1,056 research outputs found
A Superwind from Early Post-Red Giant Stars?
We suggest that the gap observed at 20,000 K in the horizontal branches of
several Galactic globular clusters is caused by a small amount of extra mass
loss which occurs when stars start to "peel off" the red giant branch (RGB),
i.e., when their effective temperature starts to increase, even though they may
still be on the RGB. We show that the envelope structure of RGB stars which
start to peel off is similar to that of late asymptotic giant branch stars
known to have a super-wind phase. An analogous super-wind in the RGB peel-off
stars could easily lead to the observed gap in the distribution of the hottest
HB stars.Comment: 9 pages; Accepted by ApJ Letters; Available also at
http://www.astro.puc.cl/~mcatelan
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Coupled climate model simulations of Mediterranean winter cyclones and large-scale flow patterns
The study aims to evaluate the ability of global, coupled climate models to reproduce the synoptic regime of the Mediterranean Basin. The output of simulations of the 9 models included in the IPCC CMIP3 effort is compared to the NCEP-NCAR reanalyzed data for the period 1961–1990. The study examined the spatial distribution of cyclone occurrence, the mean Mediterranean upper- and lower-level troughs, the inter-annual variation and trend in the occurrence of the Mediterranean cyclones, and the main large-scale circulation patterns, represented by rotated EOFs of 500 hPa and sea level pressure. The models reproduce successfully the two maxima in cyclone density in the Mediterranean and their locations, the location of the average upper- and lower-level troughs, the relative inter-annual variation in cyclone occurrences and the structure of the four leading large scale EOFs. The main discrepancy is the models' underestimation of the cyclone density in the Mediterranean, especially in its western part. The models' skill in reproducing the cyclone distribution is found correlated with their spatial resolution, especially in the vertical. The current improvement in model spatial resolution suggests that their ability to reproduce the Mediterranean cyclones would be improved as well
Defining the Termination of the Asymptotic Giant Branch
I suggest a theoretical quantitative definition for the termination of the
asymptotic giant branch (AGB) phase and the beginning of the post-AGB phase. I
suggest that the transition will be taken to occur when the ratio of the
dynamical time scale to the the envelope thermal time scale, Q, reaches its
maximum value. Time average values are used for the different quantities, as
the criterion does not refer to the short time-scale variations occurring on
the AGB and post-AGB, e.g., thermal pulses (helium shell flashes) and magnetic
activity. Along the entire AGB the value of Q increases, even when the star
starts to contract. Only when a rapid contraction starts does the value of Q
start to decrease. This criterion captures the essence of the transition from
the AGB to the post AGB phase, because Q is connected to the stellar effective
temperature, reaching its maximum value at T~4000-6000 K, it is related to the
mass loss properties, and it reaches its maximum value when rapid contraction
starts and envelope mass is very low.Comment: Submitted to ApJ Letter
Detection of a period decrease in NN Ser with ULTRACAM: evidence for strong magnetic braking or an unseen companion?
We present results of high time resolution photometry of the eclipsing
pre-cataclysmic variable NN Ser. We observed 13 primary eclipses of NN Ser
using the high-speed CCD camera ULTRACAM and derived times of mid-eclipse, from
fitting of light curve models, with uncertainties as low as 0.06 s. The
observed rates of period change appear difficult to reconcile with any models
of orbital period change. If the observed period change reflects an angular
momentum loss, the average loss rate is consistent with the loss rates (via
magnetic stellar wind braking) used in standard models of close binary
evolution, which were derived from observations of much more massive cool
stars. Observations of low-mass stars such as NN Ser's secondary predict rates
of ~100 times lower than we observe. We show that magnetic activity-driven
changes in the quadrupole moment of the secondary star (Applegate, 1992) fail
to explain the period change by an order of magnitude on energetic grounds, but
that a light travel time effect caused by the presence of a third body in a
long (~ decades) orbit around the binary could account for the observed changes
in the timings of NN Ser's mid-eclipses. We conclude that we have either
observed a genuine angular momentum loss for NN Ser, in which case our
observations pose serious difficulties for the theory of close binary
evolution, or we have detected a previously unseen low-mass companion to the
binary.Comment: 10 pages, 6 figures. Accepted for publication in MNRA
Why Magnetic Fields Cannot be the Main Agent Shaping Planetary Nebulae
An increasing amount of literature reports the detection of magnetic fields
in asymptotic giant branch (AGB) stars and in central stars of planetary
nebulae (PNs). These detections lead to claims that the magnetic fields are the
main agent shaping the PNs. In this paper, I examine the energy and angular
momentum carried by magnetic fields expelled from AGB stars, as well as other
physical phenomena that accompany the presence of large scale fields, such as
those claimed in the literature. I show that a single star cannot supply the
energy and angular momentum if the magnetic fields have the large coherent
structure required to shape the circumstellar wind. Therefore, the structure of
non-spherical planetary nebulae cannot be attributed to dynamically important
large scale magnetic fields. I conclude that the observed magnetic fields
around evolved stars can be understood by locally enhanced magnetic loops which
can have a secondary role in the shaping of the PN. The primary role, I argue,
rests with the presence of a companion.Comment: PASP, 2006, in press. (This paper was rejected by MNRAS and ApJ; my
criticism of the referee reports are in: Soker, N. astro-ph/0508525.
Shaping bipolar Planetary Nebulae : How mass loss leads to waistline development
Asymptotic Giant Branch (AGB) stars generally have spherically symmetric
envelopes, whereas most post-AGB stars and Planetary Nebulae (PNe) show
axisymmetric circumstellar envelopes. While various mechanisms for axisymmetric
circumstellar structures may explain the shapes of PNe, they do not address how
the shape of the circumstellar shell evolves. Here we address the temporal
changes in the axisymmetry of AGB star envelopes, and in particular the
development of the torus required in the Generalized Interacting Stellar Winds
(GISW) model. Assuming (1) an AGB star rotates with sufficient angular speed at
the start of the AGB phase; and (2) that the rotational angular momentum of the
AGB star is conserved, we demonstrate that some very important observational
features of AGB star axisymmetry evolution can be reproduced. We find that,
compared to the star's increasing luminosity and decreasing effective
temperature, the decreasing mass of the star primarily affects the axisymmetry
of the envelope. When a representative mass loss history is adopted, where most
of the mass is lost near the end of the AGB phase, the envelope's axisymmetry
increases over time, with the strongest increase occurring near the end of the
AGB phase. This may naturally explain why most AGB stars have spherically
symmetric envelopes, while axisymmetry seems common-place in the post-AGB/PNe
phase. The degree of axisymmetry at the end of the AGB phase is found to
increase with increasing main sequence mass, and the onset of axisymmetry
occurs only after the onset of the superwind (SW) phase, in good agreement with
the observations.Comment: 15 pages, 2 figures, accepted by Ap
The Galactic Population of Low- and Intermediate-Mass X-ray Binaries
(abridged) We present the first study that combines binary population
synthesis in the Galactic disk and detailed evolutionary calculations of low-
and intermediate-mass X-ray binaries (L/IMXBs). We show that the formation
probability of IMXBs with initial donor masses of 1.5--4 Msun is typically >~5
times higher than that of standard LMXBs, and suggest that the majority of the
observed systems may have descended from IMXBs. Distributions at the current
epoch of the orbital periods, donor masses, and mass accretion rates have been
computed, as have orbital-period distributions of BMPs. Several significant
discrepancies between the theoretical and observed distributions are discussed.
The orbital-period distribution of observed BMPs strongly favors cases where
the envelope of the neutron-star progenitor is more easily ejected during the
common-envelope phase. However, this leads to a >~100-fold overproduction of
the theoretical number of luminous X-ray sources relative to the total observed
number of LMXBs. X-ray irradiation of the donor star may result in a dramatic
reduction in the X-ray active lifetime of L/IMXBs, thus possibly resolving the
overproduction problem, as well as the long-standing BMP/LMXB birthrate
problem.Comment: 12 pages, emulateapj, submitted to Ap
Computation of protein geometry and its applications: Packing and function prediction
This chapter discusses geometric models of biomolecules and geometric
constructs, including the union of ball model, the weigthed Voronoi diagram,
the weighted Delaunay triangulation, and the alpha shapes. These geometric
constructs enable fast and analytical computaton of shapes of biomoleculres
(including features such as voids and pockets) and metric properties (such as
area and volume). The algorithms of Delaunay triangulation, computation of
voids and pockets, as well volume/area computation are also described. In
addition, applications in packing analysis of protein structures and protein
function prediction are also discussed.Comment: 32 pages, 9 figure
PSR J1740-5340: accretion inhibited by radio-ejection in a binary millisecond pulsar in the Globular Cluster NGC 6397
We present an evolutionary scenario for the spin-up and evolution of binary
millisecond pulsars, according to which the companion of the pulsar PSR J
1740-5340, recently discovered as a binary with orbital period of 32.5 hr in
the Globular Cluster NGC 6397, is presently in a phase of ``radio-ejection''
mass loss from the system. At present, Roche lobe overflow due to the nuclear
evolution of the pulsar companion and to systemic angular momentum losses by
magnetic braking is still going on, but accretion is inhibited by the momentum
exerted by the radiation of the pulsar on the matter at the inner Lagrangian
point. The presence of this matter around the system is consistent with the
long lasting irregular radio eclipses seen in the system. Roche lobe
deformation of the mass losing component is also necessary to be compatible
with the optical light curve. The "radio-ejection" phase had been recently
postulated by us to deal with the problem of the lack of submillisecond pulsars
(Burderi et al. 2001, ApJ, 560, L71).Comment: Accepted for publication in The Astrophysical Journa
Enteroendocrine cells express functional Toll-like receptors
Intestinal epithelial cells (IECs) provide a physical and immunological barrier against enteric microbial flora. Toll-like receptors (TLRs), through interactions with conserved microbial patterns, activate inflammatory gene expression in cells of the innate immune system. Previous studies of the expression and function of TLRs in IECs have reported varying results. Therefore, TLR expression was characterized in human and murine intestinal sections, and TLR function was tested in an IEC line. TLR1, TLR2, and TLR4 are coexpressed on a subpopulation of human and murine IECs that reside predominantly in the intestinal crypt and belong to the enteroendocrine lineage. An enteroendocrine cell (EEC) line demonstrated a similar expression pattern of TLRs as primary cells. The murine EEC line STC-1 was activated with specific TLR ligands: LPS or synthetic bacterial lipoprotein. In STC-1 cells stimulated with bacterial ligands, NF-κB and MAPK activation was demonstrated. Furthermore, the expression of TNF and macrophage inhibitory protein-2 were induced. Additionally, bacterial ligands induced the expression of the anti-inflammatory gene transforming growth factor-β. LPS triggered a calcium flux in STC-1 cells, resulting in a rapid increase in CCK secretion. Finally, conditioned media from STC-1 cells inhibited the production of nitric oxide and IL-12 p40 by activated macrophages. In conclusion, human and murine IECs that express TLRs belong to the enteroendocrine lineage. Using a murine EEC model, a broad range of functional effects of TLR activation was demonstrated. This study suggests a potential role for EECs in innate immune responses
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