Summary of the properties of circumbinary disks in astrophysical scenarios. Binary mass refers to the initial mass M₀ of the central binary. The disk is fed if there is a mass inflow that replenishes the disk. The disk is self-gravitating if the self-gravity of the disk has a nonnegligible effect on the dynamics and structure of the disk. Disk mass M_d is the instantaneous mass of the disk. Accretion rate is the mass accreted by the binary per unit time. Disk lifetime is the duration of a disk-mediated phase in the binary evolution, terminating when the disk is dispersed or the binary merges. Accreted mass is the amount of mass that can be accreted from the disk on to the binary within the disk lifetime. When the disk is not fed from external mass inflow, the accreted mass can be estimated as M_d/M₀, which assumes that all the mass in the disk is eventually accreted, and neglects outflows or other mechanisms of mass loss. h/r is the disk aspect ratio in the vicinity of the binary. α is the viscosity parameter of the disk. ^[1]Jørgensen et al. (2009), ^[2]Tobin et al. (2020), ^[3]Jacobsen et al. (2018), ^[4]Kido et al. (2023), ^[5]Fiorellino et al. (2023), ^[6]Takakuwa et al. (2014), ^[7]Manara et al. (2020), ^[8]Guilloteau et al. (1999), ^[9]Scaife (2013), ^[10]Dutrey et al. (2016), ^[11]Long et al. (2021), ^[12]Testi et al. (2022), ^[13]Grant et al. (2023), ^[14]Tuna & Metzger (2023), ^[15]Vos et al. (2015), ^[16]Izzard & Jermyn (2023), ^[17]Bujarrabal et al. (2018), ^[18]Kluska et al. (2022), ^[19]Bujarrabal et al. (2013), ^[20]Franchini et al. (2021), ^[21]Novak et al. (2011), ^[22]Schawinski et al. (2015), ^[23]Siwek et al. (2020), ^[24] estimated from Eq. (A.1) assuming r = 100 AU and α = 0.1, ^[25] estimated from Eq. (A.2) assuming r = 0.01 pc, α = 0.1 and η = 0.06, ^[26]Rosotti (2023), ^[27]Starling et al. (2004).