Triggered planet formation in young stellar clusters

Autor(en)

Ingo Thies, Pavel Kroupa, Christian Theis

Abstrakt

Conventional planet formation models via coagulation of planetesimals require timescales in the range of several 10 or even 100 Myr in the outer regions of a protoplanetary disk. But according to observational data, the lifetime of a protoplanetary disk is limited to about 6 Myr. Therefore the existence of Uranus and Neptune poses a problem. Planet formation via gravitational instability may be a solution for this discrepancy. We present a parameter study of the possibility of gravitationally triggered disk instability. Using a restricted N-body model which allows for a survey of an extended parameter space, we show that a passing dwarf star with a mass between 0.1 and 1 M? can probably induce gravitational instabilities in the pre-planetary solar disk for prograde passages with minimum separations below 80-170 AU. Inclined and retrograde encounters lead to similar results but require slightly closer passages. Such encounter distances are quite likely in young moderately massive star clusters. The induced gravitational instabilities may lead to enhanced planetesimal formation in the outer regions of the protoplanetary disk, and could therefore be relevant for the formation of Uranus and Neptune. Π2005 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

Organisation(en)

Institut für Astrophysik

Externe Organisation(en)

Rheinische Friedrich-Wilhelms-Universität Bonn

Journal

Astronomische Nachrichten

Band

326

Seiten

1048-1052

Anzahl der Seiten

5

ISSN

0004-6337

DOI

https://doi.org/10.1002/asna.200510471

Publikationsdatum

2005

Peer-reviewed

Ja

ÖFOS 2012

1030 Physik, Astronomie, 103003 Astronomie

Schlagwörter

Link zum Portal

https://ucris.univie.ac.at/portal/de/publications/triggered-planet-formation-in-young-stellar-clusters(f260914d-39a3-44cf-9715-0f934e560fbc).html