FILACCHIONE, GIANRICOGIANRICOFILACCHIONERAPONI, AndreaAndreaRAPONICAPACCIONI, FABRIZIOFABRIZIOCAPACCIONICIARNIELLO, MauroMauroCIARNIELLOTOSI, FedericoFedericoTOSICapria, M. T.M. T.CapriaDE SANCTIS, MARIA CRISTINAMARIA CRISTINADE SANCTISMIGLIORINI, AlessandraAlessandraMIGLIORINIPICCIONI, GIUSEPPEGIUSEPPEPICCIONICerroni, P.P.CerroniBarucci, M. A.M. A.BarucciFornasier, S.S.FornasierSchmitt, B.B.SchmittQuirico, E.E.QuiricoErard, S.S.ErardBockelee-Morvan, D.D.Bockelee-MorvanLeyrat, C.C.LeyratArnold, G.G.ArnoldMENNELLA, VitoVitoMENNELLAAmmannito, E.E.AmmannitoBELLUCCI, GiancarloGiancarloBELLUCCIBenkhoff, J.J.BenkhoffBibring, J. P.J. P.BibringBlanco, A.A.BlancoBlecka, M. I.M. I.BleckaCarlson, R.R.CarlsonCarsenty, U.U.CarsentyCOLANGELI, LuigiLuigiCOLANGELICombes, M.M.CombesCombi, M.M.CombiCrovisier, J.J.CrovisierDrossart, P.P.DrossartEncrenaz, T.T.EncrenazFederico, C.C.FedericoFink, U.U.FinkFonti, S.S.FontiFulchignoni, M.M.FulchignoniIp, W. -H.W. -H.IpIrwin, P.P.IrwinJaumann, R.R.JaumannKuehrt, E.E.KuehrtLangevin, Y.Y.LangevinMagni, G.G.MagniMcCord, T.T.McCordMoroz, L.L.MorozMottola, S.S.MottolaPALOMBA, ErnestoErnestoPALOMBASchade, U.U.SchadeStephan, K.K.StephanTaylor, F.F.TaylorTiphene, D.D.TipheneTozzi, G. P.G. P.TozziBeck, P.P.BeckBiver, N.N.BiverBonal, L.L.BonalCombe, J. -Ph.J. -Ph.CombeDespan, D.D.DespanFlamini, E.E.FlaminiFORMISANO, MichelangeloMichelangeloFORMISANOFRIGERI, ALESSANDROALESSANDROFRIGERIGRASSI, DavideDavideGRASSIGudipati, M. S.M. S.GudipatiKappel, D.D.KappelLongobardo, A.A.LongobardoMancarella, F.F.MancarellaMarkus, K.K.MarkusMerlin, F.F.MerlinOROSEI, ROBERTOROBERTOOROSEIRINALDI, GIOVANNAGIOVANNARINALDICARTACCI, MARCOMARCOCARTACCICicchetti, A.A.CicchettiHello, Y.Y.HelloHenry, F.F.HenryJacquinod, S.S.JacquinodReess, J. M.J. M.ReessNOSCHESE, RAFFAELLARAFFAELLANOSCHESEPOLITI, ROMOLOROMOLOPOLITIPeter, G.G.Peter2020-05-122020-05-1220160036-8075http://hdl.handle.net/20.500.12386/24717Carbon dioxide (CO<SUB>2</SUB>) is one of the most abundant species in cometary nuclei, but because of its high volatility, CO<SUB>2</SUB> ice is generally only found beneath the surface. We report the infrared spectroscopic identification of a CO<SUB>2</SUB> ice-rich surface area located in the Anhur region of comet 67P/Churyumov-Gerasimenko. Spectral modeling shows that about 0.1% of the 80- by 60-meter area is CO<SUB>2</SUB> ice. This exposed ice was observed a short time after the comet exited local winter; following the increased illumination, the CO<SUB>2</SUB> ice completely disappeared over about 3 weeks. We estimate the mass of the sublimated CO<SUB>2</SUB> ice and the depth of the eroded surface layer. We interpret the presence of CO<SUB>2</SUB> ice as the result of the extreme seasonal changes induced by the rotation and orbit of the comet. <P />STAMPAenArticle10.1126/science.aag31612-s2.0-84996565696000390254300046https://science.sciencemag.org/content/sci/354/6319/1563.full.pdfhttps://science.sciencemag.org/content/354/6319/15632016Sci...354.1563FFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation