multiplicity for Main Sequence stars and brown dwarfs, as well as among populations of Pre-Main Sequence stars and embedded protostars. Clear trends as a function of both primary mass and stellar evolutionary stage are identified that will serve as a comparison basis for numerical and analytical models of star formation.
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UNVERDICTED 4representative citing papers
30-year kinematic monitoring of 27 Galactic center Wolf-Rayet stars identifies five binary candidates and infers a binary fraction of 0.56 ± 0.18.
Gaia-derived parameters for 13 Orion clusters fed into N-body simulations reveal two regimes: seven with α_vir ≲ 7 retain bound cores for ≳170 Myr while six with α_vir ≳ 7 dissolve before 120 Myr.
Enhanced mass transfer stability explains the observed deficit of post-common-envelope binaries with solar-type companions, with inefficient common envelope evolution (alpha_CE=0.25) providing the best match when combined with magnetic braking and selection effects.
citing papers explorer
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A Kinematic Study of Wolf-Rayet Stars at the Galactic Center I: Binary Candidates and Constraints on the Binary Fraction
30-year kinematic monitoring of 27 Galactic center Wolf-Rayet stars identifies five binary candidates and infers a binary fraction of 0.56 ± 0.18.
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Dynamical evolution and dissolution timescale of young stellar clusters in the Orion star-forming complex
Gaia-derived parameters for 13 Orion clusters fed into N-body simulations reveal two regimes: seven with α_vir ≲ 7 retain bound cores for ≳170 Myr while six with α_vir ≳ 7 dissolve before 120 Myr.