Stellar-mass-dependent disk structure in coeval planet-forming disks

László Szucs, Dániel Apai, Ilaria Pascucci, Cornelis P. Dullemond

Research output: Contribution to journalArticlepeer-review

27 Scopus citations


Previous studies suggest that the planet-forming disks around very low mass stars/brown dwarfs may be flatter than those around more massive stars, in contrast to model predictions of larger scale heights for gas-disks around lower-mass stars. We conducted a statistically robust study to determine whether there is evidence for stellar-massdependent disk structure in planet-forming disks. We find a statistically significant difference in the Spitzer/IRAC color distributions of disks around very low mass and low mass stars all belonging to the same star-forming region, the Chamaeleon I star-forming region. We show that self-consistently calculated flared disk models cannot fit the median spectral energy distributions (SEDs) of the two groups. These SEDs can only be explained by flatter disk models, consistent with the effect of dust settling in disks. We find that, relative to the disk structure predicted for flared disks, the required reduction in disk scale height is anti-correlated with the stellar mass; i.e., disks around lower-mass stars are flatter. Our results show that the initial and boundary conditions of planet formation are stellar-mass-dependent, an important finding that must be considered in planet formation models.

Original languageEnglish (US)
Pages (from-to)1668-1673
Number of pages6
JournalAstrophysical Journal
Issue number2
StatePublished - Sep 10 2010


  • Brown dwarfs
  • Infrared: stars
  • Planets and satellites: formation
  • Protoplanetary disks
  • Stars: low-mass

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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