786 research outputs found
Warm gas in the rotating disk of the Red Rectangle: accurate models of molecular line emission
We aim to study the excitation conditions of the molecular gas in the
rotating disk of the Red Rectangle, the only post-Asymptotic-Giant-Branch
object in which the existence of an equatorial rotating disk has been
demonstrated. For this purpose, we developed a complex numerical code that
accurately treats radiative transfer in 2-D, adapted to the study of molecular
lines from rotating disks.
We present far-infrared Herschel/HIFI observations of the 12CO and 13CO
J=6-5, J=10-9, and J=16-15 transitions in the Red Rectangle. We also present
our code in detail and discuss the accuracy of its predictions, from comparison
with well-tested codes. Theoretical line profiles are compared with the
empirical data to deduce the physical conditions in the disk by means of model
fitting.
We conclude that our code is very efficient and produces reliable results.
The comparison of the theoretical predictions with our observations reveals
that the temperature of the Red Rectangle disk is typically ~ 100-150 K, about
twice as high as previously deduced from mm-wave observations of lower-J lines.
We discuss the relevance of these new temperature estimates for understanding
the thermodynamics and dynamics of this prototype object, as well as for
interpreting observations of other rarely studied post-AGB disks. Despite our
sophisticated treatment of the line formation, our model cannot explain the
relatively strong line-wing emission for intermediate-J transitions. We argue
that a model including a rotating disk only cannot reproduce these data and
suggest that there is an additional extended (probably bipolar) structure
expanding at about 7--15 km/s.Comment: 18 pages, 21 figure
The molecular envelope of CRL 618: A new model based on Herschel/HIFI observations
We study the physical properties and molecular excitation of the different
warm gas components found in the protoplanetary nebula CRL 618. We revise our
previous Herschel/HIFI observations, which consist of several 12CO and 13CO
lines in the far-infrared/sub-mm band. These data have been re-analyzed in
detail by improving calibration, the signal-to-noise-ratio, and baseline
substraction. We identify the contributions of the different nebular components
to the line profiles. We have used a spatio-kinematical model to better
constrain the temperature, density, and kinematics of the molecular components
probed by the improved CO observations. The 12CO and 13CO J=16-15, J=10-9, and
J=6-5 transitions are detected in this source. The line profiles present a
composite structure showing spectacular wings in some cases, which become
dominant as the energy level increases. Our analysis of the high-energy CO
emission with the already known low-energy J=2-1 and J=1-0 lines confirms that
the high-velocity component, or fast bipolar outflow, is hotter than previously
estimated with a typical temperature of ~300 K. This component may then be an
example of a very recent acceleration of the gas by shocks that has not yet
cooled down. We also find that the dense central core is characterized by a
very low expansion velocity, ~5 km/s, and a strong velocity gradient. We
conclude that this component is very likely to be the unaltered circumstellar
layers that are lost in the last AGB phase, where the ejection velocity is
particularly low. The physical properties of the other two nebular components,
the diffuse halo and the double empty shell, more or less agrees with the
estimations derived in previous models.Comment: Accepted for publication in Astronomy & Astrophysics. 8 pages, 3
figure
Water vapor and silicon monoxide maser observations in the protoplanetary nebula OH 231.8+4
OH 231.8+4.2 is a well studied preplanetary nebula (pPN) around a binary
stellar system that shows a remarkable bipolar outflow. To study the structure
and kinematics of the inner 10-80 AU nebular regions we performed
high-resolution observations of the HO 6--5 and SiO
=2, =1--0 maser emissions with the Very Long Baseline Array. The absolute
position of both emission distributions were recovered using the phase
referencing technique, and accurately registered in HST optical images. HO
maser clumps are found to be distributed in two areas of 20 mas in size
spatially displaced by 60 milli-arcseconds along an axis oriented nearly
north-south. SiO masers are tentatively found to be placed between the two
HO maser emitting regions, probably indicating the position of the Mira
component of the system. The SiO maser emission traces an inner equatorial
component with a diameter of 12 AU, probably a disk rotating around the M-type
star. Outwards, we detect in the HO data a pair of polar caps, separated by
80 AU. We believe that the inner regions of the nebula probably have been
altered by the presence of the companion, leading to an equator-to-pole density
contrast that may explain the lack of HO masers and strong SiO maser
emission in the denser, equatorial regions.Comment: 5 pages, 1 figure, A&A accepte
Detection of Keplerian dynamics in a disk around the post-AGB star AC Her
So far, only one rotating disk has been clearly identified and studied in AGB
or post-AGB objects (in the Red Rectangle), by means of observations with high
spectral and spatial resolution. However, disks are thought to play a key role
in the late stellar evolution and are suspected to surround many evolved stars.
We aim to extend our knowledge on these structures.
We present interferometric observations of CO J=2-1 emission from the nebula
surrounding the post-AGB star AC Her, a source belonging to a class of objects
that share properties with the Red Rectangle and show hints of Keplerian disks.
We clearly detect the Keplerian dynamics of a second disk orbiting an evolved
star. Its main properties (size, temperature, central mass) are derived from
direct interpretation of the data and model fitting. With this we confirm that
there are disks orbiting the stars of this relatively wide class of post-AGB
objectsComment: 4 pages, 3 figure
Interferometric observations of SiO thermal emission in the inner wind of M-type AGB stars IK Tauri and IRC+10011
Context. AGB stars go through a process of strong mass-loss that involves
pulsations of the atmosphere, which extends to a region where the conditions
are adequate for dust grains to form. Radiation pressure acts on these grains
which, coupled to the gas, drive a massive outflow. The details of this process
are not clear, including which molecules are involved in the condensation of
dust grains.
Aims. To study the role of the SiO molecule in the process of dust formation
and mass-loss in M-type AGB stars.
Methods. Using the IRAM NOEMA interferometer we observed the SiO and
SiO , emission from the inner circumstellar envelope of the
evolved stars IK Tau and IRC+10011. We computed azimuthally averaged emission
profiles to compare the observations to models using a molecular excitation and
ray-tracing code for SiO thermal emission.
Results. We observed circular symmetry in the emission distribution. We also
found that the source diameter varies only marginally with radial velocity,
which is not the expected behavior for envelopes expanding at an almost
constant velocity. The adopted density, velocity, and abundance laws, together
with the mass-loss rate, which best fit the observations, give us information
on the chemical behavior of the SiO molecule and its role in the dust formation
process.
Conclusions. The results indicate that there is a strong coupling between the
depletion of gas phase SiO and gas acceleration in the inner envelope. This
could be explained by the condensation of SiO into dust grains
Jet Power in Pre-Planetary Nebulae: Observations vs. Theory
High velocity jets are among the most prominent features of a wide class of
planetary nebulae, but their origins are not understood. Several different
types of physical model have been suggested to power the jets, but there is no
consensus or preferred scenario. We compare current theoretical ideas on jet
formation with observations, using the best studied pre-planetary nebulae in
millimeter CO, where the dynamical properties are best defined. In addition to
the mass, velocity, momentum, and energy of the jets, the mass and energetics
of the equatorial mass-loss that typically accompanies jet formation prove to
be important diagnostics. Our integrated approach provides estimates for some
key physical quantities - such as the binding energy of the envelope when the
jets are launched - and allows testing of model features using correlations
between parameters. Even with a relatively small sample of well-observed
objects, we find that some specific scenarios for powering jets can be ruled
out or rendered implausible, and others are promising at a quantitative level.Comment: 4 pages, 1 figure, to appear in "Planetary Nebulae: an Eye to the
Future", IAU Symposium 283, eds. A Manchado, L. Stanghellini, D. Schoenberne
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