1,460 research outputs found
M-Dwarf Fast Rotators and the Detection of Relatively Young Multiple M-Star Systems
We have searched the Kepler light curves of ~3900 M-star targets for evidence
of periodicities that indicate, by means of the effects of starspots, rapid
stellar rotation. Several analysis techniques, including Fourier transforms,
inspection of folded light curves, 'sonograms', and phase tracking of
individual modulation cycles, were applied in order to distinguish the
periodicities due to rapid rotation from those due to stellar pulsations,
eclipsing binaries, or transiting planets. We find 178 Kepler M-star targets
with rotation periods, P_rot, of < 2 days, and 110 with P_rot < 1 day. Some 30
of the 178 systems exhibit two or more independent short periods within the
same Kepler photometric aperture, while several have three or more short
periods. Adaptive optics imaging and modeling of the Kepler pixel response
function for a subset of our sample support the conclusion that the targets
with multiple periods are highly likely to be relatively young physical binary,
triple, and even quadruple M star systems. We explore in detail the one object
with four incommensurate periods all less than 1.2 days, and show that two of
the periods arise from one of a close pair of stars, while the other two arise
from the second star, which itself is probably a visual binary. If most of
these M-star systems with multiple periods turn out to be bound M stars, this
could prove a valuable way of discovering young hierarchical M-star systems;
the same approach may also be applicable to G and K stars. The ~5% occurrence
rate of rapid rotation among the ~3900 M star targets is consistent with spin
evolution models that include an initial contraction phase followed by magnetic
braking, wherein a typical M star can spend several hundred Myr before spinning
down to periods longer than 2 days.Comment: 17 pages, 12 figures, 2 tables; accepted for publication in The
Astrophysical Journa
FUSE Observations of a Full Orbit of Hercules X-1: Signatures of Disk, Star, and Wind
We observed an entire 1.7 day orbit of the X-ray binary Hercules X-1 with the
Far Ultraviolet Spectroscopic Explorer (FUSE). Changes in the O VI 1032,1037
line profiles through eclipse ingress and egress indicate a Keplerian accretion
disk spinning prograde with the orbit. These observations may show the first
double-peaked accretion disk line profile to be seen in the Hercules X-1
system. Doppler tomograms of the emission lines show a bright spot offset from
the Roche lobe of the companion star HZ Her, but no obvious signs of the
accretion disk. Simulations show that the bright spot is too far offset from
the Roche lobe to result from uneven X-ray heating of its surface. The absence
of disk signatures in the tomogram can be reproduced in simulations which
include absorption from a stellar wind. We attempt to diagnose the state of the
emitting gas from the C III 977, C III 1175, and N III 991 emission lines. The
latter may be enhanced through Bowen fluorescence.Comment: Accepted for publication in The Astrophysical Journa
A burst from the direction of UZ Fornacis with XMM-Newton
The XMM-Newton pointing towards the magnetic cataclysmic variable UZ For
finds the source to be a factor > 10^3 fainter than previous EXOSAT and ROSAT
observations. The source was not detected for the majority of a 22 ksec
exposure with the EPIC cameras, suggesting that the accretion rate either
decreased, or stopped altogether. However a 1.1 ksec burst was detected from UZ
For during the observation. Spectral fits favour optically thin, kT = 4.4 keV
thermal emission. Detection of the burst by the on-board Optical Monitor
indicates that this was most probably an accretion event. The 0.1-10 keV
luminosity of 2.1 x 10^30 erg/s is typical for accretion shock emission from
high state polars and would result from the potential energy release of ~ 10^16
g of gas. There is no significant soft excess due to reprocessing in the white
dwarf atmosphere.Comment: 7 pages, 2 postscript figures, ApJL, in pres
The Origin of Soft X-rays in DQ Herculis
DQ Herculis (Nova Herculis 1934) is a deeply eclipsing cataclysmic variable
containing a magnetic white dwarf primary. The accretion disk is thought to
block our line of sight to the white dwarf at all orbital phases due to its
extreme inclination angle. Nevertheless, soft X-rays were detected from DQ Her
with ROSAT PSPC. To probe the origin of these soft X-rays, we have performed
Chandra ACIS observations. We confirm that DQ Her is an X-ray source. The bulk
of the X-rays are from a point-like source and exhibit a shallow partial
eclipse. We interpret this as due to scattering of the unseen central X-ray
source, probably in an accretion disk wind. At the same time, we observe what
appear to be weak extended X-ray features around DQ Her, which we interpret as
an X-ray emitting knot in the nova shell.Comment: 18 pages including 4 figures, accepted for publication in
Astrphyisical Journa
Quasi-Homogeneous Thermodynamics and Black Holes
We propose a generalized thermodynamics in which quasi-homogeneity of the
thermodynamic potentials plays a fundamental role. This thermodynamic formalism
arises from a generalization of the approach presented in paper [1], and it is
based on the requirement that quasi-homogeneity is a non-trivial symmetry for
the Pfaffian form . It is shown that quasi-homogeneous
thermodynamics fits the thermodynamic features of at least some
self-gravitating systems. We analyze how quasi-homogeneous thermodynamics is
suggested by black hole thermodynamics. Then, some existing results involving
self-gravitating systems are also shortly discussed in the light of this
thermodynamic framework. The consequences of the lack of extensivity are also
recalled. We show that generalized Gibbs-Duhem equations arise as a consequence
of quasi-homogeneity of the thermodynamic potentials. An heuristic link between
this generalized thermodynamic formalism and the thermodynamic limit is also
discussed.Comment: 39 pages, uses RevteX. Published version (minor changes w.r.t. the
original one
Size Acceptance: A Discursive Analysis of Online Blogs
This document is an Accepted Manuscript of an article published by Taylor & Francis Group in Fat Studies on 25 May 2018, available online at: https://doi.org/10.1080/21604851.2018.1473704. Under embargo until 25 May 2019.Dominant discourses of âfatnessâ and âfat peopleâ have implications for physical and mental health. Although alternative discourses such as âsize acceptanceâ exist, there has been little consideration of the ways in which these alternative arguments (and speakers) may be positioned to be heard. Using a discursive thematic analysis, the authors demonstrate that size acceptance online bloggers have created a community online that enables them to persuasively provide alternative claims to âexpertise,â which positions their views as credible and legitimate alternatives to those of more established authority figuresâsuch as health professionals. This has implications not only for the lived experience of fat people, but also for researchers by emphasizing the importance of exploring not just what is said, but how, if we are to understand how different articulated positions are to be persuasive.Peer reviewe
Low-Temperature Fluorocarbonate Mineralization in Lower Devonian Rhynie Chert, UK
Funding: J.G.T.A was partially funded by the Natural Environment Research Council, grant number NE/T003677/1. Acknowledgments: We are grateful to W. Ritchie, J. Johnston, and J. Bowie for skilled technicalsupport. Samples were archived by N.H. Trewin, C.M. Rice and S. Fayers.Peer reviewedPublisher PD
LS Peg: A Low-Inclination SW Sextantis-Type Cataclysmic Binary with High-Velocity Balmer Emission Line Wings
We present time-resolved spectroscopy and photometry of the bright
cataclysmic variable LS Peg (= S193). The Balmer lines exhibit broad,
asymmetric wings Doppler-shifted by about 2000 km/s at the edges, while the HeI
lines show phase-dependent absorption features strikingly similar to SW
Sextantis stars, as well as emission through most of the phase. The CIII/NIII
emission blend does not show any phase dependence. From velocities of Halpha
emission lines, we determine an orbital period of 0.174774 +/- 0.000003 d (=
4.1946 h), which agrees with Szkody's (1995) value of approximately 4.2 hours.
No stable photometric signal was found at the orbital period. A non-coherent
quasi-periodic photometric signal was seen at a period of 20.7 +/- 0.3 min.
The high-velocity Balmer wings most probably arise from a stream re-impact
point close to the white dwarf. We present simulated spectra based on a
kinematic model similar to the modified disk-overflow scenario of Hellier &
Robinson (1994). The models reproduce the broad line wings, though some other
details are unexplained.
Using an estimate of dynamical phase based on the model, we show that the
phasing of the emission- and absorption-line variations is consistent with that
in (eclipsing) SW Sex stars. We therefore identify LS Peg as a low-inclination
SW Sex star.
Our model suggests i = 30 deg, and the observed absence of any photometric
signal at the orbital frequency establishes i < 60 deg. This constraint puts a
severe strain on interpretations of the SW Sex phenomenon which rely on disk
structures lying slightly out of the orbital plane.Comment: 29 pages, 13 figures, to be published in PASP Feb. 199
The intriguing nature of the high energy gamma ray source XSSJ12270-4859
The nature of the hard X-ray source XSSJ12270-4859 is still unclear though it
was claimed to be a magnetic Cataclysmic Variable. We here present a broad-band
X-ray and gamma ray study based on a recent XMM-Newton observation and archival
INTEGRAL and RXTE data. From the Fermi/LAT 1-year point source catalogue, we
tentatively associate XSSJ12270-4859 with 1FGLJ1227.9-4852, a source of high
energy gamma rays with emission up to 10GeV. We complement the study with UV
photometry from XMM-Newton and ground-based optical and near-IR photometry. The
X-ray emission is highly variable showing flares and intensity dips. The X-ray
flares consist of flare-dip pairs. Flares are also detected in the UV range but
not the dips. Aperiodic dipping behaviour is also observed during X-ray
quiescence but not in the UV. The 0.2-100keV spectrum is featureless and
described by a power law model with Gamma=1.7. The 100MeV-10GeV spectrum is
instead represented by a power law index of 2.45. The luminosity ratio between
0.1-100GeV and 0.2--100keV is ~0.8, hence the GeV emission is a significant
component of the total energy output. Furthermore, the X-ray spectrum does not
greatly change during flares, quiescence and the dips seen in quiescence but it
hardens during the post-flare dips. Optical photometry reveals a period of
4.32hr likely related to the binary orbit. Near-IR, possibly ellipsoidal,
variations are detected. Large amplitude variability on shorter (tens mins)
timescales are found to be non-periodic. The observed variability at all
wavelengths and the spectral characteristics strongly favour a low-mass
atypical low-luminosity X-ray binary and are against a Cataclysmic Variable
nature. The association with a Fermi/LAT high energy gamma ray source further
strengths this interpretation.Comment: 12 pages, 11 figures, 3 tables; Accepted for publication in Astronomy
& Astrophysics Main Journ
Secondary-Structure Design of Proteins by a Backbone Torsion Energy
We propose a new backbone-torsion-energy term in the force field for protein
systems. This torsion-energy term is represented by a double Fourier series in
two variables, the backbone dihedral angles phi and psi. It gives a natural
representation of the torsion energy in the Ramachandran space in the sense
that any two-dimensional energy surface periodic in both phi and psi can be
expanded by the double Fourier series. We can then easily control
secondary-structure-forming tendencies by modifying the torsion-energy surface.
For instance, we can increase/decrease the alpha-helix-forming-tendencies by
lowering/raising the torsion-energy surface in the alpha-helix region and
likewise increase/decrease the beta-sheet-forming tendencies by
lowering/raising the surface in the beta-sheet region in the Ramachandran
space. We applied our approach to AMBER parm94 and AMBER parm96 force fields
and demonstrated that our modifications of the torsion-energy terms resulted in
the expected changes of secondary-structure-forming-tendencies by performing
folding simulations of alpha-helical and beta-hairpin peptides.Comment: 13 pages, (Revtex4), 5 figure
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