Biology
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p11a1573k&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P11A-1573
Biology
[5205] Planetary Sciences: Astrobiology / Formation Of Stars And Planets
Scientific paper
Planetesimal formation in vortices in protoplanetary disks is one of the planetesimal forming scenarios. Vortices are suggested as long-lived, elliptic, coherent anticyclonic ones. Futhermore, vortices trap dust within them. There are some numerical simulations showing that the accumulated dust in vortices may reach sufficient mass to form planetesimals (e.g. Inaba & Barge 2006[1]). However they simulated by only one or a few sizes of dust. Then they do not show the relation, for example, between condensed dust mass and time. We aim to show the relation between accumulation time and dust mass in a vortex in each dust size quantitatively. We investigate the dust motion in a vortex by analytically and obtain the dust mass in a vortex in any dust size and any place vortices are. We refer to Johansen et al. (2004)[2] for gas velocity field inside vortex. We solved the equations of dust motion analytically and obtained dust drifting velocity field toward the center of a vortex and dust surface density distribution in a vortex. Under the assumption that dust flow into vortex is semipermanently, dust surface density distribution in a vortex is independent of not only dust size but also the aspect ratio of vortex ellipse and increases in reverse proportion to the square of the length of the minor-axis of concentric ellipses. And we also obtained the evolution of dust surface density distribution by estimating the dust mass flux flowing into a vortex. Then we obtained the relation between accumulation time and dust mass in a vortex in each dust size quantitatively. In this result, mm-sized dust increases to 16.8 times that of initial density for about one thousand Kepler's time. Sekiya 1998[3] suggested that if dust surface density increases to 16.8 times that of dust density in a MMSN at 1AU, the dust layer can become thin enough to trigger the selfgravitational instability. And also Barranco & Marcus 2005[4] suggested that vortex lifetime is over hundreds of years. Therefore, we conclude that mm-sized or bigger dust surface density increase in a vortex as to be able to form planetesimals. Furthermore, we discuss the effect to planet formation by existing vortices in protoplanetary disk. Furthermore, we evaluate how general is our result by comparing our local analytical result with our global numerical simulation result. This numerical simulation based on Inaba & Barge 2006[1] is using two-phase fluid of gas and dust. And it is simulating vortices formation and dust accumulation in the vortices. For inside a vortex flow, we checked that analytical flow corresponds with numerical flow. However, about the evolution of dust surface density distribution, dust is accumulated in a vortex faster in analytical result than numerical result. We discuss about this difference. [1]Inaba, S. & Barge, P. 2006, ApJ, 649, 415 [2]Johansen, A. et al. 2004, A&A, 417, 361 [3]Sekiya, M., 1998, Icarus 133, 298 [4]Barranco, J. A., & Marcus, P. S. 2005, ApJ, 623, 1157
Inaba Satoshi
Kawamura Eri
Watanabe Shin
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