[PDF] Top 20 The dynamical structure of HR 8799’s inner debris disk
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The dynamical structure of HR 8799’s inner debris disk
... The HR 8799 system, with its four giant planets and two debris belts, has an architecture closely mirroring that of our Solar system where the inner, warm asteroid belt and outer, cool ... See full document
10
Modelling the inner debris disc of HR 8799
... the HR 8799 planetary system strongly resembles our ...two debris belts, analogues to the Asteroid and Edgeworth-Kuiper ...of dynamical simulations of HR8799’s inner ... See full document
14
Towards a dynamics-based estimate of the extent of HR 8799’s unresolved warm debris belt
... the inner, unresolved debris belt around HR 8799, using UNSW Australia's supercomputing facility, ...hot debris interior to the innermost planet, HR8799 e, for a period of 60 million ... See full document
12
Constraining the presence of giant planets in two belt debris disk systems with VLT/SPHERE direct imaging and dynamical arguments
... circumstellar debris: this is the case for the HR 8799 and HD 95086 systems, and even the solar system where the Asteroid and Kuiper belts enclose the four gas and ice ...a debris disk, ... See full document
29
A circumbinary debris disk in a polluted white dwarf system
... The progenitors of extant white dwarfs are typically A- and F-type stars with masses in the range 1.2 − 3.0 M ⊙ , a stellar population that is not readily probed for inner planetary systems using conventional ... See full document
25
A Resolved Debris Disk around the G2V star HD
... in dynamical timescales. Dynamical friction will induce large eccentricities in smaller bodies, increasing their collision rate and generating broad rings ... See full document
13
A circumbinary debris disk in a polluted white dwarf system
... The progenitors of extant white dwarfs are typically A- and F-type stars with masses in the range 1.2 − 3.0 M ⊙ , a stellar population that is not readily probed for inner planetary systems using conventional ... See full document
25
Disk formation and structure
... We assume that the cloud was in hydrostatic equilibrium for some time before collapse, and we will therefore assume that it rotates as a solid body. Also, we assume that the cloud rotates slowly, so that the centrifugal ... See full document
13
ALMA observations of the narrow HR 4796A debris ring
... the disk is important for the following discussion because this extent gives a direct measure of the range of orbital inclinations of the particles ...the structure is therefore also representative of ... See full document
17
ALMA observations of the narrow HR 4796A debris ring
... The vertical extent of the disc is important for the following discussion because this extent gives a direct measure of the range of orbital inclinations of the particles observed. Because the grains observed by ALMA are ... See full document
16
Inner approximations of the region of attraction for polynomial dynamical systems
... Nevertheless, this approach does not escape the curse of dimensionality – indeed, whereas the number of variables of the LMI relaxations grows polynomially with the re- laxation order, this number grows exponentially ... See full document
6
GW Orionis : inner disk readjustments in a triple system
... Using the above simple models, we find that all the observed SEDs of GW Ori can be naturally explained by the change of the structure of the inner disk. In Fig. 21, we show the best-fit model SEDs ... See full document
22
Colors of inner disk classical Kuiper Belt objects
... the inner-classical KBOs and the cold-classical KBOs, neither our color data nor the dynamical models can resolve this issue at ...the dynamical origin of the inner classical objects, as ... See full document
5
A dynamical systems perspective on the absence of debris associated with the disappearance of flight MH370
... Figure 5a and b shows a similar analysis to that of Fig. 4a and b using HYCOM data 5 at 50 m depth. Mesoscale structures in this data are consistent with those of AVISO. For instance, the large eddy which isolates ... See full document
29
Dynamical structure and evolution of merger remnants
... a dynamical evidence for formation from an early merger since they are found to host predominantly old stellar populations (Carollo et ...two disk galaxies, where one of them is employed on a retrograde ... See full document
117
Detection and Characterization of Extrasolar Planets through Planet-Disk Dynamical Interactions
... a dynamical model of the HL Tau disk, the most detailed protoplanetary disk structure observed by ALMA to this day, without much of complex physics typically required in modeling gas-rich ... See full document
171
Thermo-dynamical measurements for ATLAS Inner Detector (evaporative cooling system)
... to the additional pump, rising refrigerant’s pressure up to 15 bar abs , and then is delivered to the liquid supply pipe line of the blending machine. This line is split in two; internal and external circuits. The ... See full document
213
Disk Storage and Basic File Structure
... the disk. Every read or write operation on the disk affects at least one sector at a ...a disk I/O ...the inner most tracks can hold much fewer bits than the outer ...the disk but, on ... See full document
32
Spatially resolved imaging of the two component η Crv debris disk with Herschel
... the inner belt has to contain substantial amounts of grains at the blow-out size and, quite possibly, even below this ...the inner belt, this difference in dust properties between the two dust belts ... See full document
19
Spatially resolved imaging of the two-component η crv debris disk with Herschel
... the inner belt has to contain substantial amounts of grains at the blow-out size and, quite possibly, even below this ...the inner belt, this difference in dust properties between the two dust belts ... See full document
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