Radial mixing in protoplanetary accretion disks - I. Stationary disc models with annealing and carbon combustion

被引:117
作者
Gail, HP [1 ]
机构
[1] Univ Heidelberg, Inst Theoret Astrophys, D-69121 Heidelberg, Germany
关键词
accretion disks; molecular processes; solar system : formation;
D O I
10.1051/0004-6361:20011130
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The interplay between radial mixing process in protoplanetary accretion discs with processes leading to destruction or modification of the extinction properties of abundant dust species has significant consequences for the properties of the disk. This paper studies the consequences of annealing amorphous silicate dust at T approximate to 800 K, of combustion of the carbon dust component at about T approximate to 1000 K and of mixing the products into cold outer disc regions out to 10 AU and beyond. A model calculation in the one-zone approximation for stationary Keplerian alpha -disks around a solar-like protostar is combined with a solution of the equations for annealing of silicate dust grains, for carbon dust oxidation, and a solution of the diffusion equations for radial mixing of the dust components in the disc by turbulent flows. It is shown that annealing of amorphous silicate dust reduces the mass extinction coefficient of the disc matter by more than an order of magnitude in the warm disc zone. Radial mixing of the freshly produced crystalline silicate dust into outer disc regions reduces the opacity of the disc material also in cold disc regions where annealing is not possible. Mixing of carbon dust free material from the zone of carbon combustion into outer disc regions also leads to a considerable reduction of the opacity of the disc material. Radial mixing processes then modify the dust composition of the outer disc regions and by means of the dependence of the disk properties (midplane temperature T-c, viscosity nu,...) on the opacity also modify the structure and evolution of a protoplanetary disc. It is shown that turbulent mixing processes in the protoplanetary accretion disc of a Solar System like system during its evolution prior to the onset of the formation of planetary bodies carry material from inner disc regions r<1 AU outwards to at least 10...20 AU. This offers a simple explanation of the findings that a significant fraction of the cometary silicate dust grains are crystallised and that the matrix material of primitive meteorites contains thermally processed crystalline dust material.
引用
收藏
页码:192 / 213
页数:22
相关论文
共 64 条
[31]  
LIDE R, 1995, CRC HDB CHEM PHYSICS
[32]  
Lin D.N.C., 1985, PROTOSTARS PLANETS, VII, P981
[33]   Theory of accretion disks .2. Application to observed systems [J].
Lin, DNC ;
Papaloizou, JCB .
ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, 1996, 34 :703-747
[34]   SIZE DISTRIBUTION OF INTERSTELLAR GRAINS [J].
MATHIS, JS ;
RUMPL, W ;
NORDSIECK, KH .
ASTROPHYSICAL JOURNAL, 1977, 217 (02) :425-433
[35]  
MCCOMB WD, 1990, PHYSICS FLUID TURBUL
[36]  
Mihalas D., 1978, Stellar atmospheres, V2nd
[37]   TRANSPORT OF DUST AND VAPOR AND CHEMICAL FRACTIONATION IN THE EARLY PROTOSOLAR CLOUD [J].
MORFILL, GE ;
VOLK, HJ .
ASTROPHYSICAL JOURNAL, 1984, 287 (01) :371-395
[38]   SOME COSMOCHEMICAL CONSEQUENCES OF A TURBULENT PROTOPLANETARY CLOUD [J].
MORFILL, GE .
ICARUS, 1983, 53 (01) :41-54
[39]  
MORFILL GE, 1985, BIRTH INFANCY STARS, P693
[40]  
MORFILL GE, 1985, PROTOSTARS PLANETS, V2, P493