J/A+A/662/A63ivo://CDS.VizieR/J/A+A/662/A63doi:10.26093/cds/vizier.36620063CDSSuleiman L.Zdunik J.L.Haensel P.Fortin M.2022-10-14T13:54:04Z2022-06-17T14:17:23ZCDS support team

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

cds-question@unistra.fratomic-physicsNeutron stars in low-mass binary systems are subject to accretion when material originating from the companion star accumulates on the surface. In most cases, the justified and common assumption in studying the properties of the neutron star crust is the fully accreted crust approximation. However, observations of some X-ray transient sources indicate that the original crust has not been completely replaced by accreted material, but is partly composed of the compressed original crust. The crust of an accreting neutron star beyond the fully accreted crust approximation was studied; a two-part (or hybrid) crust made of the original crust that is compressed and of the accreted material crashing onto it was reconstructed as a function of the accretion stage. The differences in the composition and energy sources for the fully accreted and hybrid crusts influence the cooling and transport properties. A simple semi-empirical formula of a compressible liquid drop was used to compute the equation of state and composition of the hybrid crust. Calculations were based on the single-nucleus model, with a more accurate treatment of the neutron drip point. We compared the nuclear reactions triggered by compression in the original crust and in the accreted matter part of the hybrid crust. We discuss another crust compression astrophysical phenomenon related to spinning neutron stars. The compression of the originally catalyzed outer crust triggers exothermic reactions (electron captures and pycnonuclear fusions) that deposit heat in the crust. The heat sources are cataloged as a function of the compression until the fully accreted crust approximation is reached. The pressure at which neutron drip occurs is a nonmonotonic function of the depth, leading to a temporary neutron drip anomaly. The additional potential source of energy for partially accreted crusts is the occurrence of a density inversion phenomenon between some compressed layers. The original crust of a neutron star cannot be neglected for the initial period of accretion, when the original crust is not fully replaced by the accreted matter. The amount of heat associated with the compression of the original crust is on the same order of magnitude as that from the sources acting in the accreted part of the hybrid crust.2022A&A...662A..63Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/662/A63CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/662/A63https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/662/A63http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/662/A63https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/662/A63https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/662/A63http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/662/A63GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/662/A63/snmReactions triggered by the compression of an originally catalyzed outer crust (ReactionOCCOCSNM.res)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPiniPressure at the top of the shell in its catalyzed state (1)dyn.cm**-2phys.pressuredoublerhoiniDensity of the shell in its catalyzed state (1)g.cm**-3phys.densitydoubleNucleiOriginal catalyzed nuclei (A,Z,N) (1)phys.atmol.elementcharShell[1/24] Shell number (1)meta.id;meta.mainintPPressure at which the reaction occursdyn.cm**-2phys.pressuredoublerhoDensityg.cm**-3phys.densitydoublelambdaRelative change in density due to the reaction, {Delta}{rho}/{rho}%phys.atmolfloatAiNucleon number of the parent nucleus of the reactionphys.atmol.elementintZiProton number of the parent nucleus of the reactionmeta.numberintAfNucleon number of the daughter nucleus of the reactionphys.atmol.elementintZfProton number of the daughter nucleus of the reactionmeta.numberintNfNeutron number of the daughter nucleus of the reactionmeta.numberintQEnergy per nucleon Q in keV per nucleon of the reactionkeVphys.energy;phys.atmol.leveldoubleDPCompression at which the reaction is triggereddyn.cm**-2phys.atmoldoubledP/PRelative compression at which the reaction is triggered%phys.atmoldoubleJ/A+A/662/A63/contReactions triggered by the compression of an originally catalyzed outer crust calculated with the continuous approach (ReactionOCCOCContinuous.res)rhoiniDensity of the shell in its catalyzed state (1)g.cm**-3phys.densitydoubleNucleiOriginal catalyzed nuclei (A,Z,N) (1)phys.atmol.elementcharShell[1/24] Shell number (1)meta.id;meta.mainintrhoDensityg.cm**-3phys.densitydoublelambdaRelative change in density due to the reaction, {Delta}{rho}/{rho}%phys.atmolfloatAiNucleon number of the parent nucleus of the reactionphys.atmol.elementintZiProton number of the parent nucleus of the reactionmeta.numberintAfNucleon number of the daughter nucleus of the reactionphys.atmol.elementintZfProton number of the daughter nucleus of the reactionmeta.numberintNfNeutron number of the daughter nucleus of the reactionmeta.numberintQEnergy per nucleon Q in keV per nucleon of the reactionkeVphys.energy;phys.atmol.leveldoubleDPCompression at which the reaction is triggereddyn.cm**-2phys.atmoldoubledP/PRelative compression at which the reaction is triggered%phys.atmoldoublePPressure at which the reaction occursdyn.cm**-2phys.pressuredoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPiniPressure at the top of the shell in its catalyzed state (1)dyn.cm**-2phys.pressuredouble