4,990 research outputs found
X-ray Properties of Low-Mass Pre-Main Sequence Stars in the Orion Trapezium Cluster
The Chandra High Energy Transmission Gratings (HETG) Orion Legacy Project
(HOLP) is the first comprehensive set of observations of a very young massive
stellar cluster which provides high resolution X-ray spectra of very young
stars over a wide mass range (0.7 - 2.3 Msun). In this paper, we focus on the
six brightest X-ray sources with T Tauri stellar counterparts which are
well-characterized at optical and infra-red wavelengths. All stars show column
densities which are substantially smaller than expected from optical extinction
indicating that the sources are located on the near side of the cluster with
respect to the observer as well as that these stars are embedded in more dusty
environments. Stellar X-ray luminosities are well above erg/s, in
some cases exceeding erg/s for a substantial amount of time. The
stars during these observations show no flares but are persistently bright. The
spectra can be well fit with two temperature plasma components of 10 MK and 40
MK, of which the latter dominates the flux by a ratio 6:1 on average. The total
EMs range between 3 - 8 cm and are comparable to active
coronal sources. Limits on the forbidden to inter-combination line ratios in
the He-Like K-shell lines show that we observe a predominantely optically thin
plasma with electron densities below cm. Observed abundances
compare well with active coronal sources underlying the coronal nature of these
sources. The surface flux in this sample of 0.6 to 2.3 Msun classical T Tauri
stars shows that coronal activity and possibly coronal loop size increase
significantly between ages 0.1 to 10 Myrs.Comment: 13 pages, 12 figures, submitted to the Astrophysical Journa
An uncorrelated state for the cortex?
The spike trains of nearby neurons in the sensory cortex are typically thought to be correlated due to mutual connections and common input. Multiple studies have measured these correlations and found them to be substantial (in the range of 10-40%). Two recent papers, however, reported that average correlations can be an order of magnitude smaller. Such low correlations could indicate an ‘uncorrelated state’ for the cortex, where cortical neurons act independently even in the face of strong common input
Evidence for Accretion in the High-resolution X-ray Spectrum of the T Tauri Star System Hen 3-600
We present high-resolution X-ray spectra of the multiple T Tauri star system
Hen 3-600, obtained with the High Energy Transmission Grating Spectrograph on
the Chandra X-ray Observatory. Two binary components were detected in the
zeroth-order image. Hen 3-600-A, which has a large mid-infrared excess, is a
2-3 times fainter in X-rays than Hen 3-600-B, due to a large flare on B. The
dispersed X-ray spectra of the two primary components overlap spatially;
spectral analysis was performed on the combined system. Analysis of the
individual spectra was limited to regions where the contributions of A and B
can be disentangled. This analysis results in two lines of evidence indicating
that the X-ray emission from Hen 3-600 is derived from accretion processes:
line ratios of O VII indicate that the characteristic density of its
X-ray-emitting plasma is large; a significant component of low-temperature
plasma is present and is stronger in component A. These results are consistent
with results obtained from X-ray gratings spectroscopy of more rapidly
accreting systems. All of the signatures of Hen 3-600 that are potential
diagnostics of accretion activity -- X-ray emission, UV excess, H-alpha
emission, and weak infrared excess -- suggest that its components represent a
transition phase between rapidly accreting, classical T Tauri stars and
non-accreting, weak-lined T Tauri stars.Comment: latex, 27 pages, 12 figures, 6 tables; accepted by Ap
The Coronal X-ray Spectrum of the Multiple Weak-Lined T Tauri Star System HD 98800
We present high-resolution X-ray spectra of the multiple (hierarchical
quadruple) weak-lined T Tauri star system HD 98800, obtained with the High
Energy Transmission Gratings Spectrograph (HETGS) aboard the Chandra X-ray
Observatory (CXO). In the zeroth-order CXO/HETGS X-ray image, both principle
binary components of HD 98800 (A and B, separation 0.8'') are detected;
component A was observed to flare during the observation. The infrared excess
(dust disk) component, HD 98800B, is a factor ~4 fainter in X-rays than the
apparently ``diskless'' HD 98800A, in quiescence. The line ratios of He-like
species (e.g., Ne IX, O VII) in the HD 98800A spectrum indicate that the
X-ray-emitting plasma around HD 98800 is in a typical coronal density regime
(log n <~ 11). We conclude that the dominant X-ray-emitting component(s) of HD
98800 is (are) coronally active. The sharp spectral differences between HD
98800 and the classical T Tauri star TW Hya demonstrate the potential utility
of high-resolution X-ray spectroscopy in providing diagnostics of pre-main
sequence accretion processes.Comment: 11 pages, 5 figures; to appear in the Astrophysical Journal (Letters
Evaluation of the CHUMS Child Bereavement Group : A Pilot Study Examining Statistical and Clinical Change
This is an Accepted Manuscript of an article published by Taylor & Francis in Death Studies on 7 February 2015, available online at: http://dx.doi.org/10.1080/07481187.2014.913085.This article describes the largest evaluation of a UK child bereavement service to date. Change was assessed using conventional statistical tests as well as clinical significance methodology. Consistent with the fact that the intervention was offered on a universal, preventative basis, bereaved young people experienced a statistically significant, small to medium-sized decrease in symptoms over time. This change was equivalent across child age and gender. Type of bereavement had a slight impact on change when rated by parents. Potential clinical implications are highlighted, and various limitations are discussed that we hope to address using an experimental design in future researchPeer reviewedFinal Accepted Versio
X-ray Emission and Corona of the Young Intermediate Mass Binary Ori E
Theta 1 Ori E is a young, moderate mass binary system, a rarely observed case
of spectral-type G-giants of about 3 Solar masses, which are still collapsing
towards the main sequence. We have obtained high resolution X-ray spectra with
Chandra and find that the system is very active and similar to coronal sources,
having emission typical of magnetically confined plasma: a broad temperature
distribution with a hot component and significant high energy continuum; narrow
emission lines from H- and He-like ions, as well as a range of Fe ions, and
relative luminosity, L_x/L_bol = 0.001. Density, while poorly constrained, is
consistent with the low density limits as determined from Mg XI and Ne IX
emission lines. Coronal elemental abundances are sub-Solar, with Ne being the
highest at about 0.4 times Solar. We find a possible trend in Trapezium hot
plasmas towards low relative abundances of Fe, O, and Ne, which is hard to
explain in terms of the dust depletion scenarios of low-mass young stars.
Variability was unusually low relative to other coronally active stars. The
emission is similar to post main-sequence G-stars. Coronal structures could be
compact or comparable to the dimensions of the stellar radii. We conclude that
the X-rays in theta 1 Ori E are generated by a convective dynamo.Comment: Accepted by ApJ (scheduled for Dec 2009, v707
Probing Wolf-Rayet Winds: Chandra/HETG X-Ray Spectra of WR 6
With a deep Chandra/HETGS exposure of WR 6, we have resolved emission lines
whose profiles show that the X-rays originate from a uniformly expanding
spherical wind of high X-ray-continuum optical depth. The presence of strong
helium-like forbidden lines places the source of X-ray emission at tens to
hundreds of stellar radii from the photosphere. Variability was present in
X-rays and simultaneous optical photometry, but neither were correlated with
the known period of the system or with each other. An enhanced abundance of
sodium revealed nuclear processed material, a quantity related to the
evolutionary state of the star. The characterization of the extent and nature
of the hot plasma in WR 6 will help to pave the way to a more fundamental
theoretical understanding of the winds and evolution of massive stars.Comment: Accepted by the Astrophysical Journa
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