5 research outputs found
Discs in misaligned binary systems
We perform SPH simulations to study precession and changes in alignment
between the circumprimary disc and the binary orbit in misaligned binary
systems. We find that the precession process can be described by the rigid-disc
approximation, where the disc is considered as a rigid body interacting with
the binary companion only gravitationally. Precession also causes change in
alignment between the rotational axis of the disc and the spin axis of the
primary star. This type of alignment is of great important for explaining the
origin of spin-orbit misaligned planetary systems. However, we find that the
rigid-disc approximation fails to describe changes in alignment between the
disc and the binary orbit. This is because the alignment process is a
consequence of interactions that involve the fluidity of the disc, such as the
tidal interaction and the encounter interaction. Furthermore, simulation
results show that there are not only alignment processes, which bring the
components towards alignment, but also anti-alignment processes, which tend to
misalign the components. The alignment process dominates in systems with
misalignment angle near 90 degrees, while the anti-alignment process dominates
in systems with the misalignment angle near 0 or 180 degrees. This means that
highly misaligned systems will become more aligned but slightly misaligned
systems will become more misaligned.Comment: 15 pages, 16 figures, 1 table, accepted for publication in MNRA
Collisions in young triple systems
We perform N-body simulations of young triple systems consisting of two low-mass companions orbiting around a significantly more massive primary. We find that, when the orbits of the companions are coplanar and not too widely separated, the chance of a collision between the two companions can be as high as 20 per cent. Collisions between one of the companions (always the less massive) and the primary can also occur in systems with unequal-mass companions. The chance of collisions is a few per cent in systems with more realistic initial conditions, such as with slightly non-coplanar orbits and unequal-mass companions. If the companions start widely separated then collision are very rare except in some cases when the total mass of the companions is large. We suggest that collisions between members of young multiple systems may explain some unusual young multiple systems such as apparently non-coeval companions
The Dynamics of Discs and Stars in Multiple Systems
EThOS - Electronic Theses Online ServiceGBUnited Kingdo
On Encounter Rates in Star Clusters
Close encounters between stars in star-forming regions are important as they can perturb or destroy protoplanetary disks, young planetary systems, and multiple-star systems. We simulate simple, virialized, equal-mass N -body star clusters and find that both the rate and the total number of encounters between stars vary by factors of several in statistically identical clusters due to the stochastic/chaotic details of the orbits and stellar dynamics. Encounters tend to “saturate” rapidly in the core of a cluster, with stars there each having many encounters, while more distant stars have none. However, we find that the fraction of stars that has had at least one encounter within a particular distance grows in the same way (scaling with the crossing time and half-mass radius) in all clusters, and we present a new (empirical) way of estimating the fraction of stars that has had at least one encounter at a particular distance