8,264 research outputs found
WASP-12b as a prolate, inflated and disrupting planet from tidal dissipation
The class of exotic Jupiter-mass planets that orbit very close to their
parent stars were not explicitly expected before their discovery. The recently
found transiting planet WASP-12b has a mass Mp = 1.4(+/-0.1) Jupiter masses
(MJ), a mean orbital distance of only 3.1 stellar radii (meaning it is subject
to intense tidal forces), and a period of 1.1 days. Its radius 1.79(+/- 0.09)
RJ is unexpectedly large and its orbital eccentricity 0.049(+/-0:015) is even
more surprising as such close orbits are in general quickly circularized. Here
we report an analysis of its properties, which reveals that the planet is
losing mass to its host star at a rate ~ 10^-7 MJ yr^-1. The planets surface is
distorted by the stars gravity and the light curve produced by its prolate
shape will differ by about ten per cent from that of a spherical planet. We
conclude that dissipation of the stars tidal perturbation in the planets
convective envelope provides the energy source for its large volume. We predict
up to 10mJy CO band-head (2.292 micron) emission from a tenuous disk around the
host star, made up of tidally stripped planetary gas. It may also contain a
detectable resonant super-Earth, as a hypothetical perturber that continually
stirs up WASP-12b's eccentricity.Comment: Accepted to Nature, 14 pages, 1 figur
Embryo impacts and gas giant mergers II: Diversity of Hot Jupiters' internal structure
We consider the origin of compact, short-period, Jupiter-mass planets. We
propose that their diverse structure is caused by giant impacts of embryos and
super-Earths or mergers with other gas giants during the formation and
evolution of these hot Jupiters. Through a series of numerical simulations, we
show that typical head-on collisions generally lead to total coalescence of
impinging gas giants. Although extremely energetic collisions can disintegrate
the envelope of gas giants, these events seldom occur. During oblique and
moderately energetic collisions, the merger products retain higher fraction of
the colliders' cores than their envelopes. They can also deposit considerable
amount of spin angular momentum to the gas giants and desynchronize their spins
from their orbital mean motion. We find that the oblateness of gas giants can
be used to infer the impact history. Subsequent dissipation of stellar tide
inside the planets' envelope can lead to runaway inflation and potentially a
substantial loss of gas through Roche-lobe overflow. The impact of super-Earths
on parabolic orbits can also enlarge gas giant planets' envelope and elevates
their tidal dissipation rate over 100 Myr time scale. Since giant
impacts occur stochastically with a range of impactor sizes and energies, their
diverse outcomes may account for the dispersion in the mass-radius relationship
of hot Jupiters.Comment: 19 pages, 7 figures, 7 tables. Accepted for publication in MNRA
Three dimensional adaptive method for compressible multi-fluids flows
In this paper, a hexahedral-mesh based solution adaptive algorithm for the simulation of compressible multi-fluid flows is proposed. The data structure, the refinement and coarsening process, and the solution adaptive method are described. The cells with different levels are stored in different lists. This avoids the recursive calculation of solution of mother (non-leaf) cells. Besides, the faces are separated stored into two lists: one for leaf faces and another for non-leaf faces. Thus, high efficiency is obtained due to these features. Numerical results show that there is no oscillation of pressure and velocity across the interface and it is feasible to apply it to solve compressible multi-fluid flows with large density ratio (1000) and strong shock wave interaction with the interface
Acyclic orientations on the Sierpinski gasket
We study the number of acyclic orientations on the generalized
two-dimensional Sierpinski gasket at stage with equal to
two and three, and determine the asymptotic behaviors. We also derive upper
bounds for the asymptotic growth constants for and -dimensional
Sierpinski gasket .Comment: 20 pages, 8 figures and 6 table
Tidal Barrier and the Asymptotic Mass of Proto Gas-Giant Planets
Extrasolar planets found with radial velocity surveys have masses ranging
from several Earth to several Jupiter masses. While mass accretion onto
protoplanetary cores in weak-line T-Tauri disks may eventually be quenched by a
global depletion of gas, such a mechanism is unlikely to have stalled the
growth of some known planetary systems which contain relatively low-mass and
close-in planets along with more massive and longer period companions. Here, we
suggest a potential solution for this conundrum. In general, supersonic infall
of surrounding gas onto a protoplanet is only possible interior to both of its
Bondi and Roche radii. At a critical mass, a protoplanet's Bondi and Roche
radii are equal to the disk thickness. Above this mass, the protoplanets' tidal
perturbation induces the formation of a gap. Although the disk gas may continue
to diffuse into the gap, the azimuthal flux across the protoplanets' Roche lobe
is quenched. Using two different schemes, we present the results of numerical
simulations and analysis to show that the accretion rate increases rapidly with
the ratio of the protoplanet's Roche to Bondi radii or equivalently to the disk
thickness. In regions with low geometric aspect ratios, gas accretion is
quenched with relatively low protoplanetary masses. This effect is important
for determining the gas-giant planets' mass function, the distribution of their
masses within multiple planet systems around solar type stars, and for
suppressing the emergence of gas-giants around low mass stars
Measurement of Lande g factor of 5D5/2 state of BaII with a single trapped ion
We present the first terrestrial measurement of the Lande g factor of the
5D5/2 state of singly ionized barium. Measurements were performed on single
Doppler-cooled 138Ba+ ions in a linear Paul trap. A frequency-stabilized fiber
laser with nominal wavelength 1.762 um was scanned across the 6S1/25D5/2
transition to spectroscopically resolve transitions between Zeeman sublevels of
the ground and excited states. From the relative positions of the four narrow
transitions observed at several different values for the applied magnetic
field, we find a value of 1.2020+/-0.0005 for g of 5D5/2.Comment: 3 figure
- …