## Based on the same MC1−8− survey data, the relative elemental abundances in the graphite sample were also assessed.

The relative yields of trace-element-carbide anions from a Cs+-sputtered graphite target and their use for evaluating the long-term ion source memory in AMS

## The relative elemental abundances in the condensed dust are highly affected by the thermal history of the disc.

Dust Condensation in Evolving Discs and the Composition of Meteorites, Planetesimals, and Planets

## In the Sun, their relative contribution to individual elemental abundances is well understood, except for the lightest and heaviest elements beyond iron.

The Abundance of Lead in Four Metal-poor Stars

## We present the determination of stellar parameters and individual elemental abundances for 6 million stars from $\sim$8 million low-resolution ($R\sim1800$) spectra from LAMOST DR5.

Abundance Estimates for 16 Elements in 6 Million Stars from LAMOST DR5 Low-Resolution Spectra

## We use the updated chemical network to model the sulfur chemistry in Taurus Molecular Cloud 1 (TMC 1) based on molecular abundances determined from Gas phase Elemental abundances in Molecular CloudS (GEMS) project observations.

Gas phase Elemental abundances in Molecular cloudS (GEMS)

## Gas phase Elemental abundances in Molecular CloudS (GEMS) is an IRAM 30 m Large Program designed to provide estimates of the S, C, N, and O depletions and gas ionization degree, X(e−), in a selected set of star-forming filaments of Taurus, Perseus, and Orion.

Gas phase Elemental abundances in Molecular cloudS (GEMS)

## Palynological and down-core XRF elemental abundances from a peat core from Lake Neor enabled a reconstruction of vegetational changes of the past 7000 years over the highlands of northwestern Iran.

Lake Neor reveals how mountain vegetation responded to 7000 years of hydroclimate variability in northwestern Iran

## We utilized a radiocarbon-based age-depth model integrated with lithological, XRF elemental abundances, and principal component analyses to infer changes in erosion/precipitation, lake productivity, and lake water chemistry.

A progressively wetter early through middle Holocene climate in the eastern lowlands of Guatemala

## Our results yield average values for the carbon-to-nitrogen ratio and nitrogen elemental abundances of [C/N]AF = 1.

Warm ISM in the Sgr A complex

## The second is an abrupt, positive Pb-isotope-ratio excursion toward higher values during the Mississippian period between 1150 1GSA Data Repository item 2019403, description of the methods of sample collection, Avery Lake core stratigraphy, age control, organic carbon and total nitrogen elemental abundances and isotopic composition, pollen, and X-ray fluorescence geochemistry, and the Pb pollution calculations using XRF data, is available online at http://www.

Pre-Columbian lead pollution from Native American galena processing and land use in the midcontinental United States

## Comparison between the derived elemental abundances and those predicted values by asymptotic giant branch (AGB) star nucleosynthesis models indicates that the progenitor is a star with initial mass of ~1.

Physical properties of the fullerene C60-containing planetary nebula SaSt2-3

## We have derived elemental abundances of eight RV Tauri-type post-asymptotic giant branch stars: AR Sgr, CE Vir, DY Aql, HP Lyr, SS Gem, SZ Mon, TT Oph, and UZ Oph.

Revisiting RV Tauri stars: first ionization potential (FIP) effect1

## The iron fractions of the host stars were calculated from stellar elemental abundances.

A compositional link between rocky exoplanets and their host stars

## Both kinematic information and stellar elemental abundances are needed to reveal their evolution history.

Elemental Abundance Distributions in the (R, V ϕ ) Plane with LAMOST DR5 and Gaia DR2

## This is the science driver of the 4MOST MIlky way Disc And BuLgE High-Resolution (4MIDABLE-HR) survey: to obtain high-resolution spectra at $R \sim 20\,000$ and to provide detailed elemental abundances for large samples of stars in the Galactic disc and bulge.

4MOST Consortium Survey 4: Milky Way Disc and Bulge High-Resolution Survey (4MIDABLE-HR)

## We present the first detailed elemental abundances in the ultra-faint Magellanic satellite galaxies Carina II (Car II) and Carina III (Car III).

Detailed Abundances in the Ultra-faint Magellanic Satellites Carina II and III.

## New elemental abundances for the neutron-capture elements Sr, Nb, Mo, Ru, La, Sm, and Eu are presented for a large sample of 180 barium (Ba) giant stars, a class of chemically peculiar objects that exhibit in their spectra enhancements of the elements created by the s-process, as a consequence of mass transfer between the components of a binary system.

Heavy elements in barium stars

## This study reports, for the first time, Sr and Nd isotope ratios from the mafic rocks in the Manipur Ophiolite Complex (MOC), along with new elemental abundances to show the subduction zone influence.

Subduction-related Manipur Ophiolite Complex, Indo-Myanmar Ranges: elemental and isotopic record of mantle metasomatism

## As such, having accurate knowledge of the solar elemental abundances is crucial for an extremely broad range.

The chemical make-up of the Sun: A 2020 vision

## All investigated stars show near-to-solar elemental abundances.

Elemental abundances in the center of the Galactic Nuclear Disc

## Previous work has assumed that the two percent of halo giants with unusual elemental abundances have been evaporated from globular clusters, but other origins for their abundance signatures, including binary mass transfer, must also be explored.

Discovery of a nitrogen-enhanced metal-poor binary system: Possible evidence for pollution from an extinct massive AGB Star

## The energy spectrum was successfully modeled by a collisional equilibrium plasma emission, where both the plasma and the absorbing wind have unusual elemental abundances particular to the WR stars.

Long-term X-ray variation of the colliding-wind Wolf–Rayet binary WR 125

## It is found that considering systematic uncertainties on the various nuclear ingredients affecting the radiative neutron capture rates, surface elemental abundances are typically predicted within ±0.

The intermediate neutron capture process

## To study this mechanism, we use observations of the surface elemental abundances of groups of stars, which show that at a particular point in stars’ lives, some elemental abundances change according to mixing occurring in the interior.

Thermohaline Mixing in Low-Mass Red Giant Stars

## Geochemical characterization of Shahbazpur structure (Bengal Foredeep) in terms of elemental abundances obtained from INAA are presented by investigating core samples from Shabazpur gas-field, Bangladesh.

Geochemical characterization of miocene core sediments from Shahbazpur gas-wells (Bangladesh) in terms of elemental abundances by instrumental neutron activation analysis

## The combination of multi-band photometry, Gaia proper motion and parallax data, and radial velocities and the metallicity and elemental abundances obtained from low-resolution spectra of halo giants with 4MOST, will yield an unprecedented characterisation of the Milky Way halo and its interface with the thick disc.

4MOST Consortium Survey 1 : The Milky Way Halo Low-Resolution Survey

## It has direct impact on the evolution and final state of massive stars, while also influencing the elemental abundances resulting from nucleosynthesis in such stars.

Impact of $^{16}$O($\gamma$,$\alpha$)$^{12}$C measurements on the $^{12}$C($\alpha,\gamma$)$^{16}$O astrophysical reaction rate

## It has direct impact on the evolution and final state of massive stars and also influences the elemental abundances resulting from nucleosynthesis in such stars.

Impact of O16(e,e′α)C12 measurements on the C12(α,γ)O16 astrophysical reaction rate

## The elemental abundances derived from these infrared spectra are benchmarked against results from high resolution optical spectra of the same stars.

Towards a high resolution view of infrared line formation

## Significance Using spacecraft data and elemental abundances derived from martian meteorites, earlier studies set a paradigm of a volatile- and water-rich Mars relative to Earth.

Potassium isotope composition of Mars reveals a mechanism of planetary volatile retention

10.1051/0004-6361/202039611

## We use the updated chemical network to model the sulfur chemistry in Taurus Molecular Cloud 1 (TMC 1) based on molecular abundances determined from Gas phase Elemental abundances in Molecular CloudS (GEMS) project observations.

Gas phase Elemental abundances in Molecular cloudS (GEMS)

10.1051/0004-6361/202038258

## Elemental abundances of C, N, $\alpha$-elements, iron-peak elements, and several neutron-capture elements are estimated using the equivalent width measurement technique as well as spectrum synthesis calculations in some cases.

Spectroscopic study of CEMP-(s & r/s) stars

## We may have identified a candidate star in the observational database where elemental abundances and kinematic data are available.

First star survivors as metal-rich halo stars that experienced supernova explosions in binary systems

## We integrate previously published noble gas and hydrogen elemental abundances from Genesis targets, as well as preliminary values for K and Fe.

Elemental Abundances of Major Elements in the Solar Wind as Measured in Genesis Targets and Implications on Solar Wind Fractionation

## Several explanations for the impurity of the GW Vir instability strip have been proposed, based on different elemental abundances, metallicity, and helium content.

The Missing Link? Discovery of Pulsations in the Nitrogen-rich PG 1159 Star PG 1144+005

## The complexity of constraining the stellar initial mass function (IMF) in early-type galaxies cannot be overstated, given the necessity of very high signal-to-noise ratio (S/N) data and the difficulty of breaking the strong degeneracies that occur among several stellar population parameters, including age, metallicity, and elemental abundances.

The Stellar Initial Mass Function and Population Properties of M89 from Optical and NIR Spectroscopy: Addressing Biases in Spectral Index Analysis

## One of the purposes of taking spectra for millions of stars through the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) medium-resolution survey (MRS) is to obtain the elemental abundances, so that one can trace the origin and evolution for the element of interests.

The Lithium Abundances from the Large Sky Area Multi-object Fiber Spectroscopic Telescope Medium-resolution Survey. I. The Method

10.1051/0004-6361/202141575

## It is found that considering systematic uncertainties on the various nuclear ingredients affecting the radiative neutron capture rates, surface elemental abundances are typically predicted within ±0.

The intermediate neutron capture process

## New elemental abundances for the neutron-capture elements Sr, Nb, Mo, Ru, La, Sm, and Eu are presented for a large sample of 180 barium (Ba) giant stars, a class of chemically peculiar objects that exhibit in their spectra enhancements of the elements created by the s-process, as a consequence of mass transfer between the components of a binary system.

Heavy elements in barium stars

## 84 dex) stars, we perform stellar parameter analysis and report 12 elemental abundances (C, Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Zn, Ba, and Ce) with precisions of ≈0.

The COMBS Survey - III. The Chemodynamical Origins of Metal-Poor Bulge Stars

10.1016/J.ICARUS.2021.114436

## Elemental abundances for a region in the farside highland and in the nearside western mare are derived demonstrating the method and the instrument capability of deriving the elemental abundances at different spatial scales and at different solar activity levels.

Chandrayaan-2 Large Area Soft X-ray Spectrometer (CLASS): Calibration, In-flight performance and first results

## Estimating age distributions, or star formation histories, of stellar populations in the Milky Way is important in order to study the evolution of trends in elemental abundances and kinematics.

Estimating the age–metallicity distribution of a stellar sample from the probability distributions of the individual stars

## Palynological and down-core XRF elemental abundances from a peat core from Lake Neor enabled a reconstruction of vegetational changes of the past 7000 years over the highlands of northwestern Iran.

Lake Neor reveals how mountain vegetation responded to 7000 years of hydroclimate variability in northwestern Iran

## We present a systematic investigation of physical conditions and elemental abundances in four optically thick Lyman-limit systems (LLSs) at z = 0.

The cosmic ultraviolet baryon survey (CUBS) – III. Physical properties and elemental abundances of Lyman-limit systems at z < 1

## We do this with no ab initio knowledge of elemental abundances themselves and hence bypass the uncertainties and systematics associated with modeling that rely on synthetic stellar spectra.

Disentangled Representation Learning for Astronomical Chemical Tagging

## The composition (including the ionic charge states and elemental abundances) is determined prior to and/or during CME eruptions in the solar atmosphere and does not alter during MC propagation to 1 AU and beyond.

The Inhomogeneity of Composition Along the Magnetic Cloud Axis

10.1016/J.NIMB.2021.05.011

## Based on the same MC1−8− survey data, the relative elemental abundances in the graphite sample were also assessed.

The relative yields of trace-element-carbide anions from a Cs+-sputtered graphite target and their use for evaluating the long-term ion source memory in AMS

## Elemental abundances of the most metal-poor stars reflect the conditions in the early Galaxy and the properties of the first stars.

The Pristine survey XIV: Chemical analysis of two ultra-metal-poor stars

## We test the hypothesis that the observed first-peak (Sr, Y, Zr) and second-peak (Ba) s-process elemental abundances in low-metallicity Milky Way stars, and the abundances of the elements Mo and Ru, can be explained by a pervasive r-process contribution originating in neutrino-driven winds from highly-magnetic and rapidly rotating proto-neutron stars (proto-NSs).

Nucleosynthesis signatures of neutrino-driven winds from proto-neutron stars: a perspective from chemical evolution models

## , temperature) may be effective in determining the elemental abundances of 3He-rich SEPs.

Temperature in Solar Sources of 3He-rich Solar Energetic Particles and Relation to Ion Abundances

10.1051/0004-6361/202140445

## As such, having accurate knowledge of the solar elemental abundances is crucial for an extremely broad range.

The chemical make-up of the Sun: A 2020 vision

## Using time-resolved spectroscopic analysis during these flares, we examined the evolution of temperature, emission measure, and absolute elemental abundances of four elements–Mg, Al, Si, and S.

Evolution of Elemental Abundances during B-Class Solar Flares: Soft X-Ray Spectral Measurements with Chandrayaan-2 XSM

## In the Sun, their relative contribution to individual elemental abundances is well understood, except for the lightest and heaviest elements beyond iron.

The Abundance of Lead in Four Metal-poor Stars

10.1051/0004-6361/202039979

## Elemental abundances were determined using a differential line-by-line spectrum synthesis using the TURBOSPECTRUM code with the MARCS stellar model atmospheres and accounting for the hyperfine-structure effects.

Abundances of neutron-capture elements in thin- and thick-disc stars in the solar neighbourhood

## Could potentially habitable complex brines with extremely low freezing temperatures exist in the shallow subsurface of these frigid worlds? Earth, Mars, and carbonaceous chondrites have similar bulk elemental abundances, but while the Earth is depleted in the most volatile elements, the Icy Worlds of the outer solar system are expected to be rich in them.

Complex Brines and Their Implications for Habitability

10.1007/s10967-021-07770-4

## Geochemical characterization of Shahbazpur structure (Bengal Foredeep) in terms of elemental abundances obtained from INAA are presented by investigating core samples from Shabazpur gas-field, Bangladesh.

Geochemical characterization of miocene core sediments from Shahbazpur gas-wells (Bangladesh) in terms of elemental abundances by instrumental neutron activation analysis

## We analyze the coronal elemental abundances during a small flare using Hinode/EIS observations.

The Evolution of Plasma Composition during a Solar Flare

10.1051/0004-6361/202141775

## Moreover, we calculated the spectrum synthesis of carbon molecular bands and lines due to elements with hyperfine structures to determine the elemental abundances.

The peculiar abundances of HE 1005-1439. A carbon-enhanced extremely metal-poor star contaminated with products of both s- and i-process nucleosynthesis

## Using a combination of elemental abundances and stellar parameters from the GALAH and Apache Point Observatory Galactic Evolution Experiment (APOGEE) surveys, we find that the abundances of the highest likelihood Nyx members are entirely consistent with membership of the thick disk, and inconsistent with a dwarf galaxy origin.

The GALAH Survey: No Chemical Evidence of an Extragalactic Origin for the Nyx Stream

## The elemental abundances derived from these infrared spectra are benchmarked against results from high resolution optical spectra of the same stars.

Towards a high resolution view of infrared line formation

10.1051/0004-6361/202141786

## The transport of icy pebbles has been suggested to alter the local elemental abundances in protoplanetary disks through settling, drift, and trapping in pressure bumps, resulting in a depletion of volatiles in the surface layer and an increase in the elemental C/O.

If you like C/O variations, you should have put a ring on it

## In addition, we have shown that XRF techniques offer an optimal analytical approach for building large data sets containing highly reliable and reproducible results of elemental abundances in wines, corresponding soils, and grape juice.

X-ray Fluorescence Techniques for Element Abundance Analysis in Wine

10.1016/J.CHINASTRON.2021.02.004

## Based on the observed abundances of weak r-process star HD 140283 and theoretical yields of single supernova (SN), we fit the observational elemental abundances (from C to Zn) to the entire library of single SN yield, and derive that HD 140283 may have been born from a nebula polluted by the explosion of supernova whose progenitor mass is 22.

Element Abundance Analysis of HD 140283 and Astrophysics Sources of Weak r-process Elements

## We present elemental abundances and stellar population ages for 65 massive quiescent galaxies at 0.

Elemental Abundances and Ages of z ∼ 0.7 Quiescent Galaxies on the Mass–Size Plane: Implication for Chemical Enrichment and Star Formation Quenching

10.1016/J.EPSL.2021.116807

## We utilized a radiocarbon-based age-depth model integrated with lithological, XRF elemental abundances, and principal component analyses to infer changes in erosion/precipitation, lake productivity, and lake water chemistry.

A progressively wetter early through middle Holocene climate in the eastern lowlands of Guatemala

## To examine the effects of Antarctic alteration and sample heterogeneity on the Sm-Nd and Lu-Hf isotope systematics, ten Antarctic H chondrites (HCs) and three HCs from hot deserts were characterized for their modal abundances, elemental abundances, and Sm-Nd and Lu-Hf isotopic compositions.

The effects of Antarctic alteration and sample heterogeneity on Sm-Nd and Lu-Hf systematics in H chondrites

## The iron fractions of the host stars were calculated from stellar elemental abundances.

A compositional link between rocky exoplanets and their host stars

## Tidal disruption and subsequent accretion of planetesimals by white dwarfs can reveal the elemental abundances of rocky bodies in exoplanetary systems.

Lithium pollution of a white dwarf records the accretion of an extrasolar planetesimal

10.1016/b978-0-12-815948-4.00007-3

## Three observational pillars of the concordance cosmology are: the Hubble diagram, mapping out the expansion history of the late-time universe; Big Bang Nucleosynthesis (BBN), which, combined with measurements of the primordial elemental abundances, constrains the amount of ordinary matter and early-time expansion rate; and the cosmic microwave background (CMB), which provides a view of the perturbations when the universe was less than 400,000 years old.

The concordance model of cosmology

10.1088/1674-4527/21/5/111

## In the early Galaxy, elemental abundances of the extremely metal-poor (EMP) stars contain abundant information about the neutron-capture nucleosynthesis and the chemical enrichment history.

Pollution tracks of r-process material in [Sr/Ba] vs. [Ba/Fe] space for the early Galaxy

10.1051/0004-6361/202039295

## Our results yield average values for the carbon-to-nitrogen ratio and nitrogen elemental abundances of [C/N]AF = 1.

Warm ISM in the Sgr A complex

10.1007/s10686-021-09765-1

## We present here the studies and benchmark analyses we have been performing to determine robust stellar fundamental parameters, elemental abundances, activity indices, and stellar ages.

The homogeneous characterisation of Ariel host stars

## We show that the elemental abundances of the companion star and the planetary material accreted by WD 1425+540 are consistent with the hypothesis that planet and hoststars have the same true abundances, taking into account the observational errors.

Host-star and exoplanet compositions: a pilot study using a wide binary with a polluted white dwarf

## We present a thorough analysis of the elemental abundances of a wide variety of heavy ions, measured by Advanced Composition Explorer/SWICS, in prominence material observed in the solar wind.

Elemental Abundances of Prominence Material inside ICMEs

10.5194/EGUSPHERE-EGU21-6017

## We combined sedimentological, XRF elemental abundances, and principal component (PC) analyses to reconstruct changes in erosion/precipitation, lake productivity, and lake water chemistry during the Holocene.

Holocene climate variability and associated paleoenvironmental changes in the eastern lowlands of Guatemala revealed by a lake sediment from Lake Izabal

## We also derive elemental abundances using the Cloudy synthetic models, and find an excess amount of the s-process element krypton in both targets, which supports their nature as PNe.

Hunting for Planetary Nebulae toward the Galactic Center

## Examination of the elemental abundances (C to Eu) in the GALAH catalogue shows no anomalous abundances in red clump giants and, in particular, no dependence on the Li abundance, which ranges over at least five dex.

Lithium in red giants: the roles of the He-core flash and the luminosity bump

## Elemental abundances measured in the X-ray band have been used to study the chemical enrichment of supernova remnants, elliptical galaxies, groups, and clusters of galaxies.

Elemental Abundances of the Hot Atmosphere of Luminous Infrared Galaxy Arp 299

## , Aridus and Apex) have revolutionized our ability to analyze almost any sample matrix with remarkable precision at exceedingly low elemental abundances.

Translating Analytical Techniques in Geochemistry to Environmental Health

## Stellar atmospheric parameters and elemental abundances are obtained with extremely high precision (<3.

Detailed elemental abundances of binary stars: searching for signatures of planet formation and atomic diffusion

10.1051/0004-6361/202040112

## Gas phase Elemental abundances in Molecular CloudS (GEMS) is an IRAM 30 m Large Program designed to provide estimates of the S, C, N, and O depletions and gas ionization degree, X(e−), in a selected set of star-forming filaments of Taurus, Perseus, and Orion.

Gas phase Elemental abundances in Molecular cloudS (GEMS)

## We use FIRE-2 simulations to examine 3-D variations of gas-phase elemental abundances of [O/H], [Fe/H], and [N/H] in 11 MW and M31-mass galaxies across their formation histories at z ≤ 1.

3D gas-phase elemental abundances across the formation histories of Milky Way-mass galaxies in the FIRE simulations: initial conditions for chemical tagging

10.5194/EGUSPHERE-EGU21-1403

## Core accretion followed by migration is still the favored scenario for the IGPs, considering the latter model does not satisfactorily explain the measured elemental abundances in the giant planets.

Measurements by Probe and Orbiter Critical for Models of Formation and Evolution of Uranus and Neptune

## We find that the light-(N), α-(O, Mg, Si), and Odd-Z (Al) elemental abundances of the stars in VVV CL001 follow the same trend as other Galactic metal-poor globular clusters.

VVV CL001: Likely the Most Metal-poor Surviving Globular Cluster in the Inner Galaxy

## Significance Using spacecraft data and elemental abundances derived from martian meteorites, earlier studies set a paradigm of a volatile- and water-rich Mars relative to Earth.

Potassium isotope composition of Mars reveals a mechanism of planetary volatile retention

## When coupled to a transmission electron microscope (TEM), EDS can provide both qualitative and quantitative information in the form of false-color maps and as (normalized) elemental abundances, respectively, at scales ranging from the micrometer down to the atomic.

Compositional Analysis of Chondritic Sulfide Material: A Test of the Mass-Thickness Approach to Quantitative EDS in the TEM

## We use Gaia kinematics and APOGEE elemental abundances to select stars belonging to the Gaia-Sausage-Enceladus (GSE) and Sequoia accretion events.

Selecting accreted populations: metallicity, elemental abundances, and ages of the Gaia-Sausage-Enceladus and Sequoia populations

## Our model can successfully reproduce the observed HCN column density when the elemental abundances of gas-phase carbon and oxygen are depleted by two orders of magnitude relative to those in the interstellar medium and carbon is more abundant than oxygen ([C/O]elem > 1).

Modeling Nitrogen Fractionation in the Protoplanetary Disk around TW Hya: Model Constraints on Grain Population and Carbon-to-oxygen Elemental Abundance Ratio

## Based on the bulk H, C, and N elemental abundances and isotopic compositions, Flensburg is unique among chondrites, because it has the lightest bulk H and N isotopic compositions of any type 1 or 2 chondrite investigated so far.

The old, unique C1 chondrite Flensburg – Insight into the first processes of aqueous alteration, brecciation, and the diversity of water-bearing parent bodies and lithologies

## By measuring the elemental abundances of a star, we can gain insight into the composition of its initial gas cloud—the formation site of the star and its planets.

Searching For Transiting Planets Around Halo Stars. I. Sample Selection and Validation

10.1007/s11207-021-01852-y

## Composition of interplanetary CMEs (ICMEs), referring to the charge states and elemental abundances of ions, opens an important avenue to investigate CMEs.

Solar Cycle Dependence of ICME Composition

10.1051/0004-6361/202141104

## The elemental abundances in the hot plasma component are significantly higher than those in the ‘cooler’ one, indicating its origin from the reverse shock propagating into the ejecta.

SN1987A: Tracing the flux decline and spectral evolution through a comparison of SRG/eROSITA and XMM-Newton observations

## Here, we aim to combine this up-to-date oxygen determination, which is likely to be more representative of the bulk abundance than the Galileo probe subsolar value, with the other known measurements of elemental abundances in Jupiter, to derive the formation conditions and initial composition of the building blocks agglomerated by the growing planet, and that determine the heavy element composition of its envelope.

The Nature and Composition of Jupiter’s Building Blocks Derived from the Water Abundance Measurements by the Juno Spacecraft

10.1051/0004-6361/201834735

## Elemental abundances in some coronal structures differ significantly from photospheric abundances, with a dependence on the first ionization potential (FIP) of the element.

Measuring relative abundances in the solar corona with optimised linear combinations of spectral lines.

10.1051/0004-6361/201730931

## Elemental abundances are footprints of time-integrated yields of various stellar populations that have left their specific abundance patterns prior to and during the cluster and group evolution.

Nitrogen abundance in the X-ray halos of clusters and groups of galaxies

10.1051/0004-6361/201731482

## We use the observed elemental abundances in dust of several metals (O, S, Si, Mg, and Fe) in different environments, considering systems with different metallicities and dust content, namely damped Lyman-{\alpha} absorbers (DLAs) towards quasars and the Galaxy.

Dust-depletion sequences in damped Lyman-α absorbers. II. The composition of cosmic dust, from low-metallicity systems to the Galaxy

## The relative elemental abundances in the condensed dust are highly affected by the thermal history of the disc.

Dust Condensation in Evolving Discs and the Composition of Meteorites, Planetesimals, and Planets

## We summarize the jet parameters (bulk velocity, opening angle, kinetic luminosity, base temperature, and relative elemental abundances) derived by fitting the data below 3 keV and describe the revealed degeneracies and systematic effects due to the presence of an additional component.

Diagnostics of Parameters for the X-ray Jets of SS 433 from High-Resolution Chandra Spectroscopy

10.1016/J.SCITOTENV.2019.05.263

## Within the same macroalgal species, some elemental abundances (As, I, Pb, Cu, Cd and U) are affected by mixing between freshwater riverine and North Sea marine saltwater.

Tracing the natural and anthropogenic influence on the trace elemental chemistry of estuarine macroalgae and the implications for human consumption.

## The combination of multi-band photometry, Gaia proper motion and parallax data, and radial velocities and the metallicity and elemental abundances obtained from low-resolution spectra of halo giants with 4MOST, will yield an unprecedented characterisation of the Milky Way halo and its interface with the thick disc.

4MOST Consortium Survey 1 : The Milky Way Halo Low-Resolution Survey