1,835 research outputs found
The Lieder of Mathilde von Kralik, newly discovered
Mathilde von Kralik (1857-1944) was a late 19th/ early 20th century composer from The Austrian Empire. Her extraordinary musical gifts enabled her to be accepted into the Vienna Conservatory; one of the first women to be so honored. She was in a class of 10 which included the Gustav Mahler and had Anton Bruckner as a teacher. She composed a large oeuvre of vocal, piano, instrumental and organ works including an opera, symphonies and oratorios. In her songs she had the ability to write a captivating melodic line and intricate accompaniment comparable to Mahler or Richard Strauss. Because of political events due to WWII, the dissolution of the Austrian Empire, the loss of the family possessions, titles, properties and her being a woman her music has all but disappeared.
I will be transcribing her music from hand written manuscripts to an electronic music notation software. The nine pieces that I will be focusing on are Abends (Evenings) Sonntag (Sunday) Mondennacht (Moon Night) and the two songs in Vier Lieder which are Liebe (Love) and Schiffe (Ships). The first two songs are from the Austrian National Library in Vienna, received with permission from her great nephew Rochus von Kralik. The Fünf Lieder were only recently received by Herr von Kralik along with the song Mondennacht from present day Czech Republic (where the family had lived). The songs are dedicated to Baroness Amalie Strummer von Tavarnok ( formerly Bohemia) who possessed the castle in Miroslav and was friends with Mathilde von Kralik. Mr. Vladimir Sobotka had inherited the music from his grandfather and sent it to Herr von Kralik. With this extraordinary circuit of happenstance I will transcribe this music for the 21st century in addition to a performance of the songs at SUNY Potsdam, The Crane School of Music
Simple Perturbatively Traversable Wormholes from Bulk Fermions
A new class of traversable wormholes was recently constructed which relies
only on local bulk dynamics rather than an explicit coupling between distinct
boundaries. Here we begin with a four-dimensional Weyl fermion field of any
mass propagating on a classical background defined by a
quotient of (rotating) BTZ . This setup allows one to compute
the fermion stress-energy tensor exactly. For appropriate boundary conditions
around a non-contractible curve, perturbative back-reaction at any renders
the associated wormhole traversable and suggests it can become eternally
traversable at the limit where the background becomes extremal. A key technical
step is the proper formulation of the method of images for fermions in curved
spacetime. We find the stress-energy of spinor fields to have important
kinematic differences from that of scalar fields, typically causing the sign of
the integrated null stress-energy (and thus in many cases the sign of the time
delay/advance) to vary around the throat of the wormhole. Similar effects may
arise for higher-spin fields.Comment: 30 pages, 5 figure
Energetic Consequences for a Northern, Range-Edge Lizard Population
Lizards at the northern, cool edge of their geographic range in the northern hemisphere should encounter environmental conditions that differ from those living near the core of their range. To better understand how modest climate differences affect lizard energetics, we compared daily feeding and metabolism rates of individual Sceloporus occidentalis in two populations during mid-summer. Chuckanut Beach (CB) was a cool, maritime climate in northern Washington State, and Sondino Ranch (SR) was a warmer, drier climate in southern, inland Washington. We found no difference between populations in daily energy expenditure (DEE), as calculated from doubly labeled water estimates. The CB population, however, had significantly higher prey availability and rate of daily energy intake (DEI) as estimated from fecal pellet masses. Consequently, CB lizards had higher size-adjusted body masses than lizards from SR. Within CB, during midsummer, DEE was similar to DEI. Within the SR population, DEE trended higher than DEI during midsummer, but was not significantly different. We found no population differences in lizard activity, active body temperature, or preferred body temperature. Hence, we infer the longer activity season for the SR population may compensate for the low food availability and high daily energy cost of midsummer. Moreover, for the CB population, we infer that cooler temperatures and higher food availability allow the lizards to compensate for the shorter activity. We also suggest the CB population may benefit from the predicted warmer temperatures associated with climate change given the similar activity-period body temperatures and DEE between these lizard populations assuming food availability is sufficient
The Copula: A Tool for Simulating Speckle Dynamics
Use of a copula for generating a sequence of correlated speckle patterns is introduced. The chief characteristic of this algorithm is that it generates a continuous speckle sequence with a specified evolution of the correlation and does so with just two arrays of random numbers. Thus, physically realistic temporally varying speckle patterns with proper first- and second-order statistics are easily realized. We illustrate use of the algorithm for generating sequences with prescribed Gaussian, exponential, and equal-interval correlations and demonstrate how correlation times can be specified independently. This approach to generating sequences of random realizations with prescribed correlations should prove useful in modeling such phenomena as dynamic light scatter, flow-dependent laser speckle contrast, and propagation of spatial coherence
Keck and VLT Observations of Super-damped Lyman-alpha Absorbers at z=2=2.5: Constraints on Chemical Compositions and Physical Conditions
We report Keck/ESI and VLT/UVES observations of three super-damped
Lyman-alpha quasar absorbers with H I column densities log N(HI) >= 21.7 at
redshifts z=2-2.5. All three absorbers show similar metallicities (-1.3 to -1.5
dex), and dust depletion of Fe, Ni, and Mn. Two of the absorbers show
supersolar [S/Zn] and [Si/Zn]. We combine our results with those for other DLAs
to examine trends between N(HI), metallicity, dust depletion. A larger fraction
of the super-DLAs lie close to or above the line [X/H]=20.59-log N(HI) in the
metallicity vs. N(HI) plot, compared to the less gas-rich DLAs, suggesting that
super-DLAs are more likely to be rich in molecules. Unfortunately, our data for
Q0230-0334 and Q0743+1421 do not cover H2 absorption lines. For Q1418+0718,
some H2 lines are covered, but not detected. CO is not detected in any of our
absorbers. For DLAs with log N(HI) < 21.7, we confirm strong correlation
between metallicity and Fe depletion, and find a correlation between
metallicity and Si depletion. For super-DLAs, these correlations are weaker or
absent. The absorbers toward Q0230-0334 and Q1418+0718 show potential
detections of weak Ly-alpha emission, implying star formation rates of about
1.6 and 0.7 solar masses per year, respectively (ignoring dust extinction).
Upper limits on the electron densities from C II*/C II or Si II*/Si II are low,
but are higher than the median values in less gas-rich DLAs. Finally, systems
with log N(HI) > 21.7 may have somewhat narrower velocity dispersions delta
v_90 than the less gas-rich DLAs, and may arise in cooler and/or less turbulent
gas.Comment: 57 pages, 15 figures. Accepted for publication in Ap
Magellan LDSS3 emission confirmation of galaxies hosting metal-rich Lyman-alpha absorption systems
Using the Low Dispersion Survey Spectrograph 3 at the Magellan II Clay
Telescope, we target {candidate absorption host galaxies} detected in deep
optical imaging {(reaching limiting apparent magnitudes of 23.0-26.5 in and filters) in the fields of three QSOs, each of which shows the
presence of high metallicity, high absorption systems in their
spectra (Q0826-2230: =0.9110, Q1323-0021: ,
Q1436-0051: ). We confirm three host galaxies {at
redshifts 0.7387, 0.7401, and 0.9286} for two of the Lyman- absorption
systems (one with two galaxies interacting). For these systems, we are able to
determine the star formation rates (SFRs); impact parameters (from previous
imaging detections); the velocity shift between the absorption and emission
redshifts; and, for one system, also the emission metallicity.} Based on
previous photometry, we find these galaxies have LL. The [O II]
SFRs for these galaxies are in the range M yr
{(uncorrected for dust)}, while the impact parameters lie in the range
kpc. {Despite the fact that we have confirmed galaxies at 50 kpc from the QSO,
no gradient in metallicity is indicated between the absorption metallicity
along the QSO line of sight and the emission line metallicity in the galaxies.}
We confirm the anti-correlation between impact parameter and from
the literature. We also report the emission redshift of five other galaxies:
three at , and two (LL) at not
corresponding to any known absorption systems.Comment: 14 pages, 7 figures, 4 tables, accepted to MNRA
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