Stellar Abundances in a Sentence

What is/are Stellar Abundances?

Stellar Abundances - </p><p>Here, we constrain exoplanetary diversity in terms of bulk planet composition, based on observations of stellar abundances in the Solar neighbourhood. ^[1] The retrieved H2O abundance (∼1%) suggests a superstellar atmospheric metallicity, though stellar or substellar abundances remain consistent with present observations (O/H = 0. ^[2] Even if the internal coherence of the stellar abundances in the same cluster is high, typically 0. ^[3] Theoretical prediction of surface stellar abundances of light elements–lithium, beryllium, and boron–represents one of the most interesting open problems in astrophysics. ^[4] We derive stellar abundances of Co, Zr, La, Ce, Pr, Nd, Er, and Lu using one-dimensional, local thermodynamic equilibrium codes and model atmospheres in conjunction with state-of-the art yield predictions. ^[5] This work assesses to what extent the devolatilised stellar abundances reflect rocky planetary composition. ^[6] The high interstellar abundances of polycyclic aromatic hydrocarbons (PAHs) and their size distribution are the result of complex chemical processes implying dust, UV radiation, and the main gaseous components (H, C, and O). ^[7] Though the neutrino-driven convection model for the core-collapse explosion mechanism has received strong support in recent years, there are still many uncertainties in the explosion parameters -- such as explosion energy, remnant mass, and end-of-life stellar abundances as initial conditions. ^[8] In addition to its high stellar density, the Galactic center/nuclear star cluster is also extreme in hosting high stellar abundances, compared to the surrounding inner bulge stellar populations; this has implications for formation scenarios and strengthens the case for the NSC being a distinct stellar system. ^[9] We elaborate a model that matches the pristine stellar abundances, assuming that all stars are depleted by 0. ^[10] We show how merging neutron stars can be responsible for the production of heavy elements in the solar vicinity, in particular we study the evolution of the abundance of europium (Eu) relative to iron (Fe), as derived by stellar abundances measured in the Milky Way halo and disk stars. ^[11] The approach is tested using data from both Chempy and the IllustrisTNG simulation, showing sub-percent agreement between inferred and true parameters using data from up to 1600 individual stellar abundances. ^[12] We conclude that super-Earth ingestion is a good explanation for the metal enhancement in M67 Y2235, and that a high-resolution spectroscopic survey of stellar abundances around the turn-off and main sequence of M67 has the potential to constrain the frequency of late-time dynamical instability in planetary systems. ^[13] We combine the size of these regions with the stellar abundances in the Milky Way disk and modulate our result with the expected radial abundance of planets via a generalized Titius-Bode law, as statistics of exoplanet orbits seem to point to its adequateness. ^[14] The pursuit of more realistic spectroscopic modelling and consistent abundances has led us to begin a new series of papers designed to improve current solar and stellar abundances of various atomic species. ^[15] But large surveys of stellar abundances show that this is not true. ^[16] 7$, by crossmatching the Stellar Abundances for Galactic Archaeology database to the second data release of Gaia. ^[17] Chemical tagging seeks to identify unique star formation sites from present-day stellar abundances. ^[18] Their ratios with respect to SMC stellar abundances reflect the effects of dust depletion and partial dust destruction in SNR shocks. ^[19]

stellar abundances reflect

This work assesses to what extent the devolatilised stellar abundances reflect rocky planetary composition. ^[1] Their ratios with respect to SMC stellar abundances reflect the effects of dust depletion and partial dust destruction in SNR shocks. ^[2]