1,737 research outputs found
Predictions for the First Parker Solar Probe Encounter
We examine Alfv\'en Wave Solar atmosphere Model (AWSoM) predictions of the
first Parker Solar Probe (PSP) encounter. We focus on the 12-day closest
approach centered on the 1st perihelion. AWSoM (van der Holst et al., 2014)
allows us to interpret the PSP data in the context of coronal heating via
Alfv\'en wave turbulence. The coronal heating and acceleration is addressed via
outward-propagating low-frequency Alfv\'en waves that are partially reflected
by Alfv\'en speed gradients. The nonlinear interaction of these
counter-propagating waves results in a turbulent energy cascade. To apportion
the wave dissipation to the electron and anisotropic proton temperatures, we
employ the results of the theories of linear wave damping and nonlinear
stochastic heating as described by Chandran et al. (2011). We find that during
the first encounter, PSP was in close proximity to the heliospheric current
sheet (HCS) and in the slow wind. PSP crossed the HCS two times, namely at
2018/11/03 UT 01:02 and 2018/11/08 UT 19:09 with perihelion occuring on the
south of side of the HCS. We predict the plasma state along the PSP trajectory,
which shows a dominant proton parallel temperature causing the plasma to be
firehose unstable.Comment: 16 pages, 5 figures; accepted for publication in the Astrophysical
Journal Letter
Rotating Neutron Stars in a Chiral SU(3) Model
We study the properties of rotating neutron stars within a generalized chiral
SU(3)-flavor model. The influence of the rotation on the inner structure and
the hyperon matter content of the star is discussed. We calculate the Kepler
frequency and moments of inertia of the neutron star sequences. An estimate for
the braking index of the associated pulsars is given.Comment: 14 pages, 9 figure
Quark Matter in Neutron Stars: An apercu
The existence of deconfined quark matter in the superdense interior of
neutron stars is a key question that has drawn considerable attention over the
past few decades. Quark matter can comprise an arbitrary fraction of the star,
from 0 for a pure neutron star to 1 for a pure quark star, depending on the
equation of state of matter at high density. From an astrophysical viewpoint,
these two extreme cases are generally expected to manifest different
observational signatures. An intermediate fraction implies a hybrid star, where
the interior consists of mixed or homogeneous phases of quark and nuclear
matter, depending on surface and Coulomb energy costs, as well as other finite
size and screening effects. In this brief review article, we discuss what we
can deduce about quark matter in neutron stars in light of recent exciting
developments in neutron star observations. We state the theoretical ideas
underlying the equation of state of dense quark matter, including color
superconducting quark matter. We also highlight recent advances stemming from
re-examination of an old paradigm for the surface structure of quark stars and
discuss possible evolutionary scenarios from neutron stars to quark stars, with
emphasis on astrophysical observations.Comment: 15 pages, 1 figure. Invited review for Modern Physics Letters
Gravitational wave detection using pulsars: status of the Parkes Pulsar Timing Array project
The first direct detection of gravitational waves may be made through
observations of pulsars. The principal aim of pulsar timing array projects
being carried out worldwide is to detect ultra-low frequency gravitational
waves (f ~ 10^-9 to 10^-8 Hz). Such waves are expected to be caused by
coalescing supermassive binary black holes in the cores of merged galaxies. It
is also possible that a detectable signal could have been produced in the
inflationary era or by cosmic strings. In this paper we review the current
status of the Parkes Pulsar Timing Array project (the only such project in the
Southern hemisphere) and compare the pulsar timing technique with other forms
of gravitational-wave detection such as ground- and space-based interferometer
systems.Comment: Accepted for publication in PAS
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