121 research outputs found
On the Cooling of the Neutron Star in Cassiopeia A
We demonstrate that the high-quality cooling data observed for the young
neutron star in the supernova remnant Cassiopeia A over the past 10 years--as
well as all other reliably known temperature data of neutron stars--can be
comfortably explained within the "nuclear medium cooling" scenario. The cooling
rates of this scenario account for medium-modified one-pion exchange in dense
matter and polarization effects in the pair-breaking formations of superfluid
neutrons and protons. Crucial for the successful description of the observed
data is a substantial reduction of the thermal conductivity, resulting from a
suppression of both the electron and nucleon contributions to it by medium
effects. We also find that possibly in as little as about ten years of
continued observation, the data may tell whether or not fast cooling processes
are active in this neutron star.Comment: 4 pages, 3 figure
Thermal Evolution of Neutron Stars in 2 Dimensions
There are many factors that contribute to the breaking of the spherical
symmetry of a neutron star. Most notably is rotation, magnetic fields, and/or
accretion of matter from companion stars. All these phenomena influence the
macroscopic structures of neutron stars, but also impact their microscopic
compositions. The purpose of this paper is to investigate the cooling of
rotationally deformed, two-dimensional (2D) neutron stars in the framework of
general relativity theory, with the ultimate goal of better understand the
impact of 2D effects on the thermal evolution of such objects. The equations
that govern the thermal evolution of rotating neutron stars are presented in
this paper. The cooling of neutron stars with different frequencies is computed
self-consistently by combining a fully general relativistic 2D rotation code
with a general relativistic 2D cooling code. We show that rotation can
significantly influence the thermal evolution of rotating neutron stars. Among
the major new aspects are the appearances of hot spots on the poles, and an
increase of the thermal coupling times between the core and the crust of
rotating neutron stars. We show that this increase is independent of the
microscopic properties of the stellar core, but depends only on the frequency
of the star.Comment: 8 pages, 6 figures, revised versio
Timing evolution of accreting strange stars
It has been suggested that the QPO phenomenon in LMXB's could be explained
when the central compact object is a strange star. In this work we investigate
within a standard model for disk accretion whether the observed clustering of
spin frequencies in a narrow band is in accordance with this hypothesis. We
show that frequency clustering occurs for accreting strange stars when typical
values of the parameters of magnetic field initial strength and decay time,
accretion rate are chosen. In contrast to hybrid star accretion no mass
clustering effect is found.Comment: 10 pages, 3 figures, version accepted for publication in New
Astronom
Time- and compartment-resolved proteome profiling of the extracellular niche in lung injury and repair
The extracellular matrix (ECM) is a key regulator of tissue morphogenesis and repair. However, its composition and architecture are not well characterized. Here, we monitor remodeling of the extracellular niche in tissue repair in the bleomycin-induced lung injury mouse model. Mass spectrometry quantified 8,366 proteins from total tissue and bronchoalveolar lavage fluid (BALF) over the course of 8 weeks, surveying tissue composition from the onset of inflammation and fibrosis to its full recovery. Combined analysis ofproteome, secretome, and transcriptome highlighted post-transcriptional events during tissue fibrogenesis and defined the composition of airway epithelial lining fluid. To comprehensively characterize the ECM, we developed a quantitative detergent solubility profiling (QDSP) method, which identified Emilin-2 and collagen-XXVIII as novel constituents of the provisional repair matrix. QDSP revealed which secreted proteins interact with the ECM, and showed drastically altered association of morphogens to the insoluble matrix upon injury. Thus, our proteomic systems biology study assigns proteins to tissue compartments and uncovers their dynamic regulation upon lung injury and repair, potentially contributing to the development of anti-fibrotic strategies
How to identify a Strange Star
Contrary to young neutron stars, young strange stars are not subject to the
r-mode instability which slows rapidly rotating, hot neutron stars to rotation
periods near 10 ms via gravitational wave emission. Young millisecond pulsars
are therefore likely to be strange stars rather than neutron stars, or at least
to contain significant quantities of quark matter in the interior.Comment: 4 pages, 1 figur
Intrinsic and extrinsic conduction contributions at nominally neutral domain walls in hexagonal manganites
Conductive and electrostatic atomic force microscopy (cAFM and EFM) are used
to investigate the electric conduction at nominally neutral domain walls in
hexagonal manganites. The EFM measurements reveal a propensity of mobile charge
carriers to accumulate at the nominally neutral domain walls in ErMnO3, which
is corroborated by cAFM scans showing locally enhanced d.c. conductance. Our
findings are explained based on established segregation enthalpy profiles for
oxygen vacancies and interstitials, providing a microscopic model for previous,
seemingly disconnected observations ranging from insulating to conducting
domain wall behavior. In addition, we observe variations in conductance between
different nominally neutral walls that we attribute to deviations from the
ideal charge-neutral structure within the bulk, leading to a superposition of
extrinsic and intrinsic contributions. Our study clarifies the complex
transport properties at nominally neutral domain walls in hexagonal manganites
and establishes new possibilities for tuning their electronic response based on
oxidation conditions, opening the door for domain-wall based sensor technology.Comment: 5 pages, 3 figure
Cooling of Neutron Stars: Two Types of Triplet Neutron Pairing
We consider cooling of neutron stars (NSs) with superfluid cores composed of
neutrons, protons, and electrons (assuming singlet-state pairing of protons,
and triplet-state pairing of neutrons). We mainly focus on (nonstandard)
triplet-state pairing of neutrons with the projection of the total
angular momentum of Cooper pairs onto quantization axis. The specific feature
of this pairing is that it leads to a power-law (nonexponential) reduction of
the emissivity of the main neutrino processes by neutron superfluidity. For a
wide range of neutron critical temperatures , the cooling of NSs with
the superfluidity is either the same as the cooling with the superfluidity, considered in the majority of papers, or much faster. The
cooling of NSs with density dependent critical temperatures and
can be imitated by the cooling of the NSs with some effective
critical temperatures and constant over NS cores. The
hypothesis of strong neutron superfluidity with is inconsistent
with current observations of thermal emission from NSs, but the hypothesis of
weak neutron superfluidity of any type does not contradict to observations.Comment: 10 pages, 6 figure
S-wave Pairing of Hyperons in Dense Matter
In this work we calculate the gap energies of hyperons in
neutron star matter. The calculation is based on a solution of the BCS gap
equation for an effective G-matrix parameterization of the
interaction with a nuclear matter background, presented recently by Lanskoy and
Yamamoto. We find that a gap energy of a few tenths of MeV is expected for
Fermi momenta up to about 1.3 fm. Implications for neutron
star matter are examined, and suggest the existence of a
superfluid between the threshold baryon density for formation and the
baryon density where the fraction reaches .Comment: 16 pages, Revtex, 9 figures, 33 reference
Possibility of \Lambda\Lambda pairing and its dependence on background density in relativistic Hartree-Bogoliubov model
We calculate a \Lambda\Lambda pairing gap in binary mixed matter of nucleons
and \Lambda hyperons within the relativistic Hartree-Bogoliubov model. Lambda
hyperons to be paired up are immersed in background nucleons in a normal state.
The gap is calculated with a one-boson-exchange interaction obtained from a
relativistic Lagrangian. It is found that at background density
\rho_{N}=2.5\rho_{0} the \Lambda\Lambda pairing gap is very small, and that
denser background makes it rapidly suppressed. This result suggests a
mechanism, specific to mixed matter dealt with relativistic models, of its
dependence on the nucleon density. An effect of weaker \Lambda\Lambda
attraction on the gap is also examined in connection with revised information
of the \Lambda\Lambda interaction.Comment: 8 pages, 6 figures, REVTeX 4; substantially rewritten, emphasis is
put on the LL pairing in pure neutron matte
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