20,656 research outputs found
Disc wind models for FU Ori objects
We present disc wind models aimed at reproducing the main features of the
strong Na I resonance line P-Cygni profiles in the rapidly-accreting pre-main
sequence FU Ori objects. We conducted Monte Carlo radiative transfer
simulations for a standard magnetocentrifugally driven wind (MHD) model and our
own "Genwind" models, which allows for a more flexible wind parameterisation.
We find that the fiducial MHD wind and similar Genwind models, which have flows
emerging outward from the inner disc edge, and thus have polar cavities with no
absorbing gas, cannot reproduce the deep, wide Na I absorption lines in FU Ori
objects viewed at low inclination. We find that it is necessary to include an
"inner wind" to fill this polar cavity to reproduce observations. In addition,
our models assuming pure scattering source functions in the Sobolev
approximation at intermediate viewing angles () do not yield sufficiently deep line profiles. Assuming complete
absorption yields better agreement with observations, but simple estimates
strongly suggest that pure scattering should be a much better approximation.
The discrepancy may indicate that the Sobolev approximation is not applicable,
possibly due to turbulence or non-monotonic velocity fields; there is some
observational evidence for the latter. Our results provide guidance for future
attempts to constrain FU Ori wind properties using full MHD wind simulations,
by pointing to the importance of the boundary conditions necessary to give rise
to an inner wind, and by suggesting that the winds must be turbulent to produce
sufficiently deep line profiles.Comment: 12 pages, 17 figures, accepted for publication in MNRA
A Luminous Companion to SGR 1806-20
We have obtained infrared spectra of the star suggested to be the counterpart
of the soft gamma-ray repeater (SGR) 1806-20. We found strong emission lines
similar to those seen in the spectra of the rare Luminous Blue Variables and
B[e] stars. A He I absorption line is also seen, from which we infer a spectral
type O9--B2. This classification, in combination with the minimum distance of
\simgt6 kpc inferred from its extinction, makes the star one of the most
luminous in the Galaxy. We infer that it is a companion to SGR 1806-20, and
suggest that the presence of a companion is somehow related to the SGR
phenomenon.Comment: 5 pages, AASTEX text+table and 2 PostScript figures (needs LaTeX
style files aaspptwo.sty, epsf.sty and rotate.sty). In case of problems,
contact [email protected]. Postscript file of complete article available
on request. (Replaced because first version had one wrong reference in it
Multiprotein DNA looping
DNA looping plays a fundamental role in a wide variety of biological
processes, providing the backbone for long range interactions on DNA. Here we
develop the first model for DNA looping by an arbitrarily large number of
proteins and solve it analytically in the case of identical binding. We uncover
a switch-like transition between looped and unlooped phases and identify the
key parameters that control this transition. Our results establish the basis
for the quantitative understanding of fundamental cellular processes like DNA
recombination, gene silencing, and telomere maintenance.Comment: 11 pages, 4 figure
The reverberation signatures of rotating disc winds in active galactic nuclei
The broad emission lines (BELs) in active galactic nuclei (AGN) respond to
ionizing continuum variations. The time and velocity dependence of their
response depends on the structure of the broad-line region: its geometry,
kinematics and ionization state. Here, we predict the reverberation signatures
of BELs formed in rotating accretion disc winds. We use a Monte Carlo radiative
transfer and ionization code to predict velocity-delay maps for representative
high- (C) and low-ionization (H) emission lines in both high- and
moderate-luminosity AGN. Self-shielding, multiple scattering and the ionization
structure of the outflows are all self-consistently taken into account, while
small-scale structure in the outflow is modelled in the micro-clumping
approximation. Our main findings are: (1) The velocity-delay maps of
smooth/micro-clumped outflows often contain significant negative responses.
(2)~The reverberation signatures of disc wind models tend to be rotation
dominated and can even resemble the classic "red-leads-blue" inflow signature.
(3) Traditional "blue-leads-red" outflow signatures can usually only be
observed in the long-delay limit. (4) Our models predict lag-luminosity
relationships similar to those inferred from observations, but systematically
underpredict the observed centroid delays. (5) The ratio between "virial
product" and black hole mass predicted by our models depends on viewing angle.
Our results imply that considerable care needs to be taken in interpreting data
obtained by observational reverberation mapping campaigns. In particular, basic
signatures such as "red-leads-blue", "blue-leads-red" and "blue and red vary
jointly" are not always reliable indicators of inflow, outflow or rotation.
This may help to explain the perplexing diversity of such signatures seen in
observational campaigns to date.Comment: 15 pages, 17 figures, 2 tables. Accepted by MNRAS 20/7/201
The Impact of Accretion Disk Winds on the Optical Spectra of Cataclysmic Variables
Many high-state non-magnetic cataclysmic variables (CVs) exhibit blue-shifted
absorption or P-Cygni profiles associated with ultraviolet (UV) resonance
lines. These features imply the existence of powerful accretion disk winds in
CVs. Here, we use our Monte Carlo ionization and radiative transfer code to
investigate whether disk wind models that produce realistic UV line profiles
are also likely to generate observationally significant recombination line and
continuum emission in the optical waveband. We also test whether outflows may
be responsible for the single-peaked emission line profiles often seen in
high-state CVs and for the weakness of the Balmer absorption edge (relative to
simple models of optically thick accretion disks). We find that a standard disk
wind model that is successful in reproducing the UV spectra of CVs also leaves
a noticeable imprint on the optical spectrum, particularly for systems viewed
at high inclination. The strongest optical wind-formed recombination lines are
H and He II . We demonstrate that a higher-density outflow
model produces all the expected H and He lines and produces a recombination
continuum that can fill in the Balmer jump at high inclinations. This model
displays reasonable verisimilitude with the optical spectrum of RW Trianguli.
No single-peaked emission is seen, although we observe a narrowing of the
double-peaked emission lines from the base of the wind. Finally, we show that
even denser models can produce a single-peaked H line. On the basis of
our results, we suggest that winds can modify, and perhaps even dominate, the
line and continuum emission from CVs.Comment: 15 pages, 13 figures. Accepted to MNRA
A distinct sortase SrtB anchors and processes a streptococcal adhesin AbpA with a novel structural property.
Surface display of proteins by sortases in Gram-positive bacteria is crucial for bacterial fitness and virulence. We found a unique gene locus encoding an amylase-binding adhesin AbpA and a sortase B in oral streptococci. AbpA possesses a new distinct C-terminal cell wall sorting signal. We demonstrated that this C-terminal motif is required for anchoring AbpA to cell wall. In vitro and in vivo studies revealed that SrtB has dual functions, anchoring AbpA to the cell wall and processing AbpA into a ladder profile. Solution structure of AbpA determined by NMR reveals a novel structure comprising a small globular α/β domain and an extended coiled-coil heliacal domain. Structural and biochemical studies identified key residues that are crucial for amylase binding. Taken together, our studies document a unique sortase/adhesion substrate system in streptococci adapted to the oral environment rich in salivary amylase
Cross-linguistic influence in Cantonese-English bilingual children: the case of right-dislocation
Poster PresentationThe paper investigates the conditions on and directionality of cross-linguistic influence in bilingual acquisition by looking at the development of right-dislocation in Cantonese-English bilingual children. Hulk and Müller (2000) hypothesize two conditions on cross-linguistic influence in bilingual acquisition: (1) the structure involves the interface of two modules of grammar and (2) the structure in which cross-linguistic influence occurs is one where two languages overlap. If the hypothesis is correct, then one might expect cross-linguistic influence to occur in the bilingual acquisition of right-dislocation (RD) constructions, as RD is a phenomenon at the interface of syntax and pragmatics, and shows …published_or_final_versio
Multi-level study of C3H2: The first interstellar hydrocarbon ring
Cyclic species in the interstellar medium have been searched for almost since the first detection of interstellar polyatomic molecules. Eleven different C3H2 rotational transitions were detected; 9 of which were studied in TMC-1, a nearby dark dust cloud, are shown. The 1 sub 10 yields 1 sub 01 and 2 sub 20 yields 2 sub 11 transitions were observed with the 43 m NRAO telescope, while the remaining transitions were detected with the 14 m antenna of the Five College Radio Observatory (FCRAO). The lines detected in TMC-1 have energies above the ground state ranging from 0.9 to 17.1 K and consist of both ortho and para species. Limited maps were made along the ridge for several of the transitions. The HC3N J = 2 yields 1 transition were mapped simultaneously with the C3H2 1 sub 10 yields 1 sub 01 line and therefore can compare the distribution of this ring with a carbon chain in TMC-1. C3H2 is distributed along a narrow ridge with a SE - NW extension which is slightly more extended than the HC2N J = 2 yields 1. Gaussian fits gives a FWHP extension of 8'5 for C3H2 while HC3N has a FWHP of 7'. The data show variations of the two velocity components along the ridge as a function of transition. Most of the transitions show a peak at the position of strongest HC3N emission while the 2 sub 21 yields 2 sub 10 transition shows a peak at the NH3 position
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