The Unavoidable Persistence of Forum Shopping in European Insolvency Law

Mucciarelli, Federico Maria

doi:10.2139/ssrn.2375654

Cited by 14 publications

(8 citation statements)

References 2 publications

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“…The chemical abundances of Fe and Na have been derived with the package GALA (Mucciarelli et al 2013a) by matching measured and theoretical equivalent widths (EWs) of a set of unblended lines. EWs and radial velocities (RVs) have been measured with the code DAOSPEC (Stetson & Pancino 2008), automatically launched by using the package 4DAO (Mucciarelli 2013), that allows a visual inspection of all the performed Gaussian fits. We started by adopting as input value the nominal full width at half-maximum (FWHM) of the gratings, leaving DAOSPEC free to re-adjust the FWHM in order to minimize the median value of the residuals distribution (see Stetson & Pancino 2008).…”

Section: Discussionmentioning

confidence: 99%

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

Mucciarelli

Dalessandro

Massari

et al. 2016

ApJ

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We present the first measure of Fe and Na abundances in NGC 6362, a low-mass globular cluster (GC) where firstand second-generation stars are fully spatially mixed. A total of 160 member stars (along the red giant branch (RGB) and the red horizontal branch (RHB)) were observed with the multi-object spectrograph FLAMES at the Very Large Telescope. We find that the cluster has an iron abundance of [Fe/H] = −1.09 ± 0.01 dex, without evidence of intrinsic dispersion. On the other hand, the [Na/Fe] distribution turns out to be intrinsically broad and bimodal. The Na-poor and Na-rich stars populate, respectively, the bluest and the reddest RGBs detected in the color-magnitude diagrams including the U filter. The RGB is composed of a mixture of first-and secondgeneration stars in a similar proportion, while almost all the RHB stars belong to the first cluster generation. To date, NGC 6362 is the least massive GC where both the photometric and spectroscopic signatures of multiple populations have been detected.

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Section: Discussionmentioning

confidence: 99%

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

Mucciarelli

Dalessandro

Massari

et al. 2016

ApJ

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“…Abundances of Fe have been derived from the measured equivalent widths using the GALA code (Mucciarelli et al 2013), while the equivalent widths have been measured with the DAOSPEC code (Stetson & Pancino 2008) managed through the wrapper 4DAO (Mucciarelli 2013). The abundances of Li and Na have been obtained through a χ 2 -minimisation between the observed and synthetic spectra (the latter calculated with the SYNTHE code, Kurucz 2005).…”

Section: Observations and Data Analysismentioning

confidence: 99%

The discovery of a Li/Na-rich giant star in Omega Centauri: formed from the pure ejecta of super-AGB stars?

Mucciarelli

Monaco

Bonifacio

et al. 2019

A&A

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We report the discovery of two Li-rich giant stars (fainter than the red giant branch bump) in the stellar system Omega Centauri using GIRAFFE-FLAMES spectra. These two stars have A(Li)=1.65 and 2.40 dex and they belong to the main population of the system ([Fe/H]=-1.70 and -1.82, respectively). The most Li-rich of them (#25664) has [Na/Fe]=+0.87 dex that is ∼0.5 dex higher than those measured in the most Na-rich stars of Omega Centauri of similar metallicity. The chemical abundances of Li and Na in #25664 can be qualitatively explained by deep extra mixing efficient within the star during its RGB evolution or by super-asymptotic giant branch (AGB) stars with masses between ∼7 and 8 M ⊙ . In the latter scenario, this Li-Na-rich star could be formed from the pure ejecta of super-AGB stars before the dilution with pristine material occurs, or, alternatively, be part of a binary system and experienced mass transfer from the companion when this latter evolved through the super-AGB phase. In both these cases, the chemical composition of this unique object could allow to look for the first time at the chemical composition of the gas processed in the interior of super-AGB stars.

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“…The iron abundances have been derived by comparing observed and theoretical equivalent widths (EWs) by means of the code GALA (Mucciarelli et al 2013a). EWs have been measured with the code DAOSPEC (Stetson & Pancino 2008) run through the wrapper 4DAO (Mucciarelli 2013) that allows a visual inspection of the best-fit Gaussian profile for each individual line. Model atmospheres have been computed with the code ATLAS9 2 assuming 1-dimensional, plane-parallel geometry, no overshooting in the computation of the convective flux and adopting the new opacity distribution functions by computed with an enhanced chemical composition for the α-elements (while for all the other elements a solar [X/Fe] abundance ratio is assumed).…”

Section: Iron Abundancementioning

confidence: 99%