J/A+A/690/A262ivo://CDS.VizieR/J/A+A/690/A262doi:10.26093/cds/vizier.36900262CDSBrauner M.Pignatari M.Masseron T.Garcia-Hernandez D.A.Lugaro M.2025-02-24T20:02:07Z2024-10-11T08:57:58ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frpeculiar-variable-starschemically-peculiar-starsspectroscopyThe atmospheres of phosphorus-rich (P-rich) stars have been shown to contain between 10 and 100 times more P than our Sun. Given its crucial role as an essential element for life, it is especially necessary to uncover the origin of P-rich stars to gain insights into the still unknown nucleosynthetic formation pathways of P in our Galaxy. Our objective is to obtain the extensive chemical abundance inventory of four P-rich stars, covering a large range of heavy (Z>30) elements. This characterization will serve as a milestone for the nuclear astrophysics community to uncover the processes responsible for the formation of the unique chemical fingerprint of P-rich stars. We performed a detailed 1D LTE abundance analysis on the optical UVES spectra of four P-rich stars. The abundance measurements, complemented with upper limit estimates, included 48 light and heavy elements. Our focus lies on the neutron-capture elements (Z>30), in particular on the elements between Sr and Ba, as well as Pb, as they provide valuable constraints to nucleosynthesis calculations. In past works, we showed that the heavy elements observations from the first P-rich stars are not compatible with either classical s-process or r-process abundance patterns. In this work, we compare the obtained abundances with three different nucleosynthetic scenarios: a single i-process, a double i-process and a combination of s- and i-process. We have performed the most extensive abundance analysis of P-rich stars to date, including the elements between Sr and Ba, such as Ag, which are rarely measured in any kind of stars. Constraining upper limits could also be estimated for CdI, InI, and SnI. We found overabundances with respect to solar in the s-process peak elements, accompanied by an extremely high Ba abundance and slight enhancements in some elements between Rb and Sn. Regarding the nucleosynthetic origin of the pattern, no global solution explaining all four stars could be found. The model that produces the least number of discrepancies in three of the four stars is a combination of s- and i-process, but the current lack of extensive multi-dimensional hydrodynamic simulations to follow the occurrence of the i-process in different types of stars makes this scenario highly uncertain.2024A&A...690A.262Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/690/A262CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/673/A123 : Phosphorus-rich stars (Brauner+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/690/A262https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/690/A262http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/690/A262https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/690/A262https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/690/A262http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/690/A262GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/690/A262/lightabu (Abundances of the light (Z<30) elements)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/690/A262/lightabu?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/690/A262/lightabu?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/690/A262/lightabu?GETtext/xml+votable180.050000true1.1742119-0.09871560.0055555555555555566/8891 18090 19412 47871https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/690/A262?format=asciidefaultJ/A+A/690/A262/linesLine list of the light and heavy elements including wavelength, excitation potential and oscillator strengthrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElement symbol + excitation statephys.atmol.excitationcharlambdaWavelength in angstrom0.1nmem.wldoublen_lambda[*] Note on lambda (1)meta.notecharEPExcitation potential of the lineeVphys.atmol.excitation;spect.linefloatlog(gf)Oscillator strength of the linespect.line.intensityfloatMol/Isotope?Is line a molecular line, indicating the molecule; or from isotope(s)meta.codecharJ/A+A/690/A262/modifModifications applied on the original VALD log(gf) of transitions close to a line of interestSpecies-modifiedElement symbol + excitation state of the modified speciesphys.atmol.excitationcharlambdaWavelength in angstrom of the modified species0.1nmem.wldoubleEPExcitation potential of modified lineeVphys.atmol.excitation;spect.linefloatlog(gf)VALDOscillator strength of the line before modificationphys.atmol.oscStrengthfloatlog(gf)MODOscillator strength of the line after modificationphys.atmol.oscStrengthfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElement symbol + excitation state of the element to improvephys.atmol.elementcharLine-to-improve? Wavelength in angstrom of the line to improve0.1nmem.wldoublenullablen_log(gf)MOD[+] Note on log(gf)MOD (1)meta.notecharJ/A+A/690/A262/lightabuAbundances of the light (Z<30) elementsSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintElElement symbol + excitation state (1)phys.atmol.excitationcharMolecule?Is abundance derived from molecular lines, indicating the moleculemeta.codecharStarID of the Star, 2MHHMMSSss+DDMMSSsmeta.id;meta.maincharl_[X/Fe]Limit flag on [X/Fe]meta.code.error;phys.abundchar[X/Fe]? Abundance compared to solarphys.abundfloatnullablesigma-std? Line-to-line standard deviationstat.stdevfloatnullableN? Number of linesmeta.numberintnullable_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/690/A262/uncert*Uncertainties associated with the heavy (Z>30) elements due to deviations in atmospheric parametersElElement symbol + excitation statephys.atmol.excitationchardeltaTeffSystematic uncertainty related to effective temperaturestat.errorfloatdeltaloggSystematic uncertainty related to surface gravitystat.errorfloatdeltamicrovelSystematic uncertainty related to microturbulence velocitystat.error.sys;phys.veloc.microTurbfloatsigmaparamThe total uncertainty equal to the square root of the sum of the parameter deviations squaredstat.errorfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint