Initial Conditions of Planet Formation: Lifetimes of Primordial Disks

By Eric Mamajek. 2009

207 citations recorded by the source corpus.

The statistical properties of circumstellar disks around young stars are important for constraining theoretical models for the formation and early evolution of planetary systems. In this brief review, I survey the literature related to ground‐based and Spitzer‐based infrared (IR) studies of young stellar clusters, with particular emphasis on tracing the evolution of primordial (“protoplanetary”) disks through spectroscopic and photometric diagnostics. The available data demonstrate that the fraction of young stars with optically thick primordial disks and/or those which show spectroscopic evidence for accretion appears to approximately follow an exponential decay with characteristic time ∼2.5 Myr (half‐life ∼1.7 Myr). Large IR surveys of ∼2–5 Myr‐old stellar samples show that there is real cluster‐by‐cluster scatter in the observed disk fractions as a function of age. Recent Spitzer surveys have found convincing evidence that disk evolution varies by stellar mass and environment (binarity, proximity to ma...

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/aee878f4c7f1048b4b02208601a0f4db74383658

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Citations in the corpus

GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, background): “0.5Myr (e.g., Haisch et al. 2001; Mamajek 2009).”
INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, background): “For pre-MS stars, systematic errors in ages may systematically shift the inferred timescales for protoplanetary disk dissipation and giant planet formation (e.g., Mamajek 2009; Bell et al. 2013).”
Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “…decreasing fraction of stars which have a JHKL excess as a function of mean cluster age in Haisch et al. (2001), or an exponential decrease of this fraction with time as exp(−t/2.5 Myr), which is based on more recent compilations of disk lifetimes as in Mamajek (2009) or Fedele et al. (2010).”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “From Figure 2 of Ikoma & Hori (2012), gas accretion onto cores is slowed within hotter and dustier disks, but gas disk lifetimes of tdisk ∼ 0.5–10 Myr (Mamajek 2009; Alexander et al. 2014) are long enough that 10-”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “CB chondrites are dated to ∼ 4.8 Myr after CAIs (Bollard et al., 2015).”
Protoplanetary Disks and Their Evolution (2011, unknown): “The decrease has also been modeled as an exponential with e-folding time 2.5Myr (Mamajek 2009).”
A REVISED AGE FOR UPPER SCORPIUS AND THE STAR FORMATION HISTORY AMONG THE F-TYPE MEMBERS OF THE SCORPIUS–CENTAURUS OB ASSOCIATION (2011, background): “Ages of stellar populations are a critical key to determining the evolutionary timescales of various stages of circumstellar disk evolution and, together with the accretion disk fraction, constrain planet formation timescales (e.g., Chen et al. 2011; Mamajek 2009).”
THE ROLE OF MULTIPLICITY IN DISK EVOLUTION AND PLANET FORMATION (2011, background): “Most surveys of the disk frequency as a function of age have suggested that the disk frequency declines as a linear or exponential function over time (Haisch et al. 2001; Furlan et al. 2006; Hernández et al. 2007; Hillenbrand 2008; Mamajek 2009).”
The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, methodology): “This is ∼2 Myr longer than the timescale estimated in Mamajek (2009), and would imply a longer timescale available for planet formation, but consistent with the findings of Bell et al. (2013).”
Astrochemistry and compositions of planetary systems (2020, background): “The protoplanetary disk stage lasts for ∼1–10 Myrs based on disk occurrence rates in stellar clusters with known median ages (Mamajek 2009).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “…0.5 Myr, with a similar duration for Flat SEDs, assuming a continuous flow through the classes for at least the Class II duration of 2 ± 1 Myr (e.g., Mamajek 2009), which is essentially the age when about half the stars in a dated cluster lack infrared excesses; hence all durations can be…”