Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 606394.0, MPI für Astronomie / Publikationen_mpia
Chemical evolution of turbulent protoplanetary disks and the solar nebula
Authors:Semenov, D.; Wiebe, D.
Date of Publication (YYYY-MM-DD):2011
Journal Abbrev.:The Astrophysical Journal Supplement Series
Volume:196
Issue / Number:2
Audience:Not Specified
Abstract / Description:We study the influence of transport processes on the chemical evolution of DM Tau-like protoplanetary disks. Turbulent transport of gases and ices is implicitly modeled in full two dimensions (2D), using the mixing-length approximation, along with the time-dependent chemistry. We find that turbulent transport enhances abundances and column densities of many gas-phase species and ices, particularly, complex ones. The influence of turbulent mixing on disk chemistry is more pronounced in the inner, planet-forming disk region where gradients of temperature and high-energy radiation intensities are steeper than in the outer region. The molecules that are unresponsive to transport include, e.g., C2H, C+, CH4, CN, CO, HCN, HNC, H2CO, OH, as well as water and ammonia ice. Their column densities computed with the laminar and 2D mixing model differ by a factor of <~ 2-5. Molecules whose vertical column densities in the laminar and dynamical models differ by up to two orders of magnitude include, e.g., C2H2, some carbon chains, CS, H2CS, H2O, HCO+, HCOOH, HNCO, N2H+, NH3, CO ice, H2CO ice, CH3OH ice, and electrons. Molecules whose column densities are altered by diffusion by more than two orders of magnitude include, e.g., C2S, C3S, C6H6, CO2, O2, SiO, SO, SO2, long carbon chain ices, CH3CHO ice, HCOOH ice, O2 ice, and OCN ice. We indicate several observable or potentially detectable tracers of transport processes in protoplanetary disks and the solar nebula, such as heavy hydrocarbon ices, complex organics, CO2, O2, SO, SO2, C2S, C3S compared to CO and water ice.
Free Keywords:accretion; accretion disks; astrochemistry; molecular processes; protoplanetary disks; stars: individual: DM Tau; turbulence
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2011ApJS..196...25S
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.