Protoplanetary Disks and Their Evolution
Open accessAbstract
Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical units are found around almost all low-mass stars shortly after their birth. These disks generally persist for several million years, during which time some material accretes onto the star, some is lost through outflows and photoevaporation, and some condenses into centimeter- and larger-sized bodies or planetesimals. Through observations mainly at IR through millimeter wavelengths, we can determine how common disks are at different ages; measure basic properties including mass, size, structure, and composition; and follow their varied evolutionary pathways. In this way, we see the first steps toward exoplanet formation and learn about the origins of the Solar System. This review addresses observations of the outer parts, beyond 1 AU, of protoplanetary disks with a focus on recent IR and (sub)millimeter results and an eye to the promise of new facilities in the immediate future.
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Circumstellar gas-rich disks disperse on timescales of <10 Myr, effectively limiting the runaway growth phase for gas giant planets.
“Circumstellar gas-rich disks disperse on timescales of <10 Myr, effectively limiting the runaway growth phase for gas giant planets (Williams & Cieza 2011).”
From MODELING GIANT EXTRASOLAR RING SYSTEMS IN ECLIPSE AND THE CASE OF J1407B: SCULPTING BY EXOMOONS? (2015) · cites this paper as Williams & Cieza 2011
Section 5.5 (p. 23) says gaseous inner disks last less than approximately 10 Myr, but cautions that significant gas may persist longer at larger radii. Section 5 (p. 19) says disk lifetime limits the time available for planet formation; it does not specifically identify the runaway growth phase of gas giants. (LLM, conf=0.87)
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Cites
On the Gravitational Stability of a Disk of Stars
Toomre, A. (1964) · The Astrophysical Journal · doi:10.1086/147861 · Cited by 3,349 · cited 1× · see citing works
“…high during the initial stages of formation (§3), the Toomre Q parameter, Q(R) = cΩ/πGΣ where c is the sound speed and Ω the orbital angular velocity (Toomre 1964), is generally much greater than unity for these Class II YSO disks implying that they are gravitationally stable at all radii…”
BackgroundProtoplanetary disk structures in Ophiuchus
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A <i>Spitzer Space Telescope</i> Study of Disks in the Young σ Orionis Cluster
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High‐Resolution Submillimeter Constraints on Circumstellar Disk Structure
Andrews, S. M., & Williams, J. P. (2007) · The Astrophysical Journal · doi:10.1086/511741 · Cited by 426 · see citing works
Self-citationAn Edge-on Circumstellar Disk in the Young Binary System HK Tauri
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“UY Aur (Duvert et al. 1998) and CoKu Tau 4 (Ireland & Kraus 2008) are additional examples of primordial circumbinary disks but they appear to be rare exceptions rather than the rule.”
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MODELING GIANT EXTRASOLAR RING SYSTEMS IN ECLIPSE AND THE CASE OF J1407B: SCULPTING BY EXOMOONS?
Kenworthy, M. A., & Mamajek, E. E. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/800/2/126 · Cited by 123 · see citing works
“Circumstellar gas-rich disks disperse on timescales of 10 Myr, effectively limiting the runaway growth phase for gas giant planets (Williams & Cieza 2011).”
BackgroundDynamics of Planetary Systems within Star Clusters: Aspects of the Solar System’s Early Evolution
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ALMA and NACO observations towards the young exoring transit system J1407 (V1400 Cen)
Kenworthy, M. A., Klaassen, P. D., Min, M., van der Marel, N., Bohn, A. J., Kama, M., Triaud, A., Hales, A., Monkiewicz, J., Scott, E., et al. (2020) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201936141 · Cited by 5 · see citing works
“Models for the luminosity of the central substellar object are taken from Baraffe et al. (2008) for an age of 16 Myr.”
BackgroundInfluentialK2 discovery of a circumsecondary disk transiting EPIC 220208795
van der Kamp, L., van Dam, D. M., Kenworthy, M. A., Mamajek, E. E., & Pojmański, G. (2022) · Astronomy & Astrophysics · doi:10.1051/0004-6361/202142063 · Cited by 3 · see citing works
- Authors
- Williams, J. P., & Cieza, L. A.
- Affiliations
- University of Hawaiʻi at Mānoa (US)
- Venue
- Annual Review of Astronomy and Astrophysics
- Publisher
- Annual Reviews
- Published
- 2011-09-22
- Volume
- 49
- Issue
- 1
- Pages
- 67-117
- ISSN
- 0066-4146 (ISSN-L)
- 1545-4282
- OpenAlex
- W2072255376
- Cited by
- 1,403
- References
- 6
- Citations by year
- 2026: 47 · 2025: 64 · 2024: 83 · 2023: 68 · 2022: 72 · 2021: 93 · 2020: 121 · 2019: 105 · 2018: 117 · 2017: 123 · 2016: 129 · 2015: 111 · 2014: 85 · 2013: 109 · 2012: 54
- FWCI
- 8.30
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Annual Review of Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- protoplanetary disks, disk evolution, low-mass stars, planet formation, photoevaporation, disk outflows, planetesimals, exoplanet formation, solar system formation
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