Bonito, RosariaRosariaBonitoVENUTI, LAURALAURAVENUTIUSTAMUJIC SALIHOVIC, SabinaSabinaUSTAMUJIC SALIHOVICYoachim, P.P.YoachimStreet, R. A.R. A.StreetPRISINZANO, LoredanaLoredanaPRISINZANOHartigan, P.P.HartiganGUARCELLO, Mario GiuseppeMario GiuseppeGUARCELLOStassun, K. G.K. G.StassunGIANNINI, TeresaTeresaGIANNINIFeigelson, E. D.E. D.FeigelsonCARATTI O GARATTI, AlessioAlessioCARATTI O GARATTIORLANDO, SalvatoreSalvatoreORLANDOClarkson, W. I.W. I.ClarksonMcGehee, P.P.McGeheeBellm, E. C.E. C.BellmGizis, J. E.J. E.Gizis2025-05-072025-05-0720230067-0049http://hdl.handle.net/20.500.12386/37099Vera C. Rubin Observatory, through the Legacy Survey of Space and Time (LSST), will allow us to derive a panchromatic view of variability in young stellar objects (YSOs) across all relevant timescales. Indeed, both short-term variability (on timescales of hours to days) and long-term variability (months to years), predominantly driven by the dynamics of accretion processes in disk-hosting YSOs, can be explored by taking advantage of the multiband filters option available in Rubin LSST, in particular the u, g, r, i filters that enable us to discriminate between photospheric stellar properties and accretion signatures. The homogeneity and depth of sky coverage that will be achieved with LSST will provide us with a unique opportunity to characterize the time evolution of disk accretion as a function of age and varying environmental conditions (e.g., field crowdedness, massive neighbors, metallicity) by targeting different star-forming regions. In this contribution to the Rubin LSST Survey Strategy Optimization Focus Issue, we discuss how implementing a dense observing cadence to explore short-term variability in YSOs represents a key complementary effort to the Wide-Fast-Deep observing mode that will be used to survey the sky over the full duration of the main survey (≈10 yr). The combination of these two modes will be vital to investigate the connection between the inner-disk dynamics and longer-term eruptive variability behaviors, such as those observed on EX Lupi-type objects.STAMPAenArticle10.3847/1538-4365/acb6842-s2.0-85150071137https://iopscience.iop.org/article/10.3847/1538-4365/acb684https://api.elsevier.com/content/abstract/scopus_id/851500711372023ApJS..265...27BFIS/05 - ASTRONOMIA E ASTROFISICA