arXiv subjects

Yusuke Tsukamoto

Publications and source records attributed to Yusuke Tsukamoto.

40 records · Page 3Linked to original sources

arXiv2012

Formation and Early Evolution of Circumstellar Disks in Turbulent Molecular Cloud Cores

We investigate the formation and evolution of circumstellar disks in turbulent cloud cores until several 104 years after protostar formation using smoothed particle hydrodynamics (SPH) calculations. The formation and evolution process of circumstellar disk in turbulent cloud cores differs substantially from that in rigidly rotating cloud cores. In turbulent cloud cores, a filamentary structure appears before the protostar formation and the protostar forms in the filament. If the turbulence is initially sufficiently strong, the remaining filament twists around the protostar and directly becomes a rotation-supported disk. Upon formation, the disk orientation is generally misaligned with the angular momentum of its host cloud core and it dynamically varies during the main accretion phase, even though the turbulence is weak. This is because the angular momentum of the entire cloud core is mainly determined by the large scale velocity field whose wavelength is comparable to the cloud scale, whereas the angular momentum of the disk is determined by the local velocity field where the protostar forms and these two velocity fields do not correlate with each other. In the case of disk evolution in a binary or multiple stars, the disks are misaligned with each other at least during the main accretion phase, because there is no correlation between the velocity fields around the position where each protostar forms. In addition, each disk is also misaligned with the binary orbital plane. Such misalignment can explain the recent observations of misaligned disks and misaligned protostellar outflows.

astro-ph.SR↗

arXiv2011

Classification of the Circumstellar Disk Evolution During the Main Accretion Phase

We have carried out hydro-dynamical simulations to investigate the formation and evolution of protostar and circumstellar disks from the prestellar cloud. As the initial state, we adopt the molecular cloud core with two non-dimensional parameters representing the thermal and rotational energies. With these parameters, we make 17 models and calculate the cloud evolution ~ 10^4 years after the protostar formation. We find that early evolution of the star-disk system can be qualitatively classified into four modes: the massive disk, early fragmentation, late fragmentation, and protostar dominant modes. In the 'massive disk mode' to which the majority of models belong, the disk mass is greater than the protostellar mass for over 10^4 years and no fragmentation occurs in the circumstellar disk. The collapsing cloud shows fragmentation before the protostar formation in the 'early fragmentation mode'. The circumstellar disk shows fragmentation after the protostar formation in the 'late fragmentation mode', in which the secondary star substantially gains its mass from the circumstellar disk after fragmentation and it has a mass comparable to that of the primary star. The protostellar mass rapidly increases and exceeds the circumstellar disk mass in the 'protostar dominant mode'. This mode appears only when the initial molecular cloud core has a considerably small rotational energy. Comparison of our results with observations indicates that a majority of protostar has a fairly massive disk during the main accretion phase: the circumstellar disk mass is comparable to or more massive than the protostar. It is expected that such a massive disk promotes gas-giant formation by gravitational instability in a subsequent evolution stage.

astro-ph.SR↗

arXiv2011

The self gravity effect on the orbital stability of Twotinos

We investigate how the self gravity changes the orbital stability of Twotinos using N-body simulations in which the gravitational interaction between planetesimals are fully calculated. We show the timescale in which the half of Twotinos becomes unstable, t_{half}, obey the formula, t_{half} = 4 \times 106(Mtot0.1M\oplus)-1(mp7.6 \times 1023g)-1(hi2i1/20.002)(years), if we assume the primordial planetesimals disk have the power low surface mass density, Σ= Σ_0 \times r-2/3. Where Mtot, mp, hi2i1/2 are the total mass of large bodies of Twotinos, the maximum mass of planetesimals, and the inclination dispersion. With this formulae, we conclude the total mass of Twotinos is reduced to the order of 0.01 M\oplus by the self gravity and secular perturbation of the Planets even if there was huge mass such as several order of the earth mass in 1:2 MMR of Neptune at the early age of the solar system. These results will invoke reexamination to many previous works which tried to explain the dynamical evolution of TNOs.

astro-ph.EP↗

arXiv2007

Formation of Protoplanets from Massive Planetesimals in Binary Systems

More than half of stars reside in binary or multiple star systems and many planets have been found in binary systems. From theoretical point of view, however, whether or not the planetary formation proceeds in a binary system is a very complex problem, because secular perturbation from the companion star can easily stir up the eccentricity of the planetesimals and cause high-velocity, destructive collisions between planetesimals. Early stage of planetary formation process in binary systems has been studied by restricted three-body approach with gas drag and it is commonly accepted that accretion of planetesimals can proceed due to orbital phasing by gas drag. However, the gas drag becomes less effective as the planetesimals become massive. Therefore it is still uncertain whether the collision velocity remains small and planetary accretion can proceed, once the planetesimals become massive. We performed {\it N}-body simulations of planetary formation in binary systems starting from massive planetesimals whose size is about 100-500 km. We found that the eccentricity vectors of planetesimals quickly converge to the forced eccentricity due to the coupling of the perturbation of the companion and the mutual interaction of planetesimals if the initial disk model is sufficiently wide in radial distribution. This convergence decreases the collision velocity and as a result accretion can proceed much in the same way as in isolated systems. The basic processes of the planetary formation, such as runaway growth and oligarchic growth and final configuration of the protoplanets are essentially the same in binary systems and single star systems, at least in the late stage where the effect of gas drag is small.

astro-ph↗