Results 71 to 80 of about 4,471,573 (294)

Generalization of radiative jet energy loss to non-zero magnetic mass

open access: yes, 2011
Reliable predictions for jet quenching in ultra-relativistic heavy ion collisions require accurate computation of radiative energy loss. With this goal, an energy loss formalism in a realistic finite size dynamical QCD medium was recently developed ...
Armesto   +40 more
core   +1 more source

Crystallinity versus mass-loss rate in Asymptotic Giant Branch stars [PDF]

open access: yes, 2001
Infrared Space Observatory (ISO) observations have shown that O-rich Asymptotic Giant Branch (AGB) stars exhibit crystalline silicate features in their spectra only if their mass-loss rate is higher than a certain threshold value.
de Koter, A.   +3 more
core   +3 more sources

Conserved structural motifs in PAS, LOV, and CRY proteins regulate circadian rhythms and are therapeutic targets

open access: yesFEBS Letters, EarlyView.
Cryptochrome and PAS/LOV proteins play intricate roles in circadian clocks where they act as both sensors and mediators of protein–protein interactions. Their ubiquitous presence in signaling networks has positioned them as targets for small‐molecule therapeutics. This review provides a structural introduction to these protein families.
Eric D. Brinckman   +2 more
wiley   +1 more source

O-star mass-loss rates at low metallicity

open access: yes, 2012
Mass fluxes J are computed for the extragalactic O stars investigated by Tramper et al. (2011; TSKK). For one early-type O star, computed and observed rates agree within errors. However, for two late-type O stars, theoretical mass-loss rates underpredict
Bouret   +12 more
core   +1 more source

Structural instability impairs function of the UDP‐xylose synthase 1 Ile181Asn variant associated with short‐stature genetic syndrome in humans

open access: yesFEBS Letters, EarlyView.
The Ile181Asn variant of human UDP‐xylose synthase (hUXS1), associated with a short‐stature genetic syndrome, has previously been reported as inactive. Our findings demonstrate that Ile181Asn‐hUXS1 retains catalytic activity similar to the wild‐type but exhibits reduced stability, a looser oligomeric state, and an increased tendency to precipitate ...
Tuo Li   +2 more
wiley   +1 more source

Comparison of the formation and development of cavitation damage on cast and sintered samples based on basalt [PDF]

open access: yesJournal of Mining and Metallurgy. Section A: Mining, 2019
The paper examines the resistance to the effect of cavitation of glass-ceramics based on basalt. Two types of samples were investigated: cast and sintered samples based on basalt.The cavitation erosion test was performed using the ultrasonic vibratory ...
Pavlović M.   +3 more
doaj  

Stellar adiabatic mass loss model and applications

open access: yes, 2010
Roche-lobe overflow and common envelope evolution are very important in binary evolution, which is believed to be the main evolutionary channel to hot subdwarf stars. The details of these processes are difficult to model, but adiabatic expansion provides
B. Paxton   +20 more
core   +1 more source

Eddington and Mass Loss [PDF]

open access: yesHighlights of Astronomy, 1983
AbstractThis joint discussion is dedicated to the memory of Sir Arthur Eddington who was born 100 years ago. He laid the foundation of much work on stellar evolution, which was summed up in his book The Internal Constitution of the Stars (ICS) which appeared in 1926.
openaire   +1 more source

Cell wall target fragment discovery using a low‐cost, minimal fragment library

open access: yesFEBS Letters, EarlyView.
LoCoFrag100 is a fragment library made up of 100 different compounds. Similarity between the fragments is minimized and 10 different fragments are mixed into a single cocktail, which is soaked to protein crystals. These crystals are analysed by X‐ray crystallography, revealing the binding modes of the bound fragment ligands.
Kaizhou Yan   +5 more
wiley   +1 more source

First Stars. I. Evolution without mass loss

open access: yes, 2010
The first generation of stars was formed from primordial gas. Numerical simulations suggest that the first stars were predominantly very massive, with typical masses M > 100 Mo.
A. Ferrara   +57 more
core   +1 more source

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