3,262 research outputs found
Protostellar accretion traced with chemistry. High resolution C18O and continuum observations towards deeply embedded protostars in Perseus
Context: Understanding how accretion proceeds is a key question of star
formation, with important implications for both the physical and chemical
evolution of young stellar objects. In particular, very little is known about
the accretion variability in the earliest stages of star formation.
Aims: To characterise protostellar accretion histories towards individual
sources by utilising sublimation and freeze-out chemistry of CO.
Methods: A sample of 24 embedded protostars are observed with the
Submillimeter Array (SMA) in context of the large program "Mass Assembly of
Stellar Systems and their Evolution with the SMA" (MASSES). The size of the
CO emitting region, where CO has sublimated into the gas-phase, is
measured towards each source and compared to the expected size of the region
given the current luminosity. The SMA observations also include 1.3 mm
continuum data, which are used to investigate whether a link can be established
between accretion bursts and massive circumstellar disks.
Results: Depending on the adopted sublimation temperature of the CO ice,
between 20% and 50% of the sources in the sample show extended CO
emission indicating that the gas was warm enough in the past that CO sublimated
and is currently in the process of refreezing; something which we attribute to
a recent accretion burst. Given the fraction of sources with extended CO
emission, we estimate an average interval between bursts of 20000-50000 yr,
which is consistent with previous estimates. No clear link can be established
between the presence of circumstellar disks and accretion bursts, however the
three closest known binaries in the sample (projected separations <20 AU) all
show evidence of a past accretion burst, indicating that close binary
interactions may also play a role in inducing accretion variability.Comment: Accepted for publication in A&A, 21 pages, 13 figure
The First Interferometric Measurements of NH₂D/NH₃ Ratio in Hot Corinos
The chemical evolution of nitrogen during star and planet formation is still not fully understood. Ammonia (NH_{3}) is a key specie in the understanding of the molecular evolution in star-forming clouds and nitrogen isotope fractionation. In this paper, we present high-spatial-resolution observations of multiple emission lines of NH_{3} toward the protobinary system NGC1333 IRAS4A with the Karl G. Jansky Very Large Array. We spatially resolved the binary (hereafter, 4A1 and 4A2) and detected compact emission of NH3 transitions with high excitation energies (≳100 K) from the vicinity of the protostars, indicating the NH_{3} ice has sublimated at the inner hot region. The NH3 column density is estimated to be ∼10^{17}–10^{18} cm^{−2}. We also detected two NH_{2}D transitions, allowing us to constrain the deuterium fractionation of ammonia. The NH_{2}D/NH_{3} ratios are as high as ∼0.3–1 in both 4A1 and 4A2. From comparisons with the astrochemical models in the literature, the high NH_{2}D/NH_{3} ratios suggest that the formation of NH3 ices mainly started in the prestellar phase after the formation of bulk water ice finished, and that the primary nitrogen reservoir in the star-forming cloud could be atomic nitrogen (or N atoms) rather than nitrogen-bearing species such as N_{2} and NH_{3}. The implications on the physical properties of IRAS4A's cores are discussed as well
Enhanced Bovine Colostrum Supplementation Shortens the Duration of Respiratory Disease in Thoroughbred Yearlings
AbstractBovine colostrum (BC) is used in humans as a nutritional supplement for immune support and has been shown to reduce Respiratory disease (RD). Other nutritional supplements, minerals and vitamins including mannan oligosaccharides (MOS), zinc and vitamins A, C and E have also been used for immune support. The aim of this prospective blinded randomized clinical trial was to evaluate the effects of a BC, MOS, zinc and vitamin based enhanced bovine colostrum supplement (BCS) on incidence and duration of RD occurring in yearling horses. 109 yearlings on two Thoroughbred farms in Central Kentucky were randomly assigned to treatment or placebo groups. Yearlings were supplemented once daily for 17 to 25 weeks with 100 g of a high quality commercial BCS (containing 50 g BC) or a full fat soy flour placebo, which were applied as a “top-dress” to feed. Yearlings were observed daily and evaluated weekly for signs of RD. All yearlings completed the study. The proportion of the study period during which each yearling exhibited illness was considerably shorter for BCS yearlings (least squares mean = 23% of the study period) than placebo yearlings (least squares mean = 34% of the study period, P = .002). The average duration of illness was shorter for BCS yearlings (1.96 weeks) than placebo yearlings (4.39 weeks, P < .0001). There was no statistical difference in the incidence of RD in these study yearlings
The young embedded disk L1527 IRS: constraints on the water snowline and cosmic ray ionization rate from HCO+ observations
The water snowline in circumstellar disks is a crucial component in planet
formation, but direct observational constraints on its location remain sparse
due to the difficulty of observing water in both young embedded and mature
protoplanetary disks. Chemical imaging provides an alternative route to locate
the snowline, and HCO isotopologues have been shown to be good tracers in
protostellar envelopes and Herbig disks. Here we present
0.5 resolution (35 au radius) Atacama Large
Millimeter/submillimeter Array (ALMA) observations of HCO and
HCO toward the young (Class 0/I) disk L1527 IRS. Using a
source-specific physical model with the midplane snowline at 3.4 au and a small
chemical network, we are able to reproduce the HCO and HCO
emission, but for HCO only when the cosmic ray ionization rate is lowered
to s. Even though the observations are not sensitive to the
expected HCO abundance drop across the snowline, the reduction in HCO
above the snow surface and the global temperature structure allow us to
constrain a snowline location between 1.8 and 4.1 au. Deep observations are
required to eliminate the envelope contribution to the emission and to derive
more stringent constraints on the snowline location. Locating the snowline in
young disks directly with observations of HO isotopologues may therefore
still be an alternative option. With a direct snowline measurement, HCO
will be able to provide constraints on the ionization rate.Comment: Accepted for publication in ApJ, 15 pages, 6 figures and appendi
Star Formation Under the Outflow: The Discovery of a Non-Thermal Jet from OMC-2 FIR 3 and its Relationship to the Deeply Embedded FIR 4 Protostar
We carried out multiwavelength (0.7-5 cm), multiepoch (1994-2015) Very Large
Array (VLA) observations toward the region enclosing the bright far-IR sources
FIR 3 (HOPS 370) and FIR 4 (HOPS 108) in OMC-2. We report the detection of 10
radio sources, seven of them identified as young stellar objects. We image a
well-collimated radio jet with a thermal free-free core (VLA 11) associated
with the Class I intermediate-mass protostar HOPS 370. The jet presents several
knots (VLA 12N, 12C, 12S) of non-thermal radio emission (likely synchrotron
from shock-accelerated relativistic electrons) at distances of ~7,500-12,500 au
from the protostar, in a region where other shock tracers have been previously
identified. These knots are moving away from the HOPS 370 protostar at ~ 100
km/s. The Class 0 protostar HOPS 108, which itself is detected as an
independent, kinematically decoupled radio source, falls in the path of these
non-thermal radio knots. These results favor the previously proposed scenario
where the formation of HOPS 108 has been triggered by the impact of the HOPS
370 outflow with a dense clump. However, HOPS 108 presents a large proper
motion velocity of ~ 30 km/s, similar to that of other runaway stars in Orion,
whose origin would be puzzling within this scenario. Alternatively, an apparent
proper motion could result because of changes in the position of the centroid
of the source due to blending with nearby extended emission, variations in the
source shape, and /or opacity effects.Comment: 16 pages, 4 figures, accepted for publication in The Astrophysical
Journa
Constraining the Chemical Signatures and the Outburst Mechanism of the Class 0 Protostar HOPS 383
We present observations toward HOPS 383, the first known outbursting Class 0
protostar located within the Orion molecular cloud using ALMA, VLA, and SMA.
The SMA observations reveal envelope scale continuum and molecular line
emission surrounding HOPS 383 at 0.85 mm, 1.1 mm, and 1.3 mm. The images show
that HCO and HCO peaks on or near the continuum, while
NH is reduced at the same position. This reflects the underlying
chemistry where CO evaporating close to the protostar destroys NH while
forming HCO. We also observe the molecular outflow traced by CO () and (). A disk is resolved in the ALMA
0.87 mm dust continuum, orthogonal to the outflow direction, with an apparent
radius of 62 AU. Radiative transfer modeling of the continuum gives disk
masses of 0.02 M when fit to the ALMA visibilities. The models
including VLA 8 mm data indicate that the disk mass could be up to a factor of
10 larger due to lower dust opacity at longer wavelengths. The disk temperature
and surface density profiles from the modeling, and an assumed protostar mass
of 0.5 M suggest that the Toomre parameter before the
outburst, making gravitational instability a viable mechanism to explain
outbursts at an early age if the disk is sufficiently massive.Comment: Accepted by Ap
Resonant Photoemission in f-Electron Systems: Pu and Gd
Resonant photoemission in the Pu 5f and Pu 6p states is compared to that in the Gd 4f and Gd 5p states. Spectral simulations, based upon an atomic model with angular momentum coupling, are compared to the Gd and Pu results. Additional spectroscopic measurements of Pu, including core level photoemission and x-ray absorption, are also presented
Temperature structures of embedded disks: young disks in Taurus are warm
The chemical composition of gas and ice in disks around young stars set the
bulk composition of planets. In contrast to protoplanetary disks (Class II),
young disks that are still embedded in their natal envelope (Class 0 and I) are
predicted to be too warm for CO to freeze out, as has been confirmed
observationally for L1527 IRS. To establish whether young disks are generally
warmer than their more evolved counterparts, we observed five young (Class 0/I
and Class I) disks in Taurus with the Atacama Large Millimeter/submillimeter
Array (ALMA), targeting CO , HCO , HDO
and CHOH transitions at resolution. The different freeze-out temperatures
of these species allow us to derive a global temperature structure. CO
and HCO are detected in all disks, with no signs of CO freeze-out in the
inner 100 au, and a CO abundance close to 10. HCO
emission originates in the surface layers of the two edge-on disks, as
witnessed by the especially beautiful V-shaped emission pattern in
IRAS~04302+2247. HDO and CHOH are not detected, with column density upper
limits more than 100 times lower than for hot cores. Young disks are thus found
to be warmer than more evolved protoplanetary disks around solar analogues,
with no CO freeze-out (or only in the outermost part of 100 au disks)
or CO processing. However, they are not as warm as hot cores or disks around
outbursting sources, and therefore do not have a large gas-phase reservoir of
complex molecules.Comment: Accepted for publication in ApJ. 19 pages, 11 figures, 3 tables (+
appendix
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