3,330 research outputs found
High resolution imaging of NGC 2346 with GSAOI/GeMS: disentangling the planetary nebula molecular structure to understand its origin and evolution
We present high spatial resolution ( 60--90 milliarcseconds) images
of the molecular hydrogen emission in the Planetary Nebula (PN) NGC 2346. The
data were acquired during the System Verification of the Gemini Multi-Conjugate
Adaptive Optics System + Gemini South Adaptive Optics Imager. At the distance
of NGC 2346, 700 pc, the physical resolution corresponds to 56 AU,
which is slightly higher than that an [N II] image of NGC 2346 obtained with
HST/WFPC2. With this unprecedented resolution we were able to study in detail
the structure of the H gas within the nebula for the first time. We found
it to be composed of knots and filaments, which at lower resolution had
appeared to be a uniform torus of material. We explain how the formation of the
clumps and filaments in this PN is consistent with a mechanism in which a
central hot bubble of nebular gas surrounding the central star has been
depressurized, and the thermal pressure of the photoionized region drives the
fragmentation of the swept-up shell.Comment: accepted in ApJ (17 pages, 7 figures, 1 Table
A Morphological Diagnostic for Dynamical Evolution of Wolf-Rayet Bubbles
We have observed H-alpha and [OIII] emission from eight of the most well
defined Wolf-Rayet ring nebulae in the Galaxy. We find that in many cases the
outermost edge of the [OIII] emission leads the H-alpha emission. We suggest
that these offsets, when present, are due to the shock from the Wolf-Rayet
bubble expanding into the circumstellar envelope. Thus, the details of the WR
bubble morphology at H-alpha and [OIII] can then be used to better understand
the physical condition and evolutionary stage of the nebulae around Wolf-Rayet
stars, as well as place constraints on the nature of the stellar progenitor and
its mass loss history.Comment: 11 pages, LaTex, 8 figures, accepted for publication in AJ, November
200
Optical absorption of divalent metal tungstates: Correlation between the band-gap energy and the cation ionic radius
We have carried out optical-absorption and reflectance measurements at room
temperature in single crystals of AWO4 tungstates (A = Ba, Ca, Cd, Cu, Pb, Sr,
and Zn). From the experimental results their band-gap energy has been
determined to be 5.26 eV (BaWO4), 5.08 eV (SrWO4), 4.94 eV (CaWO4), 4.15 eV
(CdWO4), 3.9-4.4 eV (ZnWO4), 3.8-4.2 eV (PbWO4), and 2.3 eV (CuWO4). The
results are discussed in terms of the electronic structure of the studied
tungstates. It has been found that those compounds where only the s electron
states of the A2+ cation hybridize with the O 2p and W 5d states (e.g BaWO4)
have larger band-gap energies than those where also p, d, and f states of the
A2+ cation contribute to the top of the valence band and the bottom of the
conduction band (e.g. PbWO4). The results are of importance in view of the
large discrepancies existent in prevoiusly published data.Comment: 16 pages, 3 figures, 1 tabl
What Produced the Ultraluminous Supernova Remnant in NGC 6946?
The ultraluminous supernova remnant (SNR) in NGC 6946 is the brightest known
SNR in X-rays, ~1000 times brighter than Cas A. To probe the nature of this
remnant and its progenitor, we have obtained high-dispersion optical echelle
spectra. The echelle spectra detect H-alpha, [N II], and [O III] lines, and
resolve these lines into a narrow (FWHM ~20--40 km/s) component from un-shocked
material and a broad (FWHM ~250 km/s) component from shocked material. Both
narrow and broad components have unusually high [N II]/H-alpha ratios, ~1.
Using the echelle observation, archival HST images, and archival ROSAT X-ray
observations, we conclude that the SNR was produced by a normal supernova,
whose progenitor was a massive star, either a WN star or a luminous blue
variable. The high luminosity of the remnant is caused by the supernova ejecta
expanding into a dense, nitrogen-rich circumstellar nebula created by the
progenitor.Comment: 20 pages, 5 figures. To be published in The Astronomical Journal,
March 200
Echo Emission From Dust Scattering and X-Ray Afterglows of Gamma-Ray Bursts
We investigate the effect of X-ray echo emission in gamma-ray bursts (GRBs).
We find that the echo emission can provide an alternative way of understanding
X-ray shallow decays and jet breaks. In particular, a shallow decay followed by
a "normal" decay and a further rapid decay of X-ray afterglows can be together
explained as being due to the echo from prompt X-ray emission scattered by dust
grains in a massive wind bubble around a GRB progenitor. We also introduce an
extra temporal break in the X-ray echo emission. By fitting the afterglow light
curves, we can measure the locations of the massive wind bubbles, which will
bring us closer to finding the mass loss rate, wind velocity, and the age of
the progenitors prior to the GRB explosions.Comment: 25 pages, 3 figures, 2 tables. Accepted for publication in Ap
A Newtonian model for the WASP-148 exoplanetary system enhanced with TESS and ground-based photometric observations
The WASP-148 planetary system has a rare architecture with a transiting
Saturn-mass planet on a tight orbit which is accompanied by a slightly more
massive planet on a nearby outer orbit. Using new space-born photometry and
ground-based follow-up transit observations and data available in literature,
we performed modeling that accounts for gravitational interactions between both
planets. Thanks to the new transit timing data for planet b, uncertainties of
orbital periods and eccentricities for both planets were reduced relative to
previously published values by a factor of 3-4. Variation in transit timing has
an amplitude of about 20 minutes and can be easily followed-up with a 1-m class
telescopes from the ground. An approximated transit ephemeris, which accounts
for gravitational interactions with an accuracy up to 5 minutes, is provided.
No signature of transits was found for planet c down to the Neptune-size
regime. No other transiting companions were found down to a size of about 2.4
Earth radii for interior orbits. We notice, however, that the regime of
terrestrial-size planets still remains unexplored in that system.Comment: Accepted for publication in Acta Astronomic
Els Qüestionaris com a recurs docent en l'aprenentatge autònom. Resultats d'una prova pilot en un curs de Química bàsica.
En aquest article es presenten uns nous qüestionaris on line dissenyats per millorar la comprensió dels continguts de l"assignatura Química Bàsica II i, alhora, propiciar el treball autònom dels estudiants. En el grup pilot que ha disposat dels qüestionaris, els resultats acadèmics dels estudiants que els han realitzat diverses vegades han estat millors que els dels alumnes que no els han utilitzat amb regularitat. Els resultats acadèmics del grup pilot també ha estat millor que els de cursos anteriors
- …