Results 51 to 60 of about 1,884 (262)

Constraining Extra Mixing During the Main Sequence: Whatever Depletes Lithium Does Not Touch Beryllium

open access: yesThe Astrophysical Journal
Measurements of lithium (Li) abundances in solar-type stars have shown that standard models of stellar evolution are incapable of explaining the observed depletion as a function of stellar age.
Henrique Reggiani   +6 more
doaj   +1 more source

The Interaction Between Accretion from the Interstellar Medium and Accretion from the Evolved Binary Component in Barium Stars [PDF]

open access: yesJournal of Astronomy and Space Sciences, 2018
The reanalysis of the previously published abundance pattern of mild barium star HD202109 (ζ Cyg) and the chemical compositions of 129 thin disk barium stars facilitated the search for possible correlations of different stellar parameters with second ...
Yeuncheol Jeong   +2 more
doaj   +1 more source

Stellar Iron Abundances: Non‐LTE Effects [PDF]

open access: yesThe Astrophysical Journal, 1999
22 pages, 9 figures, 1 table, ApJ style ...
Thevenin, F., Idiart, T. P.
openaire   +2 more sources

From mice to humans—divergent strategies for intestinal homeostasis and regeneration

open access: yesFEBS Letters, EarlyView.
Recent advances such as organoid genome editing, xenotransplantation, imaging, and whole‐genome sequencing have enabled direct studies of human intestinal stem cells (ISCs). These studies reveal species‐specific features, including slower ISC proliferation, distinct injury responses, slower somatic mutation accumulation in humans, and an inverse ...
Keiko Ishikawa   +2 more
wiley   +1 more source

Stellar photospheric abundances as a probe of discs and planets [PDF]

open access: yesMonthly Notices of the Royal Astronomical Society, 2018
Protoplanetary disks, debris disks, and disrupted or evaporating planets can all feed accretion onto stars. The photospheric abundances of such stars may then reveal the composition of the accreted material. This is especially likely in B to mid-F type stars, which have radiative envelopes and hence less bulk--photosphere mixing.
Adam S Jermyn, Mihkel Kama
openaire   +2 more sources

Phosphoinositides and inositol phosphates as molecular glues

open access: yesFEBS Letters, EarlyView.
Inositol phosphates (IPs) and phosphoinositides (PIPs) regulate diverse eukaryotic processes. Beyond recruiting signaling proteins or acting as structural cofactors, recent studies suggest they mediate protein–protein interactions as natural molecular glues.
Aleshia Seaton‐Terry   +9 more
wiley   +1 more source

NGC 1856: Using Machine Learning Techniques to Uncover Detailed Stellar Abundances from MUSE Data

open access: yesThe Astronomical Journal
We present the first application of the novel approach based on data-driven machine learning methods applied to Multi-Unit Spectroscopic Explorer (MUSE) field data to derive stellar abundances of star clusters.
Randa Asa’d   +7 more
doaj   +1 more source

Multiple Stellar Populations at Less Evolved Stages. III. A Possible Helium Spread in NGC 2210

open access: yesThe Astrophysical Journal, 2023
Helium variations are common features of globular clusters (GCs) with multiple stellar populations. All the formation scenarios predict that secondary population stars are enhanced in helium, but the exact helium content depends on the polluters ...
Chengyuan Li   +8 more
doaj   +1 more source

Three phosphatase families form a community: The phosphohydrolases that act upon inositol pyrophosphates

open access: yesFEBS Letters, EarlyView.
Inositol pyrophosphates are energy‐rich signaling molecules that perform critical functions in cells. Three different families of phosphatases hydrolyze the β phosphate of the inositol pyrophosphate molecules: two have narrow specificities and one is promiscuous.
Ronda J. Rolfes
wiley   +1 more source

About trend in zinc stellar abundances with metallisity

open access: yesOdessa Astronomical Publications, 2007
We have carried out investigation of zinc abundance behavior in wide range of stellar metallicities from 0 to -5. It has been determined zinc abundance using our Zn atom model and NonLTE calculation method.
U. Sh. Bayazitov, F. Thevenin
doaj   +1 more source

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