137 research outputs found
Feasibility, Acceptability and Preliminary Outcomes of Embracing Your Life: An Online Self-Compassion Program for Emerging Adults
Due to the psychological toll COVID-19 has had on emerging adults, as well as normative mental health challenges of this developmental period, emerging adults are struggling more than ever with depression and loneliness. The objective of this study was to assess feasibility, acceptability, and preliminary psychosocial outcomes of Embracing Your Life, a self-compassion program for emerging adults, as self-compassion is associated with better mental health. Thirty-nine emerging adults (Mage = 23.7, 67% female) enrolled in a 6-session online program from July 2020 to January 2022 participated in this study. Results indicated the program was feasible; 81% of participants attended at least five out of six sessions. Qualitative feedback indicated high acceptability, with recommended changes to make the program more interactive. Participants reported significant improvements in self-compassion, resilience, loneliness, depression, stress, and emotion regulation. Conclusions are that Embracing Your Life is a promising, accessible intervention to address the mental health of emerging adults
Long-Term Profile Variability in Active Galactic Nuclei with Double-Peaked Balmer Emission Lines
An increasing number of Active Galactic Nuclei (AGNs) exhibit broad,
double-peaked Balmer emission lines,which represent some of the best evidence
for the existence of relatively large-scale accretion disks in AGNs. A set of
20 double-peaked emitters have been monitored for nearly a decade in order to
observe long-term variations in the profiles of the double-peaked Balmer lines.
Variations generally occur on timescales of years, and are attributed to
physical changes in the accretion disk. Here we characterize the variability of
a subset of seven double-peaked emitters in a model independent way. We find
that variability is caused primarily by the presence of one or more discrete
"lumps" of excess emission; over a timescale of a year (and sometimes less)
these lumps change in amplitude and shape, but the projected velocity of these
lumps changes over much longer timescales (several years). We also find that
all of the objects exhibit red peaks that are stronger than the blue peak at
some epochs and/or blueshifts in the overall profile, contrary to the
expectations for a simple, circular accretion disk model, thus emphasizing the
need for asymmetries in the accretion disk. Comparisons with two simple models,
an elliptical accretion disk and a circular disk with a spiral arm, are unable
to reproduce all aspects of the observed variability, although both account for
some of the observed behaviors. Three of the seven objects have robust
estimates of the black hole masses. For these objects the observed variability
timescale is consistent with the expected precession timescale for a spiral
arm, but incompatible with that of an elliptical accretion disk. We suggest
that with the simple modification of allowing the spiral arm to be fragmented,
many of the observed variability patterns could be reproduced.Comment: 74 pages, 4 tables, 35 figure
The Impact of Cluster Structure and Dynamical State on Scatter in the Sunyaev-Zel'dovich Flux-Mass Relation
Cosmological constraints from cluster surveys rely on accurate mass estimates
from the mass-observable relations. In order to avoid systematic biases and
reduce uncertainties, we study the form and physical origin of the intrinsic
scatter about the mean Sunyaev-Zel'dovich (SZ) flux-mass relation using a
hydrodynamical simulation of galaxy cluster formation. We examine the
assumption of lognormal scatter and detect non-negligible positive skewness and
kurtosis (> 0.5) for a wide range of limiting masses and redshifts. These
higher-order moments should be included in the parametrization of scatter in
order not to bias cosmological constraints. We investigate the sources of the
scatter by correlating it with measures of cluster morphology, halo
concentration, and dynamical state, and we quantify the individual contribution
from each source. We find that statistically the impact of dynamical state is
weak, so the selection bias due to mergers is negligible. On the other hand,
there is a strong correlation between the scatter and halo concentration, which
can be used to reduce the scatter significantly (from 12.07% to 7.34% or by
~40% for clusters at z = 0). We also show that a cross-calibration by combining
information from X-ray followups can be used to reduce the scatter in the
flux-mass relation and also identify outliers in both X-ray and SZ cluster
surveys.Comment: 14 pages, 12 figures; accepted for publication in Ap
An HI Threshold for Star Cluster Formation in Tidal Debris
Super star clusters are young, compact star clusters found in the central
regions of interacting galaxies. Recently, they have also been reported to
preferentially form in certain tidal tails, but not in others. In this paper,
we have used 21 cm HI maps and the Hubble Space Telescope Wide Field Planetary
Camera 2 images of eight tidal tail regions of four merging galaxy pairs to
compare the kiloparsec scale HI distribution with the location of super star
clusters found from the optical images. For most of the tails, we find that
there is an increase in super star cluster density with increasing projected HI
column density, such that the star cluster density is highest when log N(HI) >=
20.6 cm^{-2}, but equal to the background count rate at lower HI column
density. However, for two tails (NGC 4038/39 Pos A and NGC 3921), there is no
significant star cluster population despite the presence of gas at high column
density. This implies that the N(HI) threshold is a necessary but not
sufficient condition for cluster formation. Gas volume density is likely to
provide a more direct criterion for cluster formation, and other factors such
as gas pressure or strength of encounter may also have an influence. Comparison
of HI thresholds needed for formation of different types of stellar structures
await higher resolution HI and optical observations of larger numbers of
interacting galaxies.Comment: 19 pages, 6 figures, 3 tables, accepted for publication in MNRA
Finding Apparent Horizons in Dynamic 3D Numerical Spacetimes
We have developed a general method for finding apparent horizons in 3D
numerical relativity. Instead of solving for the partial differential equation
describing the location of the apparent horizons, we expand the closed 2D
surfaces in terms of symmetric trace--free tensors and solve for the expansion
coefficients using a minimization procedure. Our method is applied to a number
of different spacetimes, including numerically constructed spacetimes
containing highly distorted axisymmetric black holes in spherical coordinates,
and 3D rotating, and colliding black holes in Cartesian coordinates.Comment: 19 pages, 13 figures, LaTex, to appear in Phys. Rev. D. Minor changes
mad
Carbon isotope fractionation in protoplanetary disks
We investigate the gas-phase and grain-surface chemistry in the inner 30 AU
of a typical protoplanetary disk using a new model which calculates the gas
temperature by solving the gas heating and cooling balance and which has an
improved treatment of the UV radiation field. We discuss inner-disk chemistry
in general, obtaining excellent agreement with recent observations which have
probed the material in the inner regions of protoplanetary disks. We also apply
our model to study the isotopic fractionation of carbon. Results show that the
fractionation ratio, 12C/13C, of the system varies with radius and height in
the disk. Different behaviour is seen in the fractionation of different
species. We compare our results with 12C/13C ratios in the Solar System comets,
and find a stark contrast, indicative of reprocessing.Comment: 50 pages, 10 figures, accepted for publication in the Astrophysical
Journa
CIV Emission and the Ultraviolet through X-ray Spectral Energy Distribution of Radio-Quiet Quasars
In the restframe UV, two of the parameters that best characterize the range
of emission-line properties in quasar broad emission-line regions are the
equivalent width and the blueshift of the CIV line relative to the quasar rest
frame. We explore the connection between these emission-line properties and the
UV through X-ray spectral energy distribution (SED) for radio-quiet (RQ)
quasars. Our sample consists of a heterogeneous compilation of 406 quasars from
the Sloan Digital Sky Survey and Palomar-Green survey that have well-measured
CIV emission-line and X-ray properties (including 164 objects with measured
Gamma). We find that RQ quasars with both strong CIV emission and small CIV
blueshifts can be classified as "hard-spectrum" sources that are (relatively)
strong in the X-ray as compared to the UV. On the other hand, RQ quasars with
both weak CIV emission and large CIV blueshifts are instead "soft-spectrum"
sources that are (relatively) weak in the X-ray as compared to the UV. This
work helps to further bridge optical/soft X-ray "Eigenvector 1" relationships
to the UV and hard X-ray. Based on these findings, we argue that future work
should consider systematic errors in bolometric corrections (and thus accretion
rates) that are derived from a single mean SED. Detailed analysis of the CIV
emission line may allow for SED-dependent corrections to these quantities.Comment: AJ, in press; 39 pages, 11 figures, 3 table
Ice Lines, Planetesimal Composition and Solid Surface Density in the Solar Nebula
To date, there is no core accretion simulation that can successfully account
for the formation of Uranus or Neptune within the observed 2-3 Myr lifetimes of
protoplanetary disks. Since solid accretion rate is directly proportional to
the available planetesimal surface density, one way to speed up planet
formation is to take a full accounting of all the planetesimal-forming solids
present in the solar nebula. By combining a viscously evolving protostellar
disk with a kinetic model of ice formation, we calculate the solid surface
density in the solar nebula as a function of heliocentric distance and time. We
find three effects that strongly favor giant planet formation: (1) a decretion
flow that brings mass from the inner solar nebula to the giant planet-forming
region, (2) recent lab results (Collings et al. 2004) showing that the ammonia
and water ice lines should coincide, and (3) the presence of a substantial
amount of methane ice in the trans-Saturnian region. Our results show higher
solid surface densities than assumed in the core accretion models of Pollack et
al. (1996) by a factor of 3 to 4 throughout the trans-Saturnian region. We also
discuss the location of ice lines and their movement through the solar nebula,
and provide new constraints on the possible initial disk configurations from
gravitational stability arguments.Comment: Version 2: reflects lead author's name and affiliation change,
contains minor changes to text from version 1. 12 figures, 7 tables, accepted
for publication in Icaru
Breast cancer risk and hormone receptor status in older women by parity, age of first birth, and breastfeeding: a case-control study.
BACKGROUND: Early age at first birth and multiparity reduce the risk of estrogen receptor-progesterone receptor (ERPR)-positive breast cancer, whereas breastfeeding reduces the risk of both ERPR-positive and ERPR-negative cancers. METHODS: We used multivariable logistic regression analysis to investigate whether age at first birth ( or =25 years) and breastfeeding (ever/never) modify the long-term effect of parity on risk of ERPR-positive and ERPR-negative cancer using 1,457 incident breast cancer cases and 1,455 controls ages > or =55 years who participated in the Women's Contraceptive and Reproductive Experiences Study. RESULTS: Women who gave birth before age 25 years had a 36% reduced risk of breast cancer compared with nulligravida that was not observed for women who started their families at an older age (P(heterogeneity) = 0.0007). This protective effect was restricted to ERPR-positive breast cancer (P(heterogeneity) = 0.004). Late age at first birth increased the risk of ERPR-negative cancers. Additional births reduced the risk of ERPR-positive cancers among women with an early first birth (P(trend) = 0.0001) and among women who breastfed (P(trend) = 0.004) but not among older mothers or those who never breastfed. In women with a late first birth who never breastfed, multiparity was associated with increased risk of breast cancer. CONCLUSIONS: These findings suggest that the effect of parity on a woman's long-term risk of breast cancer is modified by age at first full-term pregnancy and possibly by breastfeeding
The Influence of Concentration and Dynamical State on Scatter in the Galaxy Cluster Mass-Temperature Relation
Using a hydrodynamics plus N-body simulation of galaxy cluster formation
within a large volume and mock Chandra X-ray observations, we study the form
and evolution of the intrinsic scatter about the best-fit X-ray
temperature-mass relation for clusters. We investigate the physical origin of
the scatter by correlating it with quantities that are closely related to
clusters' formation and merging histories. We also examine the distribution of
the scatter for merging and nonmerging populations, identified using halo
merger trees derived from the simulation as well as X-ray substructure
measures. We find a strong correlation between the scatter in the M-T_X
relation and the halo concentration, in the sense that more concentrated
clusters tend to be cooler than clusters with similar masses. No bias is found
between the merging and relaxed clusters, but merging clusters generally have
greater scatter, which is related to the properties of the distribution of halo
concentrations. We also detect a signature of non-lognormality in the
distribution of scatter for our simulated clusters both at z=0 and at z=1. A
detailed comparison of merging clusters identified by substructure measures and
by halo merger trees is given in the discussion. We conclude that, when
cooling-related effects are neglected, the variation in halo concentrations is
a more important factor for driving the intrinsic scatter in the M-T_X
relation, while departures from hydrostatic equilibrium due to cluster mergers
have a minor effect.Comment: Accepted for publication in ApJ (17 pages, 13 figures, double
column), updated to match version to appear in Ap
- …