382 research outputs found
Viscoelastic Phase Patterning in Artificial Protein Hydrogels
Viscoelastic forces can affect the dynamics of pattern formation during phase separation in polymeric materials. We programmed an artificial protein hydrogel to undergo viscoelastic phase separation above a critical temperature. Highly dynamic phase patterns that coarsened under the influence of viscoelastic stresses spontaneously emerged in these gels. Local oxidative crosslinking promoted by mild photobleaching could be used to initiate phase separation locally, enabling the creation of non-equilibrium patterns that evolved under the influence of surface tension and viscoelastic stresses to yield dynamic structures of controlled size and shape
Recommended from our members
Mechanisms of diffusion in associative polymer networks: evidence for chain hopping
Networks assembled by reversible association of telechelic polymers constitute a common class of soft materials. Various mechanisms of chain migration in associative networks have been proposed; yet there remains little quantitative experimental data to discriminate among them. Proposed mechanisms for chain migration include multichain aggregate diffusion as well as single-chain mechanisms such as “walking” and “hopping”, wherein diffusion is achieved by either partial (“walking”) or complete (“hopping”) disengagement of the associated chain segments. Here, we provide evidence that hopping can dominate the effective diffusion of chains in associative networks due to a strong entropic penalty for bridge formation imposed by local network structure; chains become conformationally restricted upon association with two or more spatially separated binding sites. This restriction decreases the effective binding strength of chains with multiple associative domains, thereby increasing the probability that a chain will hop. For telechelic chains this manifests as binding asymmetry, wherein the first association is effectively stronger than the second. We derive a simple thermodynamic model that predicts the fraction of chains that are free to hop as a function of tunable molecular and network properties. A large set of self-diffusivity measurements on a series of model associative polymers finds good agreement with this model
Mechanisms of diffusion in associative polymer networks: evidence for chain hopping
Networks assembled by reversible association of telechelic polymers constitute a common class of soft materials. Various mechanisms of chain migration in associative networks have been proposed; yet there remains little quantitative experimental data to discriminate among them. Proposed mechanisms for chain migration include multichain aggregate diffusion as well as single-chain mechanisms such as “walking” and “hopping”, wherein diffusion is achieved by either partial (“walking”) or complete (“hopping”) disengagement of the associated chain segments. Here, we provide evidence that hopping can dominate the effective diffusion of chains in associative networks due to a strong entropic penalty for bridge formation imposed by local network structure; chains become conformationally restricted upon association with two or more spatially separated binding sites. This restriction decreases the effective binding strength of chains with multiple associative domains, thereby increasing the probability that a chain will hop. For telechelic chains this manifests as binding asymmetry, wherein the first association is effectively stronger than the second. We derive a simple thermodynamic model that predicts the fraction of chains that are free to hop as a function of tunable molecular and network properties. A large set of self-diffusivity measurements on a series of model associative polymers finds good agreement with this model
Precursors prior to Type IIn supernova explosions are common: precursor rates, properties, and correlations
There is a growing number of supernovae (SNe), mainly of Type IIn, which
present an outburst prior to their presumably final explosion. These precursors
may affect the SN display, and are likely related to some poorly charted
phenomena in the final stages of stellar evolution. Here we present a sample of
16 SNe IIn for which we have Palomar Transient Factory (PTF) observations
obtained prior to the SN explosion. By coadding these images taken prior to the
explosion in time bins, we search for precursor events. We find five Type IIn
SNe that likely have at least one possible precursor event, three of which are
reported here for the first time. For each SN we calculate the control time.
Based on this analysis we find that precursor events among SNe IIn are common:
at the one-sided 99% confidence level, more than 50% of SNe IIn have at least
one pre-explosion outburst that is brighter than absolute magnitude -14, taking
place up to 1/3 yr prior to the SN explosion. The average rate of such
precursor events during the year prior to the SN explosion is likely larger
than one per year, and fainter precursors are possibly even more common. We
also find possible correlations between the integrated luminosity of the
precursor, and the SN total radiated energy, peak luminosity, and rise time.
These correlations are expected if the precursors are mass-ejection events, and
the early-time light curve of these SNe is powered by interaction of the SN
shock and ejecta with optically thick circumstellar material.Comment: 15 pages, 20 figures, submitted to Ap
Swift J2058.4+0516: Discovery of a Possible Second Relativistic Tidal Disruption Flare?
We report the discovery by the Swift hard X-ray monitor of the transient
source Swift J2058.4+0516 (Sw J2058+05). Our multi-wavelength follow-up
campaign uncovered a long-lived (duration >~ months), luminous X-ray (L_X,iso ~
3 x 10^47 erg s^-1) and radio (nu L_nu,iso ~ 10^42 erg s^-1) counterpart. The
associated optical emission, however, from which we measure a redshift of
1.1853, is relatively faint, and this is not due to a large amount of dust
extinction in the host galaxy. Based on numerous similarities with the recently
discovered GRB 110328A / Swift J164449.3+573451 (Sw J1644+57), we suggest that
Sw J2058+05 may be the second member of a new class of relativistic outbursts
resulting from the tidal disruption of a star by a supermassive black hole. If
so, the relative rarity of these sources (compared with the expected rate of
tidal disruptions) implies that either these outflows are extremely narrowly
collimated (theta < 1 degree), or only a small fraction of tidal disruptions
generate relativistic ejecta. Analogous to the case of long-duration gamma-ray
bursts and core-collapse supernovae, we speculate that rapid spin of the black
hole may be a necessary condition to generate the relativistic component.
Alternatively, if powered by gas accretion (i.e., an active galactic nucleus
[AGN]), Sw J2058+05 would seem to represent a new mode of variability in these
sources, as the observed properties appear largely inconsistent with known
classes of AGNs capable of generating relativistic jets (blazars, narrow-line
Seyfert 1 galaxies).Comment: Minor typos correcte
PTF11iqb: Cool supergiant mass loss that bridges the gap between Type IIn and normal supernovae
PTF11iqb was initially classified as a TypeIIn event caught very early after
explosion. It showed narrow Wolf-Rayet (WR) spectral features on day 2, but the
narrow emission weakened quickly and the spectrum morphed to resemble those of
Types II-L and II-P. At late times, Halpha emission exhibited a complex,
multipeaked profile reminiscent of SN1998S. In terms of spectroscopic
evolution, we find that PTF11iqb was a near twin of SN~1998S, although with
weaker interaction with circumstellar material (CSM) at early times, and
stronger CSM interaction at late times. We interpret the spectral changes as
caused by early interaction with asymmetric CSM that is quickly (by day 20)
enveloped by the expanding SN ejecta photosphere, but then revealed again after
the end of the plateau when the photosphere recedes. The light curve can be
matched with a simple model for weak CSM interaction added to the light curve
of a normal SN~II-P. This plateau requires that the progenitor had an extended
H envelope like a red supergiant, consistent with the slow progenitor wind
speed indicated by narrow emission. The cool supergiant progenitor is
significant because PTF11iqb showed WR features in its early spectrum ---
meaning that the presence of such WR features in an early SN spectrum does not
necessarily indicate a WR-like progenitor. [abridged] Overall, PTF11iqb bridges
SNe~IIn with weaker pre-SN mass loss seen in SNe II-L and II-P, implying a
continuum between these types.Comment: 21 pages, 12 figures, submitted to MNRA
Undergraduate medical student perceptions and use of Evidence Based Medicine: A qualitative study
<p>Abstract</p> <p>Background</p> <p>Many medical schools teach the principles of Evidence Based Medicine (EBM) as a subject within their medical curriculum. Few studies have explored the barriers and enablers that students experience when studying medicine and attempting to integrate EBM in their clinical experience. The aim of this study was to identify undergraduate medical student perceptions of EBM, including their current use of its principles as students and perceived future use as clinicians.</p> <p>Methods</p> <p>Third year medical students were recruited via email to participate in focus group discussions. Four focus groups were conducted separately across four hospital sites. All focus groups were conducted by the same facilitator. All discussions were transcribed verbatim, and analysed independently by the two authors according to the principles of thematic analysis.</p> <p>Results</p> <p>Focus group discussions were conducted with 23 third-year medical students, representing three metropolitan and one rural hospital sites. Five key themes emerged from the analysis of the transcripts: (1) Rationale and observed use of EBM in practice, (2) Current use of EBM as students, (3) Perceived use of EBM as future clinicians, (4) Barriers to practicing EBM, and (5) Enablers to facilitate the integration of EBM into clinical practice. Key facilitators for promoting EBM to students include competency in EBM, mentorship and application to clinical disciplines. Barriers to EBM implementation include lack of visible application by senior clinicians and constraints by poor resourcing.</p> <p>Conclusions</p> <p>The principles and application of EBM is perceived by medical students to be important in both their current clinical training and perceived future work as clinicians. Future research is needed to identify how medical students incorporate EBM concepts into their clinical practice as they gain greater clinical exposure and competence.</p
Evidence for an FU Orionis-like Outburst from a Classical T Tauri Star
We present pre- and post-outburst observations of the new FU Orionis-like
young stellar object PTF 10qpf (also known as LkHa 188-G4 and HBC 722). Prior
to this outburst, LkHa 188-G4 was classified as a classical T Tauri star on the
basis of its optical emission-line spectrum superposed on a K8-type
photosphere, and its photometric variability. The mid-infrared spectral index
of LkHa 188-G4 indicates a Class II-type object. LkHa 188-G4 exhibited a steady
rise by ~1 mag over ~11 months starting in Aug. 2009, before a subsequent more
abrupt rise of > 3 mag on a time scale of ~2 months. Observations taken during
the eruption exhibit the defining characteristics of FU Orionis variables: (i)
an increase in brightness by > 4 mag, (ii) a bright optical/near-infrared
reflection nebula appeared, (iii) optical spectra are consistent with a G
supergiant and dominated by absorption lines, the only exception being Halpha
which is characterized by a P Cygni profile, (iv) near-infrared spectra
resemble those of late K--M giants/supergiants with enhanced absorption seen in
the molecular bands of CO and H_2O, and (v) outflow signatures in H and He are
seen in the form of blueshifted absorption profiles. LkHa 188-G4 is the first
member of the FU Orionis-like class with a well-sampled optical to mid-infrared
spectral energy distribution in the pre-outburst phase. The association of the
PTF 10qpf outburst with the previously identified classical T Tauri star LkHa
188-G4 (HBC 722) provides strong evidence that FU Orionis-like eruptions
represent periods of enhanced disk accretion and outflow, likely triggered by
instabilities in the disk. The early identification of PTF 10qpf as an FU
Orionis-like variable will enable detailed photometric and spectroscopic
observations during its post-outburst evolution for comparison with other known
outbursting objects.Comment: 14 pages, 11 figures, ApJ accepte
The Lick AGN Monitoring Project 2011: Dynamical Modeling of the Broad-Line Region
We present models of the H-emitting broad-line region (BLR) in seven
Seyfert 1 galaxies from the Lick AGN (Active Galactic Nucleus) Monitoring
Project 2011 sample, drawing inferences on the BLR structure and dynamics as
well as the mass of the central supermassive black hole. We find that the BLR
is generally a thick disk, viewed close to face-on, with preferential emission
back toward the ionizing source. The dynamics in our sample range from
near-circular elliptical orbits to inflowing or outflowing trajectories. We
measure black hole masses of for PG 1310108, for Mrk 50,
for Mrk 141, for Mrk 279,
for Mrk 1511, for NGC 4593, and
for Zw 229015. We use these black hole mass
measurements along with cross-correlation time lags and line widths to recover
the scale factor used in traditional reverberation mapping measurements.
Combining our results with other studies that use this modeling technique,
bringing our sample size to 16, we calculate a scale factor that can be used
for measuring black hole masses in other reverberation mapping campaigns. When
using the root-mean-square (rms) spectrum and using the line dispersion to
measure the line width, we find . Finally, we search for correlations between and other AGN
and BLR parameters and find marginal evidence that is correlated with
and the BLR inclination angle, but no significant evidence of a
correlation with the AGN luminosity or Eddington ratio.Comment: 26 pages, 14 figures. Accepted for publication in Ap
- …