The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions
We study the effect of stellar evolution on the dispersal of protoplanetary disks by performing one-dimensional simulations of long-term disk evolution. Our simulations include viscous disk accretion, magnetohydrodynamic winds, and photoevaporation as important disk dispersal processes. We consider...
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2025-01-01
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| author | Ayano Komaki Naoki Yoshida |
| author_facet | Ayano Komaki Naoki Yoshida |
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| description | We study the effect of stellar evolution on the dispersal of protoplanetary disks by performing one-dimensional simulations of long-term disk evolution. Our simulations include viscous disk accretion, magnetohydrodynamic winds, and photoevaporation as important disk dispersal processes. We consider a wide range of stellar mass of 0.1–7 M _⊙ and incorporate the luminosity evolution of the central star. For solar-mass stars, stellar evolution delays the disk dispersal time as the far-ultraviolet (FUV) luminosity decreases toward the main sequence. In the case of intermediate-mass stars, the FUV luminosity increases significantly over a few million years, driving strong photoevaporation and enhancing disk mass loss during the later stages of disk evolution. This highlights the limitations of assuming a constant FUV luminosity throughout a simulation. Photoevaporation primarily impacts the outer regions of the disk and is the dominant disk dispersal process in the late evolutionary stage. Based on the results of a large set of simulations, we study the evolution of a population of star–disk systems and derive the disk fraction as a function of time. We demonstrate that the inclusion of stellar luminosity evolution can alter the disk fraction by several tens of percent, bringing the simulations into closer agreement with recent observations. We argue that it is important to include the stellar luminosity evolution in simulations of the long-term dispersal of protoplanetary disks. |
| format | Article |
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| institution | Kabale University |
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| language | English |
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| spelling | doaj-art-b2005d7c0ab842119b2a9802549683252025-01-16T13:32:47ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197914610.3847/1538-4357/ad9746The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming RegionsAyano Komaki0https://orcid.org/0000-0002-9995-5223Naoki Yoshida1https://orcid.org/0000-0001-7925-238XDepartment of Physics, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan ; ayano.komaki@phys.s.u-tokyo.ac.jpDepartment of Physics, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan ; ayano.komaki@phys.s.u-tokyo.ac.jp; Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan; Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanWe study the effect of stellar evolution on the dispersal of protoplanetary disks by performing one-dimensional simulations of long-term disk evolution. Our simulations include viscous disk accretion, magnetohydrodynamic winds, and photoevaporation as important disk dispersal processes. We consider a wide range of stellar mass of 0.1–7 M _⊙ and incorporate the luminosity evolution of the central star. For solar-mass stars, stellar evolution delays the disk dispersal time as the far-ultraviolet (FUV) luminosity decreases toward the main sequence. In the case of intermediate-mass stars, the FUV luminosity increases significantly over a few million years, driving strong photoevaporation and enhancing disk mass loss during the later stages of disk evolution. This highlights the limitations of assuming a constant FUV luminosity throughout a simulation. Photoevaporation primarily impacts the outer regions of the disk and is the dominant disk dispersal process in the late evolutionary stage. Based on the results of a large set of simulations, we study the evolution of a population of star–disk systems and derive the disk fraction as a function of time. We demonstrate that the inclusion of stellar luminosity evolution can alter the disk fraction by several tens of percent, bringing the simulations into closer agreement with recent observations. We argue that it is important to include the stellar luminosity evolution in simulations of the long-term dispersal of protoplanetary disks.https://doi.org/10.3847/1538-4357/ad9746Protoplanetary disksStellar evolutionStar forming regionsComputational methods |
| spellingShingle | Ayano Komaki Naoki Yoshida The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions The Astrophysical Journal Protoplanetary disks Stellar evolution Star forming regions Computational methods |
| title | The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions |
| title_full | The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions |
| title_fullStr | The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions |
| title_full_unstemmed | The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions |
| title_short | The Effect of Stellar Evolution on Dispersal of Protoplanetary Disks: Disk Fraction in Star-forming Regions |
| title_sort | effect of stellar evolution on dispersal of protoplanetary disks disk fraction in star forming regions |
| topic | Protoplanetary disks Stellar evolution Star forming regions Computational methods |
| url | https://doi.org/10.3847/1538-4357/ad9746 |
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