313 research outputs found
Molecular architecture of Gαo and the structural basis for RGS16-mediated deactivation
Heterotrimeric G proteins relay extracellular cues from heptahelical transmembrane receptors to downstream effector molecules. Composed of an α subunit with intrinsic GTPase activity and a βγ heterodimer, the trimeric complex dissociates upon receptor-mediated nucleotide exchange on the α subunit, enabling each component to engage downstream effector targets for either activation or inhibition as dictated in a particular pathway. To mitigate excessive effector engagement and concomitant signal transmission, the Gα subunit's intrinsic activation timer (the rate of GTP hydrolysis) is regulated spatially and temporally by a class of GTPase accelerating proteins (GAPs) known as the regulator of G protein signaling (RGS) family. The array of G protein-coupled receptors, Gα subunits, RGS proteins and downstream effectors in mammalian systems is vast. Understanding the molecular determinants of specificity is critical for a comprehensive mapping of the G protein system. Here, we present the 2.9 Å crystal structure of the enigmatic, neuronal G protein Gαo in the GTP hydrolytic transition state, complexed with RGS16. Comparison with the 1.89 Å structure of apo-RGS16, also presented here, reveals plasticity upon Gαo binding, the determinants for GAP activity, and the structurally unique features of Gαo that likely distinguish it physiologically from other members of the larger Gαi family, affording insight to receptor, GAP and effector specificity
Non-LTE dust nucleation in sub-saturated vapors
We use the kinetic theory of nucleation to explore the properties of dust
nucleation in sub-saturated vapors. Due to radiation losses, the sub-critical
clusters have a smaller temperature compared to their vapor. This alters the
dynamical balance between attachment and detachment of monomers, allowing for
stable nucleation of grains in vapors that are sub-saturated for their
temperature. We find this effect particularly important at low densities and in
the absence of a strong background radiation field. We find new conditions for
stable nucleation in the n-T phase diagram. The nucleation in the non-LTE
regions is likely to be at much slower rate than in the super-saturated vapors.
We evaluate the nucleation rate, warning the reader that it does depend on
poorly substantiated properties of the macro-molecules assumed in the
computation. On the other hand, the conditions for nucleation depend only on
the properties of the large stable grains and are more robust. We finally point
out that this mechanism may be relevant in the early universe as an initial
dust pollution mechanism, since once the interstellar medium is polluted with
dust, mantle growth is likely to be dominant over non-LTE nucleation in the
diffuse medium.Comment: 8 pages, 8 figures, accepted for publication in MNRA
Dust sputtering by Reverse Shocks in Supernova Remnants
We consider sputtering of dust grains, believed to be formed in cooling
supernovae ejecta, under the influence of reverse shocks. In the regime of
self-similar evolution of reverse shocks, we can follow the evolution of ejecta
density and temperature analytically as a function of time in different parts
of the ejecta, and calculate the sputtering rate of graphite and silicate
grains embedded in the ejecta as they encounter the reverse shock. Through
analytic (1D) calculations, we find that a fraction of dust mass (% for silicates and %% for graphites) can be sputtered by
reverse shocks, the fraction varying with the grain size distribution and the
steepness of the density profile of the ejecta mass. It is expected that many
more grains will get sputtered in the region between the forward and reverse
shocks, so that our analytical results provide a lower limit to the destroyed
fraction of dust mass.Comment: 10 pages, 6 figures, uses emulateapj5.sty, accepted in Ap
The Three-Dimensional Structure of Cassiopeia A
We used the Spitzer Space Telescope's Infrared Spectrograph to map nearly the
entire extent of Cassiopeia A between 5-40 micron. Using infrared and Chandra
X-ray Doppler velocity measurements, along with the locations of optical ejecta
beyond the forward shock, we constructed a 3-D model of the remnant. The
structure of Cas A can be characterized into a spherical component, a tilted
thick disk, and multiple ejecta jets/pistons and optical fast-moving knots all
populating the thick disk plane. The Bright Ring in Cas A identifies the
intersection between the thick plane/pistons and a roughly spherical reverse
shock. The ejecta pistons indicate a radial velocity gradient in the explosion.
Some ejecta pistons are bipolar with oppositely-directed flows about the
expansion center while some ejecta pistons show no such symmetry. Some ejecta
pistons appear to maintain the integrity of the nuclear burning layers while
others appear to have punched through the outer layers. The ejecta pistons
indicate a radial velocity gradient in the explosion. In 3-D, the Fe jet in the
southeast occupies a "hole" in the Si-group emission and does not represent
"overturning", as previously thought. Although interaction with the
circumstellar medium affects the detailed appearance of the remnant and may
affect the visibility of the southeast Fe jet, the bulk of the symmetries and
asymmetries in Cas A are intrinsic to the explosion.Comment: Accepted to ApJ. 54 pages, 21 figures. For high resolution figures
and associated mpeg movie and 3D PDF files, see
http://homepages.spa.umn.edu/~tdelaney/pape
Properties of Newly Formed Dust Grains in The Luminous Type IIn Supernova 2010jl
Supernovae (SNe) have been proposed to be the main production sites of dust
grains in the Universe. Our knowledge on their importance to dust production
is, however, limited by observationally poor constraints on the nature and
amount of dust particles produced by individual SNe. In this paper, we present
a spectrum covering optical through near-Infrared (NIR) light of the luminous
Type IIn supernova (SN IIn) 2010jl around one and half years after the
explosion. This unique data set reveals multiple signatures of newly formed
dust particles. The NIR portion of the spectrum provides a rare example where
thermal emission from newly formed hot dust grains is clearly detected. We
determine the main population of the dust species to be carbon grains at a
temperature of ~1,350 - 1,450K at this epoch. The mass of the dust grains is
derived to be ~(7.5 - 8.5) x 10^{-4} Msun. Hydrogen emission lines show
wavelength-dependent absorption, which provides a good estimate on the typical
size of the newly formed dust grains (~0.1 micron, and most likely <~0.01
micron). We attribute the dust grains to have been formed in a dense cooling
shell as a result of a strong SN-circumstellar media (CSM) interaction. The
dust grains occupy ~10% of the emitting volume, suggesting an inhomogeneous,
clumpy structure. The average CSM density is required to be >~3 x 10^{7}
cm^{-3}, corresponding to a mass loss rate of >~0.02 Msun yr^{-1} (for a mass
loss wind velocity of ~100 km s^{-1}). This strongly supports a scenario that
SN 2010jl and probably other luminous SNe IIn are powered by strong
interactions within very dense CSM, perhaps created by Luminous Blue Variable
(LBV)-like eruptions within the last century before the explosion.Comment: 18 pages, 11 figures. Accepted by ApJ on 30 July 2013. The accepted
version was submitted on 8 July 2013, and the original version was submitted
on 3 March 201
Light Element Evolution and Cosmic Ray Energetics
Using cosmic-ray energetics as a discriminator, we investigate evolutionary
models of LiBeB. We employ a Monte Carlo code which incorporates the delayed
mixing into the ISM both of the synthesized Fe, due to its incorporation into
high velocity dust grains, and of the cosmic-ray produced LiBeB, due to the
transport of the cosmic rays. We normalize the LiBeB production to the integral
energy imparted to cosmic rays per supernova. Models in which the cosmic rays
are accelerated mainly out of the average ISM significantly under predict the
measured Be abundance of the early Galaxy, the increase in [O/Fe] with
decreasing [Fe/H] notwithstanding. We suggest that this increase could be due
to the delayed mixing of the Fe. But, if the cosmic-ray metals are accelerated
out of supernova ejecta enriched superbubbles, the measured Be abundances are
consistent with a cosmic-ray acceleration efficiency that is in very good
agreement with the current epoch data. We also find that neither the above
cosmic-ray origin models nor a model employing low energy cosmic rays
originating from the supernovae of only very massive progenitors can account
for the Li data at values of [Fe/H] below 2.Comment: latex 19 pages, 2 tables, 10 eps figures, uses aastex.cls natbib.sty
Submitted to the Astrophysical Journa
Extraordinary Late-Time Infrared Emission of Type IIn Supernovae
Near-Infrared (NIR) observations are presented for five Type IIn supernovae
(SN 1995N, SN 1997ab, SN 1998S, SN 1999Z, and SN 1999el) that exhibit strong
infrared excesses at late times (t >= 100 d). H- and K-band emission from these
objects is dominated by a continuum that rises toward longer wavelengths. The
data are interpreted as thermal emission from dust, probably situated in a
pre-existing circumstellar nebula. The IR luminosities implied by single
temperature blackbody fits are quite large,> 10^(41 - 42) erg s^-1, and the
emission evolves slowly, lasting for years after maximum light. For SN 1995N,
the integrated energy release via IR dust emission was 0.5 -- 1 * 10^50 erg. A
number of dust heating scenarios are considered, the most likely being an
infrared echo poweredby X-ray and UV emissions from the shock interaction with
a dense circumstellar medium.Comment: 14 Pages, 3 Figures, Accecpted for publication in The Astrophysical
Journa
The Peculiar Type Ib Supernova 2006jc: A WCO Wolf-Rayet Star Explosion
We present a theoretical model for Type Ib supernova (SN) 2006jc. We
calculate the evolution of the progenitor star, hydrodynamics and
nucleosynthesis of the SN explosion, and the SN bolometric light curve (LC).
The synthetic bolometric LC is compared with the observed bolometric LC
constructed by integrating the UV, optical, near-infrared (NIR), and
mid-infrared (MIR) fluxes. The progenitor is assumed to be as massive as
on the zero-age main-sequence. The star undergoes extensive mass
loss to reduce its mass down to as small as , thus becoming a WCO
Wolf-Rayet star. The WCO star model has a thick carbon-rich layer, in which
amorphous carbon grains can be formed. This could explain the NIR brightening
and the dust feature seen in the MIR spectrum. We suggest that the progenitor
of SN 2006jc is a WCO Wolf-Rayet star having undergone strong mass loss and
such massive stars are the important sites of dust formation. We derive the
parameters of the explosion model in order to reproduce the bolometric LC of SN
2006jc by the radioactive decays: the ejecta mass , hypernova-like
explosion energy ergs, and ejected Ni mass . We
also calculate the circumstellar interaction and find that a CSM with a flat
density structure is required to reproduce the X-ray LC of SN 2006jc. This
suggests a drastic change of the mass-loss rate and/or the wind velocity that
is consistent with the past luminous blue variable (LBV)-like event.Comment: 12 pages, 11 figures. Accepted for publication in the Astrophysical
Journa
Molecular Hydrogen Emission from Protoplanetary Disks II. Effects of X-ray Irradiation and Dust Evolution
Detailed models for the density and temperature profiles of gas and dust in
protoplanetary disks are constructed by taking into account X-ray and
ultraviolet (UV) irradiation from a central T Tauri star, as well as dust size
growth and settling toward the disk midplane. The spatial and size
distributions of dust grains in the disks are numerically computed by solving
the coagulation equation for settling dust particles. The level populations and
line emission of molecular hydrogen are calculated using the derived physical
structure of the disks. X-ray irradiation is the dominant heating source of the
gas in the inner disk region and in the surface layer, while the far UV heating
dominates otherwise. If the central star has strong X-ray and weak UV
radiation, the H2 level populations are controlled by X-ray pumping, and the
X-ray induced transition lines could be observable. If the UV irradiation is
strong, the level populations are controlled by thermal collisions or UV
pumping, depending on the properties of the dust grains in the disks. As the
dust particles evolve in the disks, the gas temperature at the disk surface
drops because the grain photoelectric heating becomes less efficient, while the
UV radiation fields become stronger due to the decrease of grain opacity. This
makes the H2 level populations change from local thermodynamic equilibrium
(LTE) to non-LTE distributions, which results in changes to the line ratios of
H2 emission. Our results suggest that dust evolution in protoplanetary disks
could be observable through the H2 line ratios. The emission lines are strong
from disks irradiated by strong UV and X-rays and possessing small dust grains;
such disks will be good targets in which to observe H2 emission.Comment: 33 pages, accepted for publication in the Astrophysical Journa
Do Airports green cities? : Von der Airport City zur nachhaltigen Region ; Flughafenstrategien und Regionalentwicklung
Multivariate pattern recognition approaches have become a prominent tool in neuroimaging data analysis. These methods enable the classification of groups of participants (e.g. controls and patients) on the basis of subtly different patterns across the whole brain. This study demonstrates that these methods can be used, in combination with automated morphometric analysis of structural MRI, to determine with great accuracy whether a single subject has been engaged in regular mental training or not. The proposed approach allowed us to identify with 94.87% accuracy (p<0.001) if a given participant is a regular meditator (from a sample of 19 regular meditators and 20 non-meditators). Neuroimaging has been a relevant tool for diagnosing neurological and psychiatric impairments. This study may suggest a novel step forward: the emergence of a new field in brain imaging applications, in which participants could be identified based on their mental experience
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