Are Binary Separations Related to their System Mass?

Sterzik, M. F.; Durisen, R. H.

doi:10.1017/s0252921100008447

Cited by 9 publications

(2 citation statements)

References 17 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Their separations are orders of magnitude larger than those of the VLM tight binaries. They represent a challenge for the widely accepted idea that lighter systems tend to have smaller separations (Sterzik & Durisen 2004) and for the "embryoejection" scenario of formation of substellar objects (Reipurth & Clarke 2001;Bate, Bonnell & Bromm 2003). Large hydrodynamical simulations can produce wide low-mass binary systems, albeit rarely.…”

Section: Introductionmentioning

confidence: 99%

Southern Very Low Mass Stars and Brown Dwarfs in Wide Binary and Multiple Systems

Caballero

2007

ApJ

View full text Add to dashboard Cite

The results of the Koenigstuhl survey in the Southern Hemisphere are presented. I have searched for common-proper motion companions to 173 field very low-mass stars and brown dwarfs with spectral types > M5.0V and magnitudes J 14.5 mag. I have measured for the first time the common-proper motion of two new wide systems containing very low-mass components, Koenigstuhl 2 AB and 3 A-BC. Together with Koenigstuhl 1 AB and 2M0126-50AB, they are among the widest systems in their respective classes (r = 450-11 900 AU). I have determined the minimum frequency of field wide multiples (r > 100 AU) with late-type components at 5.0±1.8 % and the frequency of field wide late-type binaries with mass ratios q > 0.5 at 1.2±0.9 %. These values represent a key diagnostic of evolution history and low-mass star and brown-dwarf formation scenarios. Additionally, the proper motions of 76 field very low-mass dwarfs are measured here for the first time.

show abstract

Section: Introductionmentioning

confidence: 99%

Southern Very Low Mass Stars and Brown Dwarfs in Wide Binary and Multiple Systems

Caballero

2007

ApJ

View full text Add to dashboard Cite

show abstract

“…Greenstein (1986) and Oswalt & Sion (1988) were among the first to present observational evidence for such expansion. Oswalt & Strunk (1994) and Sterzik & Durisen (2004) noticed that FBs with MS components of early spectral type tend to have much wider mean separations than those of later spectral class. Valls-Gabaud (1988) and showed that expansion of up to an order of magnitude can occur with the right combination of initial primary mass and binary mass ratio.…”

Section: Importance Of Fragile Binaries With Evolved Componentsmentioning

confidence: 99%

Fragile Binaries: Observational Leverage on Difficult Astrophysical Problems

et al. 2006

View full text Add to dashboard Cite

Loosely bound, fragile binary stars, whose separations may reach ∼ 0.1 pc, are like open clusters with two coeval components. They provide a largely overlooked avenue for the investigation of many astrophysical questions. For example, the orbital distribution of fragile binaries with two long-lived main-sequence components provides a sensitive test of the cumulative effects of the Galactic environment. In pairs where one component is evolved, the orbits have been amplified by post-main-sequence mass loss, potentially providing useful constraints on the initial-to-final mass relation for white dwarfs. The nearly featureless spectra of cool white dwarfs usually provide little information about intrinsic radial velocity, full space motion, population membership, metallicity, etc. However, distant main sequence companions provide benchmarks against which those properties can be determined. In addition, the cooling ages of white dwarf components provide useful limits on the ages of their main sequence companions, independent of other stellar age determination methods. This paper summarizes some of the ways fragile binaries provide useful leverage on these and other problems of interest.

show abstract

Pairing mechanisms for binary stars

Kouwenhoven¹,

Goodwin

Zwart

et al. 2008

Astron Nachr

View full text Add to dashboard Cite

Knowledge of the binary population in stellar groupings provides important information about the outcome of the star forming process in different environments. Binarity is also a key ingredient in stellar population studies and is a prerequisite to calibrate the binary evolution channels. In these proceedings we present an overview of several commonly used methods to pair individual stars into binary systems, which we refer to as the pairing function. Many pairing functions are frequently used by observers and computational astronomers, either for the mathematical convenience, or because they roughly describe the expected outcome of the star forming process. We discuss the consequences of each pairing function for the interpretation of observations and numerical simulations. The binary fraction and mass ratio distribution generally depend strongly on the selection of the range in primary spectral type in a sample. These quantities, when derived from a binary survey with a mass-limited sample of target stars, are thus not representative for the population as a whole.Comment: 4 pages, 2 figures, in: Galactic and stellar dynamics in the era of high-resolution surveys, Boily C., Combes F., Hensler G., eds., Strasbourg (France), March 2008, in press (Astron. Nachr.

show abstract

Are Binary Separations Related to their System Mass?

Cited by 9 publications

References 17 publications

Southern Very Low Mass Stars and Brown Dwarfs in Wide Binary and Multiple Systems

Southern Very Low Mass Stars and Brown Dwarfs in Wide Binary and Multiple Systems

Fragile Binaries: Observational Leverage on Difficult Astrophysical Problems

Pairing mechanisms for binary stars

Contact Info

Product

Resources

About