763 research outputs found
Adaptive BDDC in Three Dimensions
The adaptive BDDC method is extended to the selection of face constraints in
three dimensions. A new implementation of the BDDC method is presented based on
a global formulation without an explicit coarse problem, with massive
parallelism provided by a multifrontal solver. Constraints are implemented by a
projection and sparsity of the projected operator is preserved by a generalized
change of variables. The effectiveness of the method is illustrated on several
engineering problems.Comment: 28 pages, 9 figures, 9 table
Global surfaces of section in the planar restricted 3-body problem
The restricted planar three-body problem has a rich history, yet many
unanswered questions still remain. In the present paper we prove the existence
of a global surface of section near the smaller body in a new range of energies
and mass ratios for which the Hill's region still has three connected
components. The approach relies on recent global methods in symplectic geometry
and contrasts sharply with the perturbative methods used until now.Comment: 11 pages, 1 figur
Herschel observations of interstellar chloronium
Using the Herschel Space Observatory's Heterodyne Instrument for the
Far-Infrared (HIFI), we have observed para-chloronium (H2Cl+) toward six
sources in the Galaxy. We detected interstellar chloronium absorption in
foreground molecular clouds along the sight-lines to the bright submillimeter
continuum sources Sgr A (+50 km/s cloud) and W31C. Both the para-H2-35Cl+ and
para-H2-37Cl+ isotopologues were detected, through observations of their
1(11)-0(00) transitions at rest frequencies of 485.42 and 484.23 GHz,
respectively. For an assumed ortho-to-para ratio of 3, the observed optical
depths imply that chloronium accounts for ~ 4 - 12% of chlorine nuclei in the
gas phase. We detected interstellar chloronium emission from two sources in the
Orion Molecular Cloud 1: the Orion Bar photodissociation region and the Orion
South condensation. For an assumed ortho-to-para ratio of 3 for chloronium, the
observed emission line fluxes imply total beam-averaged column densities of ~
2.0E+13 cm-2 and ~ 1.2E+13 cm-2, respectively, for chloronium in these two
sources. We obtained upper limits on the para-H2-35Cl+ line strengths toward H2
Peak 1 in the Orion Molecular cloud and toward the massive young star AFGL
2591. The chloronium abundances inferred in this study are typically at least a
factor ~10 larger than the predictions of steady-state theoretical models for
the chemistry of interstellar molecules containing chlorine. Several
explanations for this discrepancy were investigated, but none has proven
satisfactory, and thus the large observed abundances of chloronium remain
puzzling.Comment: Accepted for publication in the Astrophysical Journa
Alien Registration- Parent, Joseph B. (Van Buren, Aroostook County)
https://digitalmaine.com/alien_docs/32354/thumbnail.jp
Observations of the 6 Centimeter Lines of OH in Evolved (OH/IR) Stars
Recent observational and theoretical advances have called into question
traditional OH maser pumping models in evolved (OH/IR) stars. The detection of
excited-state OH lines would provide additional constraints to discriminate
amongst these theoretical models. In this Letter, we report on VLA observations
of the 4750 MHz and 4765 MHz lines of OH toward 45 sources, mostly evolved
stars. We detect 4765 MHz emission in the star forming regions Mon R2 and LDN
1084, but we do not detect excited-state emission in any evolved stars. The
flux density and velocity of the 4765 MHz detection in Mon R2 suggests that a
new flaring event has begun.Comment: 4 pages, to appear in ApJ
Molecular absorption lines toward star-forming regions : a comparative study of HCO+, HNC, HCN, and CN
Aims. The comparative study of several molecular species at the origin of the
gas phase chemistry in the diffuse interstellar medium (ISM) is a key input in
unraveling the coupled chemical and dynamical evolution of the ISM. Methods.
The lowest rotational lines of HCO+, HCN, HNC, and CN were observed at the
IRAM-30m telescope in absorption against the \lambda 3 mm and \lambda 1.3 mm
continuum emission of massive star-forming regions in the Galactic plane. The
absorption lines probe the gas over kiloparsecs along these lines of sight. The
excitation temperatures of HCO+ are inferred from the comparison of the
absorptions in the two lowest transitions. The spectra of all molecular species
on the same line of sight are decomposed into Gaussian velocity components.
Most appear in all the spectra of a given line of sight. For each component, we
derived the central opacity, the velocity dispersion, and computed the
molecular column density. We compared our results to the predictions of
UV-dominated chemical models of photodissociation regions (PDR models) and to
those of non-equilibrium models in which the chemistry is driven by the
dissipation of turbulent energy (TDR models). Results. The molecular column
densities of all the velocity components span up to two orders of magnitude.
Those of CN, HCN, and HNC are linearly correlated with each other with mean
ratios N(HCN)/N(HNC) = 4.8 1.3 and N(CN)/N(HNC) = 34 12, and more
loosely correlated with those of HCO+, N(HNC)/N(HCO+) = 0.5 0.3,
N(HCN)/N(HCO+) = 1.9 0.9, and N(CN)/N(HCO+) = 18 9. These ratios
are similar to those inferred from observations of high Galactic latitude lines
of sight, suggesting that the gas sampled by absorption lines in the Galactic
plane has the same chemical properties as that in the Solar neighbourhood. The
FWHM of the Gaussian velocity components span the range 0.3 to 3 km s-1 and
those of the HCO+ lines are found to be 30% broader than those of CN-bearing
molecules. The PDR models fail to reproduce simultaneously the observed
abundances of the CN-bearing species and HCO+, even for high-density material
(100 cm-3 < nH < 104 cm-3). The TDR models, in turn, are able to reproduce the
observed abundances and abundance ratios of all the analysed molecules for the
moderate gas densities (30 cm-3 < nH < 200 cm-3) and the turbulent energy
observed in the diffuse interstellar medium. Conclusions. Intermittent
turbulent dissipation appears to be a promising driver of the gas phase
chemistry of the diffuse and translucent gas throughout the Galaxy. The details
of the dissipation mechanisms still need to be investigated
Interactive narration with a child: impact of prosody and facial expressions
International audienceIntelligent Virtual Agents are suitable means for interactive sto-rytelling for children. The engagement level of child interaction with virtual agents is a challenging issue in this area. However, the characteristics of child-agent interaction received moderate to little attention in scientific studies whereas such knowledge may be crucial to design specific applications. This article proposes a Wizard of Oz platform for interactive narration. An experimental study in the context of interactive story-telling exploiting this platform is presented to evaluate the impact of agent prosody and facial expressions on child participation during storytelling. The results show that the use of the virtual agent with prosody and facial expression modalities improves the engagement of children in interaction during the narrative sessions
Herschel/HIFI observations of interstellar OH+ and H2O+ towards W49N: a probe of diffuse clouds with a small molecular fraction
We report the detection of absorption by interstellar hydroxyl cations and
water cations, along the sight-line to the bright continuum source W49N. We
have used Herschel's HIFI instrument, in dual beam switch mode, to observe the
972 GHz N = 1 - 0 transition of OH+ and the 1115 GHz 1(11) - 0(00) transition
of ortho-H2O+. The resultant spectra show absorption by ortho-H2O+, and strong
absorption by OH+, in foreground material at velocities in the range 0 to 70
km/s with respect to the local standard of rest. The inferred OH+/H2O+
abundance ratio ranges from ~ 3 to ~ 15, implying that the observed OH+ arises
in clouds of small molecular fraction, in the 2 - 8% range. This conclusion is
confirmed by the distribution of OH+ and H2O+ in Doppler velocity space, which
is similar to that of atomic hydrogen, as observed by means of 21 cm absorption
measurements, and dissimilar from that typical of other molecular tracers. The
observed OH+/H abundance ratio of a few E-8 suggests a cosmic ray ionization
rate for atomic hydrogen of (0.6 - 2.4) E-16 s-1, in good agreement with
estimates inferred previously for diffuse clouds in the Galactic disk from
observations of interstellar H3+ and other species.Comment: Accepted for publication in A&A Letter
The telencephalon of the bat. I. The non-cortical nuclear masses and certain pertinent fiber connections
No Abstract.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/49917/1/900650115_ftp.pd
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The cultural currency of a 'good' sense of humour: British comedy and new forms of distinction
Traditionally considered lowbrow art par excellence, British comedy has grown steadily in legitimacy since the âAlternative Comedy Movementâ of the early 1980s. Yet while there might be evidence of a transformation in British comic production, there is little understanding of how this has been reflected in patterns of consumption. Indeed, there is a remarkable absence of studies probing comedy taste in British cultural sociology, most notably in Bennett et alâs (2009) recent and otherwise exhaustive mapping of cultural taste and participation. This paper aims to plug this gap in the literature by examining contemporary comedy taste cultures in Britain. Drawing on a large-scale survey and in-depth interviews carried out at the Edinburgh Festival Fringe, it argues that comedy now represents an emerging field for the culturally privileged to activate their cultural capital resources. However, unlike previous studies on cultural capital and taste, this research finds that field-specific âcomic cultural capitalâ is mobilised less through taste for certain legitimate âobjectsâ of comedy and more through the expression of rarefied and somewhat âdisinterestedâ styles of comic appreciation. In short, it is âembodiedâ rather than âobjectifiedâ forms of cultural capital that largely distinguish the privileged in the field of comedy
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