Disintegrating Multiple Systems in Early Stellar Evolution

By B. Reipurth. 2000

159 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/bdb3be27bb6d1d74e3e684c98a4d429d9e02d597

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

On the Evolutionary Status of Class I Stars and Herbig-Haro Energy Sources in Taurus-Auriga (2004, background): “It has also been suggested that HH stars are more likely to be in binary systems (Reipurth 2000).”
Stellar Multiplicity and the Initial Mass Function: Most Stars Are Single (2006, background): “On the other hand, most stars could still initially form in binary or multiple systems provided that most such systems promptly disintegrate via dynamical interactions or decay in an early, perhaps even protostellar, stage of evolution (e.g., Kroupa 1995; Sterzik & Durisen 1998, Reipurth 2000).”
Stellar Multiplicity (2013, background): “In addition, high-resolution observations at near-infrared and centimeter wavelengths are probing scattered light and free-free emission (Reipurth 2000, Reipurth et al. 2004), respectively, neither of which can be used to unambiguously detect companions.”
Tertiary Companions to Close Spectroscopic Binaries (2006, background): “Reipurth (2000) gives convincing evidence that strong accretion and jet activity is actually observed in embedded young multiple systems.”
The physics of star formation (2003, background): “…to be single can be accounted for if stars typically form in unstable triple systems that decay into a binary and a single star (Larson 1972a; Reipurth 2000); this simple scenario would be consistent with the observed fact that about two-thirds of all stars are in binary systems while about…”
A Keplerian disk around a Class 0 source: ALMA observations of VLA1623A (2013, background): “Second, due to three-body interaction, VLA1623W was ejected from the closer binary of VLA1623A and B (Reipurth 2000).”
STELLAR POPULATIONS IN THE CENTRAL 0.5 pc OF THE GALAXY. II. THE INITIAL MASS FUNCTION (2013, background): “…cluster, and possibly the density of a cluster (e.g. Ghez et al. 1993; Petr et al. 1998; Mason et al. 1998; Duchêne et al. 1999; Köhler et al. 2000; Reipurth 2000; Patience et al. 2002; Shatsky & Tokovinin 2002; Köhler et al. 2006; Duchêne et al. 2007; Köhler et al. 2008; Mason et al. 2009;…”
The Formation of Brown Dwarfs as Ejected Stellar Embryos (2001, background): “…close dynamical interactions between small unstable groups of nascent stellar seeds, i.e. brown dwarfs differ from hydrogen burning stars only in that dynamical interactions deprived them from gaining further mass by prematurely cutting them off from their infalling gas reservoirs (Reipurth 2000).”
Simulating star formation in molecular cloud cores. I. The influence of low levels of turbulence on fragmentation and multiplicity (2003, background): “Second, the multiplicity of young pre-Main Sequence stars is if anything even higher than for mature field stars (Reipurth & Zinnecker 1993; Reipurth 2000; Patience et al. 2002).”
Clustered and Triggered Star Formation in W5: Observations with Spitzer (2008, background): “Numerical studies show that a given triple system will eject a member within about 100 crossing times (∼30000 years: Reipurth 2000).”
HERBIG-HARO FLOWS: Probes of Early Stellar Evolution (2001, background): “Inspired by the extreme multiplicity frequency among giant HH flow sources, Reipurth (2000) has suggested that there may be a causal link between multiplicity and major HH activity.”