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@ARTICLE{Pfalzner:1024258,
      author       = {Pfalzner, Susanne and Dincer, Furkan},
      title        = {{L}ow-mass {S}tars: {T}heir {P}rotoplanetary {D}isk
                      {L}ifetime {D}istribution},
      journal      = {The astrophysical journal / Part 1},
      volume       = {963},
      number       = {2},
      issn         = {0004-637X},
      address      = {London},
      publisher    = {Institute of Physics Publ.},
      reportid     = {FZJ-2024-02065},
      pages        = {122},
      year         = {2024},
      abstract     = {While most protoplanetary disks lose their gas within less
                      than 10 Myr, individual disk lifetimes vary from <1 Myr to
                      ≫20 Myr, with some disks existing for 40 Myr. Mean disk
                      half-lifetimes hide this diversity; only a so-far
                      nonexisting disk lifetime distribution could capture this
                      fact. The benefit of a disk lifetime distribution would be
                      twofold. First, it would provide a stringent test on disk
                      evolution theories. Second, it could function as an input
                      for planet formation models. Here, we derive such a disk
                      lifetime distribution. We heuristically test different
                      standard distribution forms for their ability to account for
                      the observed disk fractions at certain ages. We here
                      concentrate on the distribution for low-mass stars (spectral
                      types M3.7–M6, Ms ≈ 0.1–0.24 M⊙) because disk
                      lifetimes depend on stellar mass. A Weibull-type
                      distribution (k = 1.78, λ = 9.15) describes the
                      observational data if all stars have a disk at a cluster age
                      tc = 0. However, a better match exists for lower initial
                      disk fractions. For f(t=0) = 0.65, a Weibull distribution (k
                      = 2.34, λ = 11.22) and a Gaussian distribution (σ = 9.52,
                      μ = 9.52) fit the data similarly well. All distributions
                      have in common that they are wide, and most disks are
                      dissipated at ages >5 Myr. The next challenge is to
                      quantitatively link the diversity of disk lifetimes to the
                      diversity in planets.},
      cin          = {JSC},
      ddc          = {520},
      cid          = {I:(DE-Juel1)JSC-20090406},
      pnm          = {5111 - Domain-Specific Simulation $\&$ Data Life Cycle Labs
                      (SDLs) and Research Groups (POF4-511) / Big Bang to Big Data
                      - B3D [NRW-Cluster für datenintensive Radioastronomie]
                      (PROFILNRW-2020-038B)},
      pid          = {G:(DE-HGF)POF4-5111 / G:(DE-Juel-1)PROFILNRW-2020-038B},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:001180587600001},
      doi          = {10.3847/1538-4357/ad1bef},
      url          = {https://juser.fz-juelich.de/record/1024258},
}