2,251 research outputs found
Warm Molecular Layers in Protoplanetary Disks
We have investigated molecular distributions in protoplanetary disks,
adopting a disk model with a temperature gradient in the vertical direction.
The model produces sufficiently high abundances of gaseous CO and HCO+ to
account for line observations of T Tauri stars using a sticking probability of
unity and without assuming any non-thermal desorption. In regions of radius R >
10 AU, with which we are concerned, the temperature increases with increasing
height from the midplane. In a warm intermediate layer, there are significant
amounts of gaseous molecules owing to thermal desorption and efficient
shielding of ultraviolet radiation by the flared disk. The column densities of
HCN, CN, CS, H2CO, HNC and HCO+ obtained from our model are in good agreement
with the observations of DM Tau, but are smaller than those of LkCa15.
Molecular line profiles from our disk models are calculated using a
2-dimensional non-local-thermal-equilibrium (NLTE) molecular-line radiative
transfer code for a direct comparison with observations. Deuterated species are
included in our chemical model. The molecular D/H ratios in the model are in
reasonable agreement with those observed in protoplanetary disks.Comment: 11 pages, Latex (aa.cls), to be published in Astronomy and
Astrophysic
Effects of accretion flow on the chemical structure in the inner regions of protoplanetary disks
We have studied the dependence of the profiles of molecular abundances and
line emission on the accretion flow in the hot (\ga 100K) inner region of
protoplanetary disks. The gas-phase reactions initiated by evaporation of the
ice mantle on dust grains are calculated along the accretion flow. We focus on
methanol, a molecule that is formed predominantly through the evaporation of
warm ice mantles, to show how the abundance profile and line emission depend on
the accretion flow. Our results show that some evaporated molecules keep high
abundances only when the accretion velocity is large enough, and that methanol
could be useful as a diagnostic of the accretion flow by means of ALMA
observations at the disk radius of \la 10AU.Comment: 6 pages, 5 figures, Accepted for publication in A&
Modeling Molecular-Line Emission from Circumstellar Disks
Molecular lines hold valuable information on the physical and chemical
composition of disks around young stars, the likely progenitors of planetary
systems. This invited contribution discusses techniques to calculate the
molecular emission (and absorption) line spectrum based on models for the
physical and chemical structure of protoplanetary disks. Four examples of
recent research illutrate these techniques in practice: matching resolved
molecular-line emission from the disk around LkCa15 with theoertical models for
the chemistry; evaluating the two-dimensional transfer of ultraviolet radiation
into the disk, and the effect on the HCN/CN ratio; far-infrared CO line
emission from a superheated disk surface layer; and inward motions in the disk
around L1489 IRS.Comment: 6 pages, no figures. To appear in "The Dense Interstellar Medium in
Galaxies", Procs. Fourth Cologne-Bonn-Zermatt-Symposiu
Cyclotron Resonance Study of the Two-Dimensional Electron Layers and Double-Layers in Tilted Magnetic Fields
The far-infrared absorption in two-dimensional electron layers subject to
magnetic field of general orientation was studied theoretically. The Kubo
formula is employed to derive diagonal components of the magneto-conductivity
tensor of two-dimensional electron single-layers and double-layers. The
parabolic quantum well is used to model a simple single-layer system. Both
single-layer and double-layer systems can be realized in a pair of
tunnel-coupled, strictly two-dimensional quantum wells. Obtained results are
compared to experimental data.Comment: 4 pages, 6 figures, elsart/PHYEAUTH macros; presented on the EP2DS-15
Conference in Nara, Japan. To be published in Physica
Observation of the Fano-Kondo Anti-Resonance in a Quantum Wire with a Side-Coupled Quantum Dot
We have observed the Fano-Kondo anti-resonance in a quantum wire with a
side-coupled quantum dot. In a weak coupling regime, dips due to the Fano
effect appeared. As the coupling strength increased, conductance in the regions
between the dips decreased alternately. From the temperature dependence and the
response to the magnetic field, we conclude that the conductance reduction is
due to the Fano-Kondo anti-resonance. At a Kondo valley with the Fano parameter
, the phase shift is locked to against the gate voltage
when the system is close to the unitary limit in agreement with theoretical
predictions by Gerland {\it et al.} [Phys. Rev. Lett. {\bf 84}, 3710 (2000)].Comment: 4 pages, 4 figure
Direct evaporative cooling of 41K into a Bose-Einstein condensate
We have investigated the collisional properties of 41K atoms at ultracold
temperature. To show the possibility to use 41K as a coolant, a Bose-Einstein
condensate of 41K atoms in the stretched state (F=2, m_F=2) was created for the
first time by direct evaporation in a magnetic trap. An upper bound of three
body loss coefficient for atoms in the condensate was determined to be 4(2)
10^{-29} cm -6 s-1. A Feshbach resonance in the F=1, m_F=-1 state was observed
at 51.42(5) G, which is in good agreement with theoretical prediction.Comment: 4 pages, 4 figure
Line Emission from Gas in Optically Thick Dust Disks around Young Stars
We present self-consistent models of gas in optically-thick dusty disks and
calculate its thermal, density and chemical structure. The models focus on an
accurate treatment of the upper layers where line emission originates, and at
radii AU. We present results of disks around stars where we have varied dust properties, X-ray luminosities and
UV luminosities. We separately treat gas and dust thermal balance, and
calculate line luminosities at infrared and sub-millimeter wavelengths from all
transitions originating in the predominantly neutral gas that lies below the
ionized surface of the disk. We find that the [ArII] 7m, [NeII]
12.8m, [FeI] 24m, [SI] 25m, [FeII] 26m, [SiII] 35 m,
[OI] 63m and pure rotational lines of H, HO and CO can be quite
strong and are good indicators of the presence and distribution of gas in
disks. We apply our models to the disk around the nearby young star, TW Hya,
and find good agreement between our model calculations and observations. We
also predict strong emission lines from the TW Hya disk that are likely to be
detected by future facilities. A comparison of CO observations with our models
suggests that the gas disk around TW Hya may be truncated to AU,
compared to its dust disk of 174 AU. We speculate that photoevaporation due to
the strong stellar FUV field from TW Hya is responsible for the gas disk
truncation.Comment: Accepted to Astrophysical Journa
Resolving the chemistry in the disk of TW Hydrae I. Deuterated species
We present Submillimeter Array (SMA) observations of several deuterated
species in the disk around the classical T Tauri star TW Hydrae at arcsecond
scales, including detections of the DCN J=3-2 and DCO+ J=3-2 lines, and upper
limits to the HDO 3(1,2)-2(2,1), ortho-H2D+ 1(1,0)-1(1,1) and para-D2H+
1(1,0)-1(0,1) transitions. We also present observations of the HCN J=3-2, HCO+
J=3-2 and H13CO+ J=4-3 lines for comparison with their deuterated
isotopologues. We constrain the radial and vertical distributions of various
species in the disk by fitting the data using a model where the molecular
emission from an irradiated accretion disk is sampled with a 2D Monte Carlo
radiative transfer code. We find that the distribution of DCO+ differs markedly
from that of HCO+. The D/H ratios inferred change by at least one order of
magnitude (0.01 to 0.1) for radii 70 AU and there is a rapid falloff
of the abundance of DCO+ at radii larger than 90 AU. Using a simple analytical
chemical model, we constrain the degree of ionization, x(e-)=n(e-)/n(H2), to be
~10^-7 in the disk layer(s) where these molecules are present. Provided the
distribution of DCN follows that of HCN, the ratio of DCN to HCN is determined
to be 1.7\pm0.5 \times 10^-2; however, this ratio is very sensitive to the
poorly constrained vertical distribution of HCN. The resolved radial
distribution of DCO+ indicates that {\it in situ} deuterium fractionation
remains active within the TW Hydrae disk and must be considered in the
molecular evolution of circumstellar accretion disks.Comment: 12 pages, 12 figures, accepted to Ap
Narrow-line magneto-optical trap for erbium
We report on the experimental realization of a robust and efficient
magneto-optical trap for erbium atoms, based on a narrow cooling transition at
583nm. We observe up to atoms at a temperature of about
. This simple scheme provides better starting conditions for direct
loading of dipole traps as compared to approaches based on the strong cooling
transition alone, or on a combination of a strong and a narrow kHz transition.
Our results on Er point to a general, simple and efficient approach to laser
cool samples of other lanthanide atoms (Ho, Dy, and Tm) for the production of
quantum-degenerate samples
- …