Shadows cast on the transition disk of HD 135344B
T. StolkerC. DominikH. AvenhausM. MinJ. de BoerC. GinskiH. M. SchmidÁ. JuhászA. BazzonL. B. F. M. WatersA. GarufiJ.‐C. AugereauM. BenistyA. BoccalettiTh. HenningM. LangloisA. L. MaireF. MénardM. R. MeyerC. PinteSascha P. QuanzC. ThalmannJ.-L. BeuzitM. CarbilletA. CostilleKjetil DohlenM. FeldtD. GislerD. MouilletA. PavlovD. PerretC. PetitJ. PragtS. RochatR. RoelfsemaBernardo SalasnichC. SoenkeF. Wildi
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Context. The protoplanetary disk around the F-type star HD 135344B (SAO 206462) is in a transition stage and shows many intriguing structures both in scattered light and thermal (sub-)millimeter emission which are possibly related to planet formation processes.Keywords:
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We have developed a physically self-consistent model of the disk around the nearby 10 Myr old star TW Hya that matches the observed spectral energy distribution and 7 mm images of the disk. The model requires both significant dust-size evolution and a partially evacuated inner disk region, as predicted by theories of planet formation. The outer disk, which extends to at least 140 AU in radius, is very optically thick at infrared wavelengths and quite massive (~0.06 M☉) for the relatively advanced age of this T Tauri star. This implies long viscous and dust evolution timescales, although dust must have grown to sizes of the order of ~1 cm to explain the submillimeter and millimeter spectral slopes. In contrast, the negligible near-infrared excess emission of this system requires that the disk be optically thin inside ≲4 AU. This inner region cannot be completely evacuated; we need ~0.5 lunar mass of ~1 μm particles remaining to produce the observed 10 μm silicate emission. Our model requires a distinct transition in disk properties at ~4 AU separating the inner and outer disks. The inner edge of the optically thick outer disk must be heated almost frontally by the star to account for the excess flux at mid-infrared wavelengths. We speculate that this truncation of the outer disk may be the signpost of a developing gap due to the effects of a growing protoplanet; the gap is still presumably evolving because material still resides in it, as indicated by the silicate emission, the molecular hydrogen emission, and the continued accretion onto the central star (albeit at a much lower rate than typical of younger T Tauri stars). Thus, TW Hya may become the Rosetta stone for our understanding of the evolution and dissipation of protoplanetary disks.
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The core accretion mechanism for gas giant planet formation requires multiple-Earthmass protoplanets to form in the presence of the disk gas, i.e., prior to the dispersal of the protoplanetary disk. Such protoplanets are subject to rapid orbital migration through their gravitational interactions with the disk. Studies of the interactions of Earth-mass protoplanets with the disk gas generally assume a disk mass low enough that the disk’s self-gravity can be neglected. However, forming Earth-mass cores prior to dissipation of the gaseous disk may require a disk that is massive enough (~ 0.1 solar mass) to be marginally gravitationally unstable. In this case, the self-gravity of the disk must be taken into account when attempting to follow the orbital evolution of growing protoplanets.
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view Abstract Citations (164) References (59) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Gap Formation in Protoplanetary Disks Takeuchi, Taku ; Miyama, Shoken M. ; Lin, D. N. C. Abstract Evolution of a protoplanetary disk under the tidal interaction between the disk and an embedded protoplanet is analyzed with a self-consistent WKB approximation. We assume that the protoplanetary disk is infinitesimally thin and non-self-gravitating and that the protoplanet's orbit is circular. The protoplanet excites density waves at its Lindblad resonances. As they propagate throughout the disk, these waves carry a flux of angular momentum that is eventually deposited into the gas at the locations where the waves are dissipated viscously. Protoplanets with a sufficiently large mass can induce the formation of a gap in the disk. The size of the gap and the structure of the disk are determined by the wave propagation length scale, which is a decreasing function of viscosity. For small effective viscosity, density waves propagate to inner regions near the protostellar surface. Using an α prescription, we find that a protoplanet with a mass of Jupiter can lead to the removal of the inner disk if α ≲ 3 × 10-4 . For larger values of α, the surface density in the disk surrounding the gap is adjusted in a manner such that the rapid orbital evolution of the protoplanet is prevented. We also inferred that α ∼ 1.7 × 10-2 in the disk around the binary T Tauri star GW Ori, based on the gap size derived from the observational data. Publication: The Astrophysical Journal Pub Date: April 1996 DOI: 10.1086/177013 Bibcode: 1996ApJ...460..832T Keywords: ACCRETION; ACCRETION DISKS; STARS: PLANETARY SYSTEMS; STARS: FORMATION full text sources ADS | data products SIMBAD (2)
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Young planets interact with their parent gas disks through tidal torques. An imbalance between inner and outer torques causes bodies of mass $\ga 0.1$ Earth masses to lose angular momentum and migrate inward rapidly relative to the disk; this is known as ``Type I'' migration. However, protoplanets that grow to gas giant mass, O($10^2) M_\oplus$, open a gap in the disk and are subsequently constrained to migrate more slowly, locked into the disk's viscous evolution in what is called "Type II" migration. In a young planetary system, both Type I and Type II bodies likely coexist; if so, differential migration ought to result in close encounters when the former originate on orbits exterior to the latter. We investigate the resulting dynamics, using two different numerical approaches: an N-body code with dissipative forces added to simulate the effect of the gas disk, and a hybrid code which combines an N-body component with a 1-dimensional viscous disk model, treating planet-disk interactions in a more self-consistent manner. In both cases, we find that sub-gap-opening bodies have a high likelihood of being resonantly captured when they encounter a gap-opening body. A giant planet thus tends to act as a barrier in a protoplanetary disk, collecting smaller protoplanets outside of its orbit. Such behavior has two important implications for giant planet formation: First, for captured protoplanets it mitigates the problem of the migration timescale becoming shorter than the growth timescale. Secondly, it suggests one path to forming systems with multiple giant planets: Once the first has formed, it traps/accretes the future solid core of the second in an exterior mean-motion resonance, and so on. The most critical step in giant planet formation may thus be the formation of the very first one.
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Views Icon Views Article contents Figures & tables Video Audio Supplementary Data Peer Review Share Icon Share Twitter Facebook Reddit LinkedIn Tools Icon Tools Reprints and Permissions Cite Icon Cite Search Site Citation Takayuki Muto, Shu‐ichiro Inutsuka; Orbital Evolution of Particles Embedded in a Protoplanetary Disk and the Possibility of Observing Low‐mass Planets in a Protoplanetary/Debris Disk. AIP Conf. Proc. 5 August 2009; 1158 (1): 255–256. https://doi.org/10.1063/1.3215859 Download citation file: Ris (Zotero) Reference Manager EasyBib Bookends Mendeley Papers EndNote RefWorks BibTex toolbar search Search Dropdown Menu toolbar search search input Search input auto suggest filter your search All ContentAIP Publishing PortfolioAIP Conference Proceedings Search Advanced Search |Citation Search
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The regular satellites found around Neptune ($\approx 17~M_{\Earth}$) and Uranus ($\approx 14.5~M_{\Earth}$) suggest that past gaseous circumplanetary disks may have co-existed with solids around sub-Neptune-mass protoplanets ($< 17~M_{\Earth}$). These disks have been shown to be cool, optically thin, quiescent, with low surface density and low viscosity. Numerical studies of the formation are difficult and technically challenging. As an introductory attempt, three-dimensional global simulations are performed to explore the formation of circumplanetary disks around sub-Neptune-mass protoplanets embedded within an isothermal protoplanetary disk at the inviscid limit of the fluid in the absence of self-gravity. Under such conditions, a sub-Neptune-mass protoplanet can reasonably have a rotationally supported circumplanetary disk. The size of the circumplanetary disk is found to be roughly one-tenth of the corresponding Hill radius, which is consistent with the orbital radii of irregular satellites found for Uranus. The protoplanetary gas accretes onto the circumplanetary disk vertically from high altitude and returns to the protoplanetary disk again near the midplane. This implies an open system in which the circumplanetary disk constantly exchanges angular momentum and material with its surrounding prenatal protoplanetary gas.
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The paper proposes a method of solving the problem of restoring the galaxy surface brightness. The real brightness picture is distorted due to interference in the atmosphere and optics. The model of the distortions system is characterized by a Point Spread Function. Implemented numerical algorithm allows to draw conclusions about optimal values of the function parameters for obtaining more accurate values of the observed brightness.
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The gravitational interaction between a protoplanet and an isothermal gaseous disk is investigated through three-dimensional hydrodynamical simulations with the shearing sheet model. The torque exerted on the disk is evaluated and compared with previous estimates by the linear theory. It is found that a protoplanet mainly excites waves without vertical motion. Thus, the motion of the gas in a disk with thickness is similar to that in an infinitesimally thin disk. The angular momentum transfer is also dominated by waves without vertical motion, and the torque has a similar value to that in an infinitesimally thin disk, except for the correction factor 0.43 owing to the vertical averaging of the gravitational potential of the protoplanet. If the mass of the protoplanet is small enough, the torque increases proportionally with the square of the mass, as is predicted by the linear theory. However, for a large protoplanet whose Hill radius is larger than about the disk scale height, a nonlinear effect reduces the torque from the value proportional to the square of the mass. The torque reduction due to the nonlinearity is less significant for a disk with thickness than for an infinitesimally thin disk and is not effective for a small protoplanet with mass less than 10 times the Earth mass at 1 AU. This result suggests that during the formation of terrestrial planets and the cores of giant planets, the torque continues to increase as the protoplanets grow. The reduction in the torque due to the thickness of the disk and the nonlinearity is not large enough to solve the problem that the migration of protoplanets is too fast. Before protoplanets acquire the masses needed to suppress torque by the nonlinearity, they would experience large migration and some protoplanets would fall onto the central star in the lifetime of the gas in the protoplanetary disks.
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view Abstract Citations (800) References (19) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS On the Tidal Interaction between Protoplanets and the Protoplanetary Disk. III. Orbital Migration of Protoplanets Lin, D. N. C. ; Papaloizou, John Abstract The tidal interaction between a protoplanet and a gaseous protoplanetary disk is investigated, and the dynamical evolution of the disk and the orbital migration of the protoplanet in a self-consistent manner is considered. It is shown that the orbital migration of a protoplanet does not suppress the tendency for tidal truncation in the vicinity of its orbit. If the necessary condition for tidal truncation is satisfied, the protoplanet induces a tidal feedback mechanism that regulates the rate of angular momentum transfer between the protoplanet and the disk. Significant orbital migration can only occur on the viscous evolution time scale of the disk. Publication: The Astrophysical Journal Pub Date: October 1986 DOI: 10.1086/164653 Bibcode: 1986ApJ...309..846L Keywords: Planetary Evolution; Protoplanets; Stellar Evolution; Stellar Models; Tides; Angular Momentum; Feedback; Momentum Transfer; Orbit Perturbation; Astrophysics; PLANETS: FORMATION; STARS: FORMATION full text sources ADS | Related Materials (2) Part 1: 1984ApJ...285..818P Part 2: 1986ApJ...307..395L
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The discovery of new protoplanetary disk structures can help reveal the dynamics of the young planetary systems and potentially point to planet formation within the disk. In my dissertation, I present investigations of three stellar/sub-stellar systems; DoAr 28, VHS J125601.92-125723.9 (VHS 1256), and HD 163296. First, I will discuss the first near-IR scattered light detection of the protoplanetary disk around DoAr 28. I modeled both the observed SED and H-band PI imagery of the system and found that our best fit models have a partially depleted inner gap from the dust sublimation radius out to ~8 au. Second, I present and analyze Subaru/IRCS L' and M' images of the nearby M dwarf VHS 1256, which was recently claimed to have a ~11 Mjup companion (VHS 1256 b). I found that the central star is a binary and conclude that VHS 1256 is most likely a very low mass (VLM) hierarchical triple system. Finally, I present Subaru/HiCIAO H-band imagery, Subaru/SCExAO near-IR imagery, and HST/STIS optical imagery of the protoplanetary disk around HD 163296. I demonstrate that the new Subaru/HiCIAO and HST/STIS imagery exhibits disk illumination variability on timescales < 3 months, possibly due to a non-axisymmetric distribution of dust clouds. show that our SCExAO/CHARIS observations fail to recover the previously identified 6-7 Mjup planetary candidate. Additionally, I did not detect the predicted launch of a new HH-knot nor did I detect any of the previously observed HH-knots, suggesting a potential change in the jet of HD 163296.
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