Planetary system formation through binary star merging

Details Planetary system formation through binary star merging Planetary system formation through binary star merging

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sosyr..41..132s&link_type=abstract

Solar System Research, Volume 41, Issue 2, pp.132-139

Statistics

Computation

96.15.Bc, 97.80.-D

Scientific paper

A scenario is considered for the formation of a planetary system through the merging of a binary star comprised of low-mass (0.5 1 M &sun;) stars in the stage of contracting towards the main sequence. According to our previous computations (Sirotkin and Karetnikov, 2006), under certain conditions, the destruction of the more massive component can result in the formation of a central star, an accretion disk, and an extended arm. The extended arm is fragmented to form clouds of planetary masses (<5M J). The formed disk and clouds rotate in the same direction as the central star. The clouds are in elongated orbits (e > 0.3) lying in the orbital plane of the initial binary system. To test these earlier results, we repeated computations for the same system parameters but with higher accuracy. The new computations confirmed the earlier results and gave new information about the cloud and disk structure.

Affiliated with

Also associated with

No associations

Rating

Planetary system formation through binary star merging does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Planetary system formation through binary star merging, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Planetary system formation through binary star merging will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1361042