36,700 research outputs found
Modelling submillimetre spectra of the protostellar infall candidates NGC1333-IRAS2 and Serpens SMM4
We present a radiative transfer model, which is applicable to the study of
submillimetre spectral line observations of protostellar envelopes. The model
uses an exact, non-LTE, spherically symmetric radiative transfer `Stenholm'
method, which numerically solves the radiative transfer problem by the process
of `Lambda-iteration'. We also present submillimetre spectral line data of the
Class 0 protostars NGC1333-IRAS2 and Serpens SMM4. We examine the physical
constraints which can be used to limit the number and range of parameters used
in protostellar envelope models, and identify the turbulent velocity and tracer
molecule abundance as the principle sources of uncertainty in the radiative
transfer modelling. We explore the trends in the appearance of the predicted
line profiles as key parameters in the models are varied.
We find that the separation of the two peaks of a typical infall profile is
dependent not on the evolutionary status of the collapsing protostar, but on
the turbulent velocity dispersion in the envelope. We also find that the line
shapes can be significantly altered by rotation.
Fits are found for the observed line profiles of IRAS2 and SMM4 using
plausible infall model parameters. The density and velocity profiles in our
best fit models are inconsistent with a singular isothermal sphere model. We
find better agreement with a form of collapse which assumes non-static initial
conditions. We also find some evidence that the infall velocities are retarded
from free-fall towards the centre of the cloud, probably by rotation, and that
the envelope of SMM4 is rotationally flattened.Comment: Accepted by MNRA
Theoretical calculation of the electromagnetic response of a radially layered model moon Technical report
Theoretical calculation of electromagnetic response of radially layered moon mode
W49A North - Global or Local or No Collapse?
We attempt to fit observations with 5" resolution of the J=2-1 transition of
CS in the directions of H II regions A, B, and G of W49A North as well as
observations with 20" resolution of the J=2-1, 3-2, 5-4, and 7-6 transitions in
the directions of H II regions A and G by using radiative transfer
calculations. These calculations predict the intensity profiles resulting from
several spherical clouds along the line of sight. We consider three models:
global collapse of a very large (5 pc radius) cloud, localized collapse from
smaller (1 pc) clouds around individual H II regions, and multiple, static
clouds. For all three models we can find combinations of parameters that
reproduce the CS profiles reasonably well provided that the component clouds
have a core-envelope structure with a temperature gradient. Cores with high
temperature and high molecular hydrogen density are needed to match the higher
transitions (e.g. J=7-6) observed towards A and G. The lower temperature, low
density gas needed to create the inverse P-Cygni profile seen in the CS J=2-1
line (with 5" beam) towards H II region G arises from different components in
the 3 models. The infalling envelope of cloud G plus cloud B creates the
absorption in global collapse, cloud B is responsible in local collapse, and a
separate cloud, G', is needed in the case of many static clouds. The exact
nature of the velocity field in the envelopes for the case of local collapse is
not important as long as it is in the range of 1 to 5 km/s for a turbulent
velocity of about 6 km/s. High resolution observations of the J=1-0 and 5-4
transitions of CS and C34S may distinguish between these three models. Modeling
existing observations of HCO+ and C18O does not allow one to distinguish
between the three models but does indicate the existence of a bipolar outflow.Comment: 42 pages, 27 figures, accepted for publication in the ApJS August
2004, v153 issu
Development and evaluation of a prototype global volcano surveillance system utilizing the ERTS-1 satellite data collection system
There are no author-identified significant results in this report
A new method for monitoring global volcanic activity
The ERTS Data Collection System makes it feasible for the first time to monitor the level of activity at widely separated volcanoes and to relay these data rapidly to one central office for analysis. While prediction of specific eruptions is still an evasive goal, early warning of a reawakening of quiescent volcanoes is now a distinct possibility. A prototypical global volcano surveillance system was established under the ERTS program. Instruments were installed in cooperation with local scientists on 15 volcanoes in Alaska, Hawaii, Washington, California, Iceland, Guatemala, El Salvador and Nicaragua. The sensors include 19 seismic event counters that count four different sizes of earthquakes and six biaxial borehole tiltmeters that measure ground tilt with a resolution of 1 microradian. Only seismic and tilt data are collected because these have been shown in the past to indicate most reliably the level of volcano activity at many different volcanoes. Furthermore, these parameters can be measured relatively easily with new instrumentation
Evolution of Migrating Planets Undergoing Gas Accretion
We analyze the orbital and mass evolution of planets that undergo run-away
gas accretion by means of 2D and 3D hydrodynamic simulations. The disk torque
distribution per unit disk mass as a function of radius provides an important
diagnostic for the nature of the disk-planet interactions. We first consider
torque distributions for nonmigrating planets of fixed mass and show that there
is general agreement with the expectations of resonance theory. We then present
results of simulations for mass-gaining, migrating planets. For planets with an
initial mass of 5 Earth masses, which are embedded in disks with standard
parameters and which undergo run-away gas accretion to one Jupiter mass (Mjup),
the torque distributions per unit disk mass are largely unaffected by migration
and accretion for a given planet mass. The migration rates for these planets
are in agreement with the predictions of the standard theory for planet
migration (Type I and Type II migration). The planet mass growth occurs through
gas capture within the planet's Bondi radius at lower planet masses, the Hill
radius at intermediate planet masses, and through reduced accretion at higher
planet masses due to gap formation. During run-away mass growth, a planet
migrates inwards by only about 20% in radius before achieving a mass of ~1
Mjup. For the above models, we find no evidence of fast migration driven by
coorbital torques, known as Type III migration. We do find evidence of Type III
migration for a fixed mass planet of Saturn's mass that is immersed in a cold
and massive disk. In this case the planet migration is assumed to begin before
gap formation completes. The migration is understood through a model in which
the torque is due to an asymmetry in density between trapped gas on the leading
side of the planet and ambient gas on the trailing side of the planet.Comment: 26 pages, 29 figures. To appear in The Astrophysical Journal vol.684
(September 20, 2008 issue
Mapping Observations of DNC and HN^13C in Dark Cloud Cores
We present results of mapping observations of the DNC, HN^13C, and H^13CO^+
lines (J=1-0) toward 4 nearby dark cloud cores, TMC-1, L1512, L1544, and L63,
along with observations of the DNC and HN^13C lines (J=2-1) toward selected
positions. By use of statistical equilibrium calculations based on the LVG
model, the H_2 densities are derived to be (1.4-5.5)*10^5 cm^-3, and the
[DNC]/[HN^13C] ratios are derived to be 1.25-5.44 with a typical uncertainty by
a factor of 2. The observed [DNC]/[HNC] ratios range from 0.02 to 0.09,
assuming the [^12C]/[^13C] ratio of 60. Distributions of DNC and HN^13C are
generally similar to each other, whereas the distribution of H^13CO^+ is more
extended than those of DNC and HN^13C, indicating that they reside in an inner
part of the cores than HCO^+. The [DNC]/[HN^13C] ratio is rather constant
within each core, although a small systematic gradients are observed in TMC-1
and L63. Particularly, no such systematic gradient is found in L1512 and L1544,
where a significant effect of depletion of molecules is reported toward the
central part of the cores. This suggests that the [DNC]/[HNC] ratio would not
be very sensitive to depletion factor, unlike the [DCO^+]/[HCO^+] ratio. On the
other hand, the core to core variation of the [DNC]/[HNC] ratio, which range an
order of magnitude, is more remarkable than the variation within each core.
These results are interpreted qualitatively by a combination of three competing
time-dependent processes; gas-phase deuterium fractionation, depletion of
molecules onto grain surface, and dynamical evolution of a core.Comment: 22 pages, 8 EPS figures, aasLaTex 5.0, accepted to The Astrophysical
Journa
Matrix Pencils and Entanglement Classification
In this paper, we study pure state entanglement in systems of dimension
. Two states are considered equivalent if they can be
reversibly converted from one to the other with a nonzero probability using
only local quantum resources and classical communication (SLOCC). We introduce
a connection between entanglement manipulations in these systems and the
well-studied theory of matrix pencils. All previous attempts to study general
SLOCC equivalence in such systems have relied on somewhat contrived techniques
which fail to reveal the elegant structure of the problem that can be seen from
the matrix pencil approach. Based on this method, we report the first
polynomial-time algorithm for deciding when two states
are SLOCC equivalent. Besides recovering the previously known 26 distinct SLOCC
equivalence classes in systems, we also determine the
hierarchy between these classes
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