214,304 research outputs found
Dense molecular clumps in the envelope of the yellow hypergiant IRC+10420
The circumstellar envelope of the hypergiant star IRC+10420 has been traced
as far out in SiO J=2-1 as in CO J = 1-0 and CO J = 2-1, in dramatic contrast
with the centrally condensed (thermal) SiO- but extended CO-emitting envelopes
of giant and supergiant stars. Here, we present an observation of the
circumstellar envelope in SiO J=1-0 that, when combined with the previous
observation in {\sioii}, provide more stringent constraints on the density of
the SiO-emitting gas than hitherto possible. The emission in SiO peaks at a
radius of 2\arcsec\ whereas that in SiO J=2-1 emission peaks at a smaller
radius of 1\arcsec, giving rise to their ring-like appearances. The ratio
in brightness temperature between SiO J=1-0 and SiO J=2-1 decreases from a
value well above unity at the innermost measurable radius to about unity at
radius of 2\arcsec, beyond which this ratio remains approximately
constant. Dividing the envelope into three zones as in models for the CO J =
1-0 and CO J = 2-1 emission, we show that the density of the SiO-emitting gas
is comparable with that of the CO-emitting gas in the inner zone, but at least
an order of magnitude higher by comparison in both the middle and outer zones.
The SiO-emitting gas therefore originates from dense clumps, likely associated
with the dust clumps seen in scattered optical light, surrounded by more
diffuse CO-emitting interclump gas. We suggest that SiO molecules are released
from dust grains due to shock interactions between the dense SiO-emitting
clumps and the diffuse CO-emitting interclump gas.Comment: Accepted for publication in Ap
Simultaneous VLBI Astrometry of H2O and SiO Masers toward the Semiregular Variable R Crateris
We obtained, for the first time, astrometrically registered maps of the 22.2
GHz H2O and 42.8, 43.1, and 86.2 GHz SiO maser emission toward the semiregular
b-type variable (SRb) R Crateris, at three epochs (2015 May 21, and 2016
January 7 and 26) using the Korean Very-long-baseline Interferometry Network.
The SiO masers show a ring-like spatial structure, while the H2O maser shows a
very asymmetric one-side outflow structure, which is located at the southern
part of the ring-like SiO maser feature. We also found that the 86.2 GHz SiO
maser spots are distributed in an inner region, compared to those of the 43.1
GHz SiO maser, which is different from all previously known distributions of
the 86.2 GHz SiO masers in variable stars. The different distribution of the
86.2 GHz SiO maser seems to be related to the complex dynamics caused by the
overtone pulsation mode of the SRb R Crateris. Furthermore, we estimated the
position of the central star based on the ring fitting of the SiO masers, which
is essential for interpreting the morphology and kinematics of a circumstellar
envelope. The estimated stellar coordinate corresponds well to the position
measured by Gaia
SiO maser observations of a wide dust-temperature range sample
We present the results of SiO line observations of a sample of known SiO
maser sources covering a wide dust-temperature range. The aim of the present
research is to investigate the causes of the correlation between infrared
colors and SiO maser intensity ratios among different transition lines. We
observed in total 75 SiO maser sources with the Nobeyama 45m telescope
quasi-simultaneously in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines.
We also observed the sample in the 29SiO J=1-0 v=0 and J=2-1 v=0, and 30SiO
J=1-0 v=0 lines, and the H2O 6(1,6)-5(2,3) line. As reported in previous
papers, we confirmed that the intensity ratios of the SiO J=1-0 v=2 to v=1
lines clearly correlate with infrared colors. In addition, we found possible
correlation between infrared colors and the intensity ratios of the SiO J=1-0
v=3 to v=1&2 lines.Comment: 5 pages, 2 figures, iaus.cls, to appear in IAU Symp. 242 proceedings
(Astrophysical masers and their environments
Correlation between Infrared Colors and Intensity Ratios of SiO Maser Lines
We present the results of SiO millimeter-line observations of a sample of
known SiO maser sources covering a wide dust-temperature range. A cold part of
the sample was selected from the SiO maser sources found in our recent SiO
maser survey of cold dusty objects. The aim of the present research is to
investigate the causes of the correlation between infrared colors and SiO maser
intensity ratios among different transition lines. In particular, the
correlation between infrared colors and SiO maser intensity ratio among the
J=1-0 v=1, 2, and 3 lines are mainly concerned in this paper. We observed in
total 75 SiO maser sources with the Nobeyama 45m telescope quasi-simultaneously
in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines. We also observed the
sample in the 29SiO J=1-0 v=0 and J=2-1 v=0, and 30SiO J=1-0 v=0 lines, and the
H2O 6(1,6)-5(2,3) line. As reported in previous papers, we confirmed that the
intensity ratios of the SiO J=1-0 v=2 to v=1 lines clearly correlate with
infrared colors. In addition, we found possible correlation between infrared
colors and the intensity ratios of the SiO J=1-0 v=3 to v=1&2 lines. Two
overlap lines of H2O (i.e., 11(6,6) nu_2=1 -> 12(7,5) nu_2=0 and 5(0,5) nu_2=2
-> 6(3,4) nu_2=1) might explain these correlation if these overlap lines become
stronger with increase of infrared colors, although the phenomena also might be
explained by more fundamental ways if we take into account the variation of
opacity from object to object.Comment: 49 pages, 7 figures, 3 tables, accepted for publication in ApJ. Full
resolution version available at
http://www.asiaa.sinica.edu.tw/~junichi/paper
Circumstellar molecular composition of the oxygen-rich AGB star IK~Tau: II. In-depth non-LTE chemical abundance analysis
Aims: Little information exists on the circumstellar molecular abundance
stratifications of many molecules. The aim is to study the circumstellar
chemical abundance pattern of 11 molecules and isotopologs (CO,
CO, SiS, SiO, SiO, SiO, HCN, CN, CS, SO, SO) in
the oxygen-rich evolved star IK~Tau. Methods: We have performed an in-depth
analysis of a large number of molecular emission lines excited in the
circumstellar envelope around IK~Tau. The analysis is done based on a non-local
thermodynamic equilibrium (non-LTE) radiative transfer analysis, which
calculates the temperature and velocity structure in a self-consistent way. The
chemical abundance pattern is coupled to theoretical outer wind model
predictions including photodestruction and cosmic ray ionization. Not only the
integrated line intensities, but also the line shapes, are used as diagnostic
tool to study the envelope structure. Results: The deduced wind acceleration is
much slower than predicted from classical theories. SiO and SiS are depleted in
the envelope, possibly due to the adsorption onto dust grains. For HCN and CS a
clear difference with respect to inner wind non-equilibrium predictions is
found, either indicating uncertainties in the inner wind theoretical modeling
or the possibility that HCN and CS (or the radical CN) participate in the dust
formation. The low signal-to-noise profiles of SO and CN prohibit an accurate
abundance determination; the modeling of high-excitation SO lines is
cumbersome, possibly related to line misidentifications or problems with the
collisional rates. The SiO isotopic ratios (SiO/SiO and
SiO/SiO) point toward an enhancement in SiO compared to
results of classical stellar evolution codes. Predictions for HO lines in
the spectral range of the Herschel/HIFI mission are performed. [abbreviated]Comment: 24 pagees, accepted for publication in Astronomy & Astrophysic
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