J/ApJ/733/L51ivo://CDS.VizieR/J/ApJ/733/L51doi:10.26093/cds/vizier.17339051CDSCasanellas J.Lopes I.2013-01-06T09:22:53Z2012-12-19T09:56:58ZCDS support team

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

cds-question@unistra.fropen-star-clustersastronomical-modelsstellar-evolutionary-tracksIn order to characterize how dark matter (DM) annihilation inside stars changes the aspect of a stellar cluster, we computed the evolution until the ignition of the He burning of stars from 0.7M_{sun}_ to 3.5M_{sun}_ within halos of DM with different characteristics. We found that, when a cluster is surrounded by a dense DM halo, the positions of the cluster' stars in the H-R diagram have a brighter and hotter turnoff point than in the classical scenario without DM, therefore giving the cluster a younger appearance. The high DM densities required to produce these effects are expected only in very specific locations, such as near the center of our Galaxy. In particular, if DM is formed by the 8 GeV weakly interacting massive particles recently invoked to reconcile the results from direct detection experiments, then this signature is predicted for halos of DM with a density {rho}_{chi}_=3x10^5^GeV/cm^3^. A DM density gradient inside the stellar cluster would result in a broader main sequence, turnoff, and red giant branch regions. Moreover, we found that for very high DM halo densities the bottom of the isochrones in the H-R diagram rises to higher luminosities, leading to a characteristic signature on the stellar cluster. We argue that this signature could be used to indirectly probe the presence of DM particles in the location of a cluster.2011ApJ...733L..51Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/733/L51CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/717/257 : Synthetic spectra of dark stars (Zackrisson+, 2010)J/ApJ/703/1323 : Stars in the Galaxy's nuclear cluster (Do+ 2009J/A+A/499/483 : NIR obs. of sources in galactic center (Buchholz+, 2009)J/A+AS/141/371 : Low-mass stars evolutionary tracks+isochrones (Girardi+, 2000)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/733/L51https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/733/L51http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/733/L51https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/733/L51https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/733/L51http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/733/L51GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/733/L51/table1Isochrones of stellar clusters embedded in halos of dark matter particles with different dark matter densitiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintrho[0,1.e10] Dark matter density {rho} (1)GeV.cm**-3phys.densityfloatAge[25/13000] Isochrone ageMyrtime.ageintf_Age[a] conservative estimation of Age (2)meta.codecharMass[0.7/3.5] Isochrone masssolMassphys.massdoublelogTlog of the isochrone effective temperaturelog(K)phys.temperature.effectivedoublelogLlog of the isochrone luminositylog(solLum)phys.luminositydouble