27 research outputs found
LGBTQ Training for Aquatic Employees: Impact on Attitudes and Professional Competencies
This study examined the impact of a LGBTQ diversity training on the attitudes and professional competencies of aquatic employees within a campus recreational sports setting. While diversity training is often discussed as a key component of inclusive aquatic programming, little empirical research examining the outcomes associated with such trainings exists. As such, members of the research team developed, implemented, and evaluated a four-month long training program consisting of one in-person training session and monthly inclusion handouts discussing issues related to the inclusion of LGBTQ participants. A comparative quantitative research design was used to measure employee’s attitudes towards the LGBTQ population and inclusive-recreational sports aquatic professional competencies for both individuals who underwent the training and a control group of employees who did not participate in the training. Results indicate initial support for this training initiative with those who attended the training scoring higher on average in both attitudinal and competency-based measures
We Just Treat Everyone the Same : LGBTQ Aquatic Management Strategies, Barriers and Implementation
This study examined the management of aquatic venues in a number of areas (facilities, programming, human resource management, marketing, policies) as it pertains to LGBTQ participants and participation. The study utilized in-depth semi-structured interviews with 16 aquatic managers to examine steps that are currently being taken (or lack thereof) when it comes to creating environments that are perceived to be open, or closed, to LGBTQ participants. A grounded theory-based process of data collection and analysis resulted in emergent themes. These themes included: (a) gendered spaces, (b) non-aquatic initiatives, (c) staff knowledgeability, (d) departmental and organizational mission, (e) aquatic-specific programming and regulations and (f) barriers to inclusion. Management strategies around these emergent themes are discussed, with implications for aquatic managers regarding the creating of inclusive environments for LGBTQ participant populations
Turbulence driven by outflow-blown cavities in the molecular cloud of NGC 1333
Outflows from young stellar objects have been identified as a possible source
of turbulence in molecular clouds. To investigate the relationship between
outflows, cloud dynamics and turbulence, we compare the kinematics of the
molecular gas associated with NGC 1333, traced in 13CO(1-0), with the
distribution of young stellar objects (YSOs) within. We find a velocity
dispersion of ~ 1-1.6 km/s in 13CO that does not significantly vary across the
cloud, and is uncorrelated with the number of nearby young stellar outflows
identified from optical and submillimeter observations. However, from velocity
channel maps we identify about 20 cavities or depressions in the 13CO intensity
of scales > 0.1-0.2 pc and velocity widths 1-3 km/s. The cavities exhibit limb
brightened rims in both individual velocity channel maps and position velocity
diagrams, suggesting that they are slowly expanding. We interpret these
cavities to be remnants of past YSO outflow activity: If these cavities are
presently empty, they would fill in on time scales of a million years. This can
exceed the lifetime of a YSO outflow phase, or the transit time of the central
star through the cavity, explaining the the absence of any clear correlation
between the cavities and YSO outflows. We find that the momentum and energy
deposition associated with the expansion of the cavities is sufficient to power
the turbulence in the cloud. In this way we conclude that the cavities are an
important intermediary step between the conversion of YSO outflow energy and
momentum into cloud turbulent motions.Comment: Accepted for publication in ApJ. Check out
http://astro.pas.rochester.edu/~aquillen/coolpics.html for channel map and
PosVel movies of N133
Protostellar Outflow Evolution in Turbulent Environments
The link between turbulence in star formatting environments and protostellar
jets remains controversial. To explore issues of turbulence and fossil cavities
driven by young stellar outflows we present a series of numerical simulations
tracking the evolution of transient protostellar jets driven into a turbulent
medium. Our simulations show both the effect of turbulence on outflow
structures and, conversely, the effect of outflows on the ambient turbulence.
We demonstrate how turbulence will lead to strong modifications in jet
morphology. More importantly, we demonstrate that individual transient outflows
have the capacity to re-energize decaying turbulence. Our simulations support a
scenario in which the directed energy/momentum associated with cavities is
randomized as the cavities are disrupted by dynamical instabilities seeded by
the ambient turbulence. Consideration of the energy power spectra of the
simulations reveals that the disruption of the cavities powers an energy
cascade consistent with Burgers'-type turbulence and produces a driving
scale-length associated with the cavity propagation length. We conclude that
fossil cavities interacting either with a turbulent medium or with other
cavities have the capacity to sustain or create turbulent flows in star forming
environments. In the last section we contrast our work and its conclusions with
previous studies which claim that jets can not be the source of turbulence.Comment: 24 pages, submitted to the Astrophysical Journa
Protostellar Jets and Turbulence in Molecular Clouds: The Role of Interactions
We present a series of numerical studies of the interaction of colliding
radiative, hydrodynamic young stellar outflows. We study the effect of the
collision impact parameter on the acceleration of ambient material and the
degree to which the flow is isotropized by the collision as a mechanism for
driving turbulence in the parent molecular cloud. Our results indicate that the
high degrees of compression of outflow material, achieved through radiative
shocks near the vertex of the interaction, prevents the redirected outflow from
spraying over a large spatial region. Furthermore, the collision reduces the
redirected outflow's ability to entrain and impart momentum into the ambient
cloud. Consideration of the probabilities of outflow collisions leads us to
conclude that individual low velocity fossil outflows are the principle
coupling between outflows and the cloud.Comment: 21 pages, 10 figures, submitted to Ap
The epsilon Chamaeleontis young stellar group and the characterization of sparse stellar clusters
We present the outcomes of a Chandra X-ray Observatory snapshot study of five
nearby Herbig Ae/Be (HAeBe) stars which are kinematically linked with the
Oph-Sco-Cen Association (OSCA). Optical photometric and spectroscopic followup
was conducted for the HD 104237 field. The principal result is the discovery of
a compact group of pre-main sequence (PMS) stars associated with HD 104237 and
its codistant, comoving B9 neighbor epsilon Chamaeleontis AB. We name the group
after the most massive member. The group has five confirmed stellar systems
ranging from spectral type B9-M5, including a remarkably high degree of
multiplicity for HD 104237 itself. The HD 104237 system is at least a quintet
with four low mass PMS companions in nonhierarchical orbits within a projected
separation of 1500 AU of the HAeBe primary. Two of the low-mass members of the
group are actively accreting classical T Tauri stars. The Chandra observations
also increase the census of companions for two of the other four HAeBe stars,
HD 141569 and HD 150193, and identify several additional new members of the
OSCA.
We discuss this work in light of several theoretical issues: the origin of
X-rays from HAeBe stars; the uneventful dynamical history of the
high-multiplicity HD 104237 system; and the origin of the epsilon Cha group and
other OSCA outlying groups in the context of turbulent giant molecular clouds.
Together with the similar eta Cha cluster, we paint a portrait of sparse
stellar clusters dominated by intermediate-mass stars 5-10 Myr after their
formation.Comment: Accepted for publication in the Astrophysical Journal. 32 pages and 7
figure
Outflow Driven Turbulence in Molecular Clouds
In this paper we explore the relationship between protostellar outflows and
turbulence in molecular clouds. Using 3-D numerical simulations we focus on the
hydrodynamics of multiple outflows interacting within a parsec scale volume. We
explore the extent to which transient outflows injecting directed energy and
momentum into a sub-volume of a molecular cloud can be converted into random
turbulent motions. We show that turbulence can readily be sustained by these
interactions and show that it is possible to broadly characterize an effective
driving scale of the outflows. We compare the velocity spectrum obtained in our
studies to that of isotropically forced hydrodynamic turbulence finding that in
outflow driven turbulence a power law is indeed achieved. However we find a
steeper spectrum (beta ~ 3) is obtained in outflow driven turbulence models
than in isotropically forced simulations (beta ~ 2). We discuss possible
physical mechanisms responsible for these results as well and their
implications for turbulence in molecular clouds where outflows will act in
concert with other processes such as gravitational collapse.Comment: 12 pages, 3 figure
Chandra Study of Young Stellar Objects in the NGC 1333 Star-forming Cloud
NGC 1333, a highly active star formation region within the Perseus molecular
cloud complex, has been observed with the ACIS-I detector on board the Chandra
X-ray Observatory. In our image with a sensitivity limit of ~ 1e28 erg/s, we
detect 127 X-ray sources, of which, 95 are known cluster members. The X-ray
luminosity function of the discovered YSO population spans a range of
1e28-3.2e31 erg/s in the 0.5-8 keV band. Comparison with K-band source counts
indicates that we detect all of the known cluster members with K < 12, and
about half of members with K > 12. We detect seven X-ray emitting YSOs which
drive optically visible jets as well as one deeply embedded object that has not
been detected in near-IR observations. The presence or absence of an outflows
does not appear to produce any difference in X-ray properties of YSOs. We also
find no systematic differences in X-ray luminosity distributions between two
complete subsamples of CTTs and WTTs. That suggests that there is no difference
in the astrophysical mechanism of WTT and CTT X-ray emission production.
Additional results include: the X-ray emission from two late-B stars which
illuminate the reflection nebula originates from unresolved late-type
companions; two T Tauri stars are discovered as previously unknown components
of visual binaries; and the X-ray counterpart of SVS 16 has the column density
much lower than that expected from near-IR photometry and thus its X-ray
luminosity is not anomalously high, as has been previously suggested.Comment: 53 pages, 14 figures, 3 tables. To appear in the Astrophysical
Journal; scheduled for 2002, ApJ, 575 (August 10th). High quality copy
available at ftp://ftp.astro.psu.edu/pub/gkosta/ngc1333
The Eta Chamaeleontis Cluster: Origin in the Sco-Cen OB Association
A young, nearby compact aggregate of X-ray emitting pre-main sequence stars
was recently discovered in the vicinity of eta Cha (B8V). In this paper, we
further investigate this cluster: its membership, its environs and origins.
ROSAT HRI X-ray data for the cluster's T Tauri stars show high levels of
magnetic activity and variability. The cluster has an anomalous X-ray
luminosity function compared to other young clusters, deficient in stars with
low, but detectable X-ray luminosities. This suggests that many low-mass
members have escaped the surveyed core region. Photographic photometry from the
USNO-A2.0 catalog indicates that additional, X-ray-quiet members exist in the
cluster core region. The components of the eclipsing binary RS Cha, previously
modeled in the literature as post-MS with discordant ages, are shown to be
consistent with being coeval pre-MS stars. We compute the Galactic motion of
the cluster from Hipparcos data, and compare it to other young stars and
associations in the fourth Galactic quadrant. The kinematic study shows that
the eta Cha cluster, the TW Hya association, and a new group near epsilon Cha,
probably originated near the giant molecular cloud complex that formed the two
oldest subgroups of the Sco-Cen OB association roughly 10-15 Myr ago. Their
dispersal is consistent with the velocity dispersions seen in giant molecular
clouds. A large H I filament and dust lane located near eta Cha has been
identified as part of a superbubble formed by Sco-Cen OB winds and supernova
remnants. The passage of the superbubble may have terminated star-formation in
the eta Cha cluster and dispersed its natal molecular gas.Comment: 26 pages, 9 figures, LaTex2.09, ApJ, in press,
http://etacha.as.arizona.edu/~eem/etacha/MLF00/index.htm
A High Resolution Study of the HI-H2 Transition across the Perseus Molecular Cloud
To investigate the fundamental principles of H2 formation in a giant
molecular cloud (GMC), we derive the HI and H2 surface density (Sigma_HI and
Sigma_H2) images of the Perseus molecular cloud on sub-pc scales (~0.4 pc). We
use the far-infrared data from the Improved Reprocessing of the IRAS Survey and
the V-band extinction image provided by the COMPLETE Survey to estimate the
dust column density image of Perseus. In combination with the HI data from the
Galactic Arecibo L-band Feed Array HI Survey and an estimate of the local
dust-to-gas ratio, we then derive the Sigma_H2 distribution across Perseus. We
find a relatively uniform Sigma_HI ~ 6-8 Msun pc^-2 for both dark and
star-forming regions, suggesting a minimum HI surface density required to
shield H2 against photodissociation. As a result, a remarkably tight and
consistent relation is found between Sigma_H2/Sigma_HI and Sigma_HI+Sigma_H2.
The transition between the HI- and H2-dominated regions occurs at N(HI)+2N(H2)
~ (8-14) x 10^20 cm^-2. Our findings are consistent with predictions for H2
formation in equilibrium, suggesting that turbulence may not be of primary
importance for H2 formation. However, the importance of a warm neutral medium
for H2 shielding, an internal radiation field, and the timescale of H2
formation still remain as open questions. We also compare H2 and CO
distributions and estimate the fraction of "CO-dark" gas, f_DG ~ 0.3. While
significant spatial variations of f_DG are found, we do not find a clear
correlation with the mean V-band extinction.Comment: updated to match the final version published in April 201