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Multiplicity in Star Formation
2012The previous chapter formulated the characteristics of the formation of single young stars not taking in account effects of fragmentation. That fragmention in critical stages when seed stars form is likely to occur throughout the Galaxy. This implies that the vast majority of protostars and PMS stars are found in multiple systems.
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1991
The observational study of double and multiple stars is traditionally seen as comprised of several specialized subfields, each defined by particular observational selection effects. Improvements in increased precision and accuracy, higher resolution, higher signal-to-noise ratios, greater sensitivity etc.), are leading the study of double stars to a ...
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The observational study of double and multiple stars is traditionally seen as comprised of several specialized subfields, each defined by particular observational selection effects. Improvements in increased precision and accuracy, higher resolution, higher signal-to-noise ratios, greater sensitivity etc.), are leading the study of double stars to a ...
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Multiple Stars: Physics vs. Dynamics
2007We review physical and dynamical parameters of multiple stars. Possible scenaria of multiple star formation are discussed: their birth in dense cloud cores and the decay of small stellar groups and clusters. We compare physical and dynamical features of simulated multiple stars formed by these processes with the actual multiple stars.
Zhuchkov R., Orlov V., Rubinov A.
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1994
The nature of research on double and multiple stars has changed drastically during the past several decades. Prior to then the research was mostly concerned with visual measures for the purposes of obtaining orbital elements and masses. Then came spectroscopic studies that (1) when combined with the visual orbital elements allowed the determination of ...
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The nature of research on double and multiple stars has changed drastically during the past several decades. Prior to then the research was mostly concerned with visual measures for the purposes of obtaining orbital elements and masses. Then came spectroscopic studies that (1) when combined with the visual orbital elements allowed the determination of ...
openaire +2 more sources
Speckle interferometry of nearby multiple stars. V. 2002–2006 positional measurements
, 2013I. Balega+7 more
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