Results 81 to 90 of about 9,884 (228)
Trojan Horse Investigation for AGB Stellar Nucleosynthesis
Asymptotic Giant Branch (AGB) stars are among the most important astrophysical sites influencing the nucleosynthesis and the chemical abundances in the Universe. From a pure nuclear point of view, several processes take part during this peculiar stage of
Maria Letizia Sergi +17 more
doaj +1 more source
Vortices in the Wakes of Asymptotic Giant Branch Stars [PDF]
Vortices have been postulated at a range of size scales in the universe, including at the stellar-size scale. While hydrodynamically simulating the wind from an asymptotic giant branch (AGB) star moving through and sweeping up its surrounding interstellar medium (ISM), we have found vortices on the size scale of 10-1 to 101 pc in the wake of the star ...
Wareing, C. J. +2 more
openaire +2 more sources
The stellar spectral features of nearby galaxies in the near infrared: tracers of thermally pulsing asymptotic giant branch stars? [PDF]
We analyze the stellar absorption features in high signal-to-noise ratio near-infrared (NIR) spectra of the nuclear region of 12 nearby galaxies, mostly spirals.
R. Riffel +14 more
semanticscholar +1 more source
Random planar trees and the Jacobian conjecture
Abstract We develop a probabilistic approach to the celebrated Jacobian conjecture, which states that any Keller map (i.e. any polynomial mapping F:Cn→Cn$F\colon \mathbb {C}^n \rightarrow \mathbb {C}^n$ whose Jacobian determinant is a non‐zero constant) has a compositional inverse which is also a polynomial. The Jacobian conjecture may be formulated in
Elia Bisi +5 more
wiley +1 more source
Asymptotic giant branch stars in the Phoenix dwarf galaxy [PDF]
JHKs near-infrared photometry of stars in the Phoenix dwarf galaxy is presented and discussed. Combining these data with the optical photometry of Massey et al. allows a rather clean separation of field stars from Phoenix members. The discovery of a Mira variable (P = 425 days), which is almost certainly a carbon star, leads to an estimate of the ...
Menzies, J. W +5 more
openaire +3 more sources
Dust from asymptotic giant branch stars: relevant factors and modelling uncertainties [PDF]
The dust formation process in the winds of Asymptotic Giant Branch stars is discussed, based on full evolutionary models of stars with mass in the range 1M⊙ 6M6 8M⊙, and metallicities 0.001 < Z < 0.008. Dust grains are assumed to form in an isotropically
P. Ventura +8 more
semanticscholar +1 more source
This study introduces a novel fractal–fractional extension of the Hodgkin–Huxley model to capture complex neuronal dynamics, with particular focus on intrinsically bursting patterns. The key innovation lies in the simultaneous incorporation of Caputo–Fabrizio operators with fractional order α for memory effects and fractal dimension τ for temporal ...
M. J. Islam +4 more
wiley +1 more source
Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters
To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s -process elements in post-AGB stars in Galactic globular ...
William V. Dixon
doaj +1 more source
Goos–Hänchen effect singularities in transdimensional plasmonic films
Abstract We identify and classify topologically protected singularities for the reflection coefficient of transdimensional plasmonic systems. Originating from nonlocal electromagnetic response due to vertical electron confinement in the system, such singularities lead to lateral (angular) Goos–Hänchen shifts on the millimeter (milliradian) scale in the
Svend‐Age Biehs, Igor V. Bondarev
wiley +1 more source
Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
We have analyzed high-dispersion spectra in the Li 6708 Å region for 167 stars within the anticenter cluster NGC 2204. From 105 probable members, abundance analysis of 45 evolved stars produces [Fe/H] = −0.40 ± 0.12, [Si/Fe] = 0.14 ± 0.12, [Ca/Fe] = 0.29
Barbara J. Anthony-Twarog +4 more
doaj +1 more source

