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Isomeric diversity of GlcNAc(Man<sub>3</sub>GlcNAc<sub>2</sub>) and GlcNAc<sub>2</sub>(Man<sub>3</sub>GlcNAc<sub>2</sub>) N-glycans in multicellular eukaryotes. [PDF]
Sci RepLin YT +8 more
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The nucleardatapy toolkit for simple access to experimental nuclear data, astrophysical observations, and theoretical predictions. [PDF]
Eur Phys J A Hadron NuclMargueron J +12 more
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Consumed by Abdominal Distention
Arthritis Care &Research, EarlyView.
Abimbola Fadairo‐Azinge +3 more
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A low-mass star with a large-mass planet
Science, 2023A large planet orbiting a very low-mass star challenges theories of planet ...
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Searching for Low Mass Stars in the Halo
Astrophysics and Space Science, 1999From microlensing events detected at high galactic latitude as well as from direct measurements of the halo stellar density, estimations of a potential contribution of low mass stars to the mass budget is questioned. Up to now no clear answer has been found for one main reason: the difficulty to observe them in a sufficient volume, which requires deep ...
A.C. Robin, M. Crézé, V. Mohan
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Astrophysics and Space Science, 1994
Low mass stars contribute an important fraction to the mass of our Galaxy. Due to the faintness of these stars a direct investigation of their space distribution and kinematics can be carried out only in the immediate solar neighbourhood. This fact emphasizes the importance of the “Third Catalogue of Nearby Stars” (CNS3) as a probe of the stellar ...
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Low mass stars contribute an important fraction to the mass of our Galaxy. Due to the faintness of these stars a direct investigation of their space distribution and kinematics can be carried out only in the immediate solar neighbourhood. This fact emphasizes the importance of the “Third Catalogue of Nearby Stars” (CNS3) as a probe of the stellar ...
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Origins of life and evolution of the biosphere, 1997
Recent evidence indicates that most low mass stars in the Galaxy (< 5 M [symbol: see text]) form alongside massive stars in clusters embedded in giant molecular clouds. Once their parental gas is removed, the fate of these clusters is to disperse and blend into the field population of the galactic disk.
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Recent evidence indicates that most low mass stars in the Galaxy (< 5 M [symbol: see text]) form alongside massive stars in clusters embedded in giant molecular clouds. Once their parental gas is removed, the fate of these clusters is to disperse and blend into the field population of the galactic disk.
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Annual Review of Astronomy and Astrophysics, 1987
Very low mass (VLM) stars, which we define here somewhat arbitrarily as those with masses ;$ 0.3 M 0' pose some of the more interesting problems in stellar astrophysics. The physics of their envelopes and atmospheres are more complicated and their structures less well modeled than their more massive counterparts.
James Liebert, Ronald G. Probst
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Very low mass (VLM) stars, which we define here somewhat arbitrarily as those with masses ;$ 0.3 M 0' pose some of the more interesting problems in stellar astrophysics. The physics of their envelopes and atmospheres are more complicated and their structures less well modeled than their more massive counterparts.
James Liebert, Ronald G. Probst
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Low- and Intermediate-Mass Stars
2018Energy in stars is provided by nuclear reactions, which, in many cases, produce radioactive nuclei. When stable nuclei are irradiated by a flux of protons or neutrons, capture reactions push stable matter out of stability into the regime of unstable species. The ongoing production of radioactive nuclei in the deep interior of the Sun via proton-capture
Maria Lugaro, Alessandro Chieffi
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