640 research outputs found
Wide-Field Survey of Emission-line Stars in IC 1396
We have made an extensive survey of emission-line stars in the IC 1396 HII
region to investigate the low-mass population of pre-main sequence (PMS) stars.
A total of 639 H-alpha emission-line stars were detected in an area of 4.2
deg^2 and their i'-photometry was measured. Their spatial distribution exhibits
several aggregates near the elephant trunk globule (Rim A) and bright-rimmed
clouds at the edge of the HII region (Rim B and SFO 37, 38, 39, 41), and near
HD 206267, which is the main exciting star of the HII region. Based on the
extinction estimated from the near-infrared (NIR) color-color diagram, we have
selected pre-main sequence star candidates associated with IC 1396. The age and
mass were derived from the extinction corrected color-magnitude diagram and
theoretical pre-main sequence tracks. Most of our PMS candidates have ages of <
3 Myr and masses of 0.2-0.6 Mo. Although it appears that only a few stars were
formed in the last 1 Myr in the east region of the exciting star, the age
difference among subregions in our surveyed area is not clear from the
statistical test. Our results may suggest that massive stars were born after
the continuous formation of low-mass stars for 10 Myr. The birth of the
exciting star could be the late stage of slow but contiguous star formation in
the natal molecular cloud. It may have triggered to form many low-mass stars at
the dense inhomogeneity in and around the HII region by a radiation-driven
implosion.Comment: 48 pages, 12 figures, 5 tables, accepted for publication in A
The Elephant Trunk Nebula and the Trumpler 37 cluster: Contribution of triggered star formation to the total population of an HII region
Rich young stellar clusters produce HII regions whose expansion into the
nearby molecular cloud is thought to trigger the formation of new stars.
However, the importance of this mode of star formation is uncertain. This
investigation seeks to quantify triggered star formation (TSF) in IC 1396A
(a.k.a., the Elephant Trunk Nebula), a bright rimmed cloud (BRC) on the
periphery of the nearby giant HII region IC 1396 produced by the Trumpler 37
cluster. X-ray selection of young stars from Chandra X-ray Observatory data is
combined with existing optical and infrared surveys to give a more complete
census of the TSF population. Over 250 young stars in and around IC 1396A are
identified; this doubles the previously known population. A spatio-temporal
gradient of stars from the IC 1396A cloud toward the primary ionizing star HD
206267 is found. We argue that the TSF mechanism in IC 1396A is the
radiation-driven implosion process persisting over several million years.
Analysis of the X-ray luminosity and initial mass functions indicates that >140
stars down to 0.1 Msun were formed by TSF. Considering other BRCs in the IC
1396 HII region, we estimate the TSF contribution for the entire HII region
exceeds 14-25% today, and may be higher over the lifetime of the HII region.
Such triggering on the periphery of HII regions may be a significant mode of
star formation in the Galaxy.Comment: Accepted for publication in MNRAS; 28 pages, 18 figure
A comprehensive framework for the activation, management, and evaluation of Co-production in the public sector
Co-production analyses the practices in which state or firms and lay actors work together in any phase of the production cycle. In the public sector, citizens are not seen as mere recipients of services but as co-producers at different stages. Scholarly interest in co-production has grown steadily in the past years. However, the research has yet to integrate the many co-production concepts into a distinctive theoretical comprehensive framework able to strengthen the understanding of the interrelated dynamics at play. The article conducts a systematic in- depth qualitative review of the co-production literature for the public sector. The results highlight the main components into four pillars of a comprehensive theoretical framework to guide scholars and practitioners in the activation and management of co-production as well as in the evaluation of its outcomes. The article concludes by formulating a future research agenda for co-production in the public sector
Protoplanetary Disk Evolution around the Triggered Star Forming Region Cepheus B
The Cepheus B (CepB) molecular cloud and a portion of the nearby CepOB3b OB
association, one of the most active regions of star formation within 1 kpc,
have been observed with the IRAC detector on board the Spitzer Space Telescope.
The goals are to study protoplanetary disk evolution and processes of
sequential triggered star formation in the region. Out of ~400 pre-main
sequence (PMS) stars selected with an earlier Chandra X-ray Observatory
observation, 95% are identified with mid-infrared sources and most of these are
classified as diskless or disk-bearing stars. The discovery of the additional
>200 IR-excess low-mass members gives a combined Chandra+Spitzer PMS sample
complete down to 0.5 Mo outside of the cloud, and somewhat above 1 Mo in the
cloud. Analyses of the nearly disk-unbiased combined Chandra+Spitzer selected
stellar sample give several results. Our major finding is a spatio-temporal
gradient of young stars from the hot molecular core towards the primary
ionizing O star HD 217086. This strongly supports the radiation driven
implosion (RDI) model of triggered star formation in the region. The empirical
estimate for the shock velocity of 1 km/s is very similar to theoretical models
of RDI in shocked molecular clouds...ABRIDGED... Other results include: 1.
agreement of the disk fractions, their mass dependency, and fractions of
transition disks with other clusters; 2. confirmation of the youthfulness of
the embedded CepB cluster; 3. confirmation of the effect of suppression of
time-integrated X-ray emission in disk-bearing versus diskless systems.Comment: Accepted for publication in The Astrophysical Journal. 48 pages, 14
figures. For a version with high-quality figures, see
http://www.astro.psu.edu/users/gkosta/RESEARCH/cepb_spitzer_chandra.pd
MBM 12: young protoplanetary discs at high galactic latitude
(abridged) We present Spitzer infrared observations to constrain disc and
dust evolution in young T Tauri stars in MBM 12, a star-forming cloud at high
latitude with an age of 2 Myr and a distance of 275 pc. The region contains 12
T Tauri systems, with primary spectral types between K3 and M6; 5 are weak-line
and the rest classical T Tauri stars. We first use MIPS and literature
photometry to compile spectral energy distributions for each of the 12 members
in MBM 12, and derive their IR excesses. The IRS spectra are analysed with the
newly developed two-layer temperature distribution (TLTD) spectral
decomposition method. For the 7 T Tauri stars with a detected IR excess, we
analyse their solid-state features to derive dust properties such as
mass-averaged grain size, composition and crystallinity. We find a spatial
gradient in the forsterite to enstatite range, with more enstatite present in
the warmer regions. The fact that we see a radial dependence of the dust
properties indicates that radial mixing is not very efficient in the discs of
these young T Tauri stars. The SED analysis shows that the discs in MBM 12, in
general, undergo rapid inner disc clearing, while the binary sources have
faster discevolution. The dust grains seem to evolve independently from the
stellar properties, but are mildly related to disc properties such as flaring
and accretion rates.Comment: 14 pages, accepted by Astronomy and Astrophysic
Geometry of phase separation
We study the domain geometry during spinodal decomposition of a 50:50 binary
mixture in two dimensions. Extending arguments developed to treat non-conserved
coarsening, we obtain approximate analytic results for the distribution of
domain areas and perimeters during the dynamics. The main approximation is to
regard the interfaces separating domains as moving independently. While this is
true in the non-conserved case, it is not in the conserved one. Our results can
therefore be considered as a first-order approximation for the distributions.
In contrast to the celebrated Lifshitz-Slyozov-Wagner distribution of
structures of the minority phase in the limit of very small concentration, the
distribution of domain areas in the 50:50 case does not have a cut-off. Large
structures (areas or perimeters) retain the morphology of a percolative or
critical initial condition, for quenches from high temperatures or the critical
point respectively. The corresponding distributions are described by a tail, where and are exactly known. With increasing time,
small structures tend to have a spherical shape with a smooth surface before
evaporating by diffusion. In this regime the number density of domains with
area scales as , as in the Lifshitz-Slyozov-Wagner theory. The
threshold between the small and large regimes is determined by the
characteristic area, . Finally, we study the
relation between perimeters and areas and the distribution of boundary lengths,
finding results that are consistent with the ones summarized above. We test our
predictions with Monte Carlo simulations of the 2d Ising Model.Comment: 10 pages, 8 figure
High-Resolution Spectroscopy in Tr37: Gas Accretion Evolution in Evolved Dusty Disks
Using the Hectochelle multifiber spectrograph, we have obtained
high-resolution (R~34,000) spectra in the Halpha region for a large number of
stars in the 4 Myr-old cluster Tr 37, containing 146 previously known members
and 26 newly identified ones. We present the Halpha line profiles of all
members, compare them to our IR observations of dusty disks (2MASS/JHK + IRAC +
MIPS 24 micron), use the radial velocities as a membership criterion, and
calculate the rotational velocities. We find a good correlation between the
accretion-broadened profiles and the presence of protoplanetary disks, noting
that a small fraction of the accreting stars presents broad profiles with
Halpha equivalent widths smaller than the canonical limit separating CTTS and
WTTS. The number of strong accretors appears to be lower than in younger
regions, and a large number of CTTS have very small accretion rates
(dM/dt<10^{-9} Msun/yr). Taking into account that the spectral energy
distributions are consistent with dust evolution (grain growth/settling) in the
innermost disk, this suggests a parallel evolution of the dusty and gaseous
components. We also observe that about half of the "transition objects" (stars
with no IR excesses at wavelengths shorter than ~6 micron) do not show any
signs of active accretion, whereas the other half is accreting with accretion
rates <10^{-9} Msun/yr. These zero or very low accretion rates reveal important
gas evolution and/or gas depletion in the innermost disk, which could be
related to grain growth up to planetesimal or even planet sizes. Finally, we
examine the rotational velocities of accreting and non accreting stars, finding
no significant differences that could indicate disk locking at these ages.Comment: 51 pages, 13 (reduced resolution) figures, 2 tables. AJ in pres
Timescale of Mass Accretion in Pre-Main-Sequence Stars
We present initial result of a large spectroscopic survey aimed at measuring
the timescale of mass accretion in young, pre-main-sequence stars in the
spectral type range K0 - M5. Using multi-object spectroscopy with VIMOS at the
VLT we identified the fraction of accreting stars in a number of young stellar
clusters and associations of ages between 1 - 50 Myr. The fraction of accreting
stars decreases from ~60% at 1.5 - 2 Myr to ~2% at 10 Myr. No accreting stars
are found after 10 Myr at a sensitivity limit of Msun yr-1. We
compared the fraction of stars showing ongoing accretion (f_acc) to the
fraction of stars with near-to-mid infrared excess (f_IRAC). In most cases we
find f_acc < f_IRAC, i.e., mass accretion appears to cease (or drop below
detectable level) earlier than the dust is dissipated in the inner disk. At 5
Myr, 95% of the stellar population has stopped accreting material at a rate of
> 10^{-11} Msun yr-1, while ~20% of the stars show near-infrared excess
emission. Assuming an exponential decay, we measure a mass accretion timescale
(t_acc) of 2.3 Myr, compared to a near-to-mid infrared excess timescale
(t_IRAC) of 2.9 Myr. Planet formation, and/or migration, in the inner disk
might be a viable mechanism to halt further accretion onto the central star on
such a short timescale.Comment: Accepted for publicatio
Understanding the need for novelty from the perspective of self-determination theory
A fundamental tenet of self-determination theory is that the satisfaction of three basic, innate psychological needs for autonomy, competence, and relatedness is necessary for optimal functioning. The aim of this research was to propose novelty as a basic psychological need in self-determination theory and develop a new measure to assess novelty need satisfaction, the Novelty Need Satisfaction Scale (NNSS). Two studies were performed, one at the global lifestyle level (Study 1: general adults, N = 399, Mage = 31.30 years) and the other at a contextual level in physical education (Study 2: first-year post-compulsory secondary school students, N = 1035, Mage = 16.20 years). Participants completed the NNSS alongside measures of psychological needs and regulation styles from self-determination theory and psychological well-being. The six-item NNSS showed adequate psychometric properties and discriminant validity with other psychological needs in both studies. Novelty need satisfaction predicted life satisfaction (Study 1) and intrinsic motivation in physical education (Study 2) independent of the other three psychological needs. Results provide preliminary evidence that need for novelty is a unique candidate need alongside existing needs from self-determination theory, but further confirmatory and experimental research is required
Evolution of Galaxy Star Formation and Metallicity: Impact on Double Compact Object Mergers
In this paper, we study the impact of different galaxy statistics and empirical metallicity scaling relations on the
merging rates and properties of compact object binaries. Firstly, we analyze the similarities and differences of
using the star formation rate functions versus stellar mass functions as galaxy statistics for the computation of
cosmic star formation rate density. We then investigate the effects of adopting the Fundamental Metallicity
Relation versus a classic Mass Metallicity Relation to assign metallicity to galaxies with given properties. We find
that when the Fundamental Metallicity Relation is exploited, the bulk of the star formation occurs at relatively high
metallicities, even at high redshift; the opposite holds when the Mass Metallicity Relation is employed, since in this
case the metallicity at which most of the star formation takes place strongly decreases with redshift. We discuss the
various reasons and possible biases giving rise to this discrepancy. Finally, we show the impact of these different
astrophysical prescriptions on the merging rates and properties of compact object binaries; specifically, we present
results for the redshift-dependent merging rates and for the chirp mass and time delay distributions of the merging
binaries
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