bluuebunny/crossref_metadata_2025_split huggingface dataset:
Comparison of simulated powder snow avalanches with photogrammetric measurements
Authors: Dreier Lisa , Bühler Yves , Ginzler Christian , Bartelt Perry 
Published: March 2016

AbstractPhotogrammetric measurements of powder-cloud surfaces from large avalanches enable the observation of cloud evolution and dispersion as well as quantification of cloud velocities and powder volumes. Since 2002, a total of six large powder avalanches have been recorded at the test site, Vallée de la Sionne, Switzerland. The high-spatial-resolution photographs, acquired from two different observation angles, allow us to measure the velocity and height of plume-and-cleft structures on the powder-cloud surface. The photogrammetric measurements are supplemented by airborne laser scans of release, entrainment and deposition zones before and after the artificial avalanche release. Even though the precision of the photogrammetric measurements is limited, they are the best data available to test models of powder snow avalanche dynamics. The laser scan data capture initial and boundary conditions while time series of photogrammetric measurements provide insight into mechanisms driving blow-out formation and inertial propagation of the cloud. In this paper we present the experimental measurements and make direct comparisons with model simulations.
Meteorological conditions, seasonal and annual mass balances of Chhota Shigri Glacier, western Himalaya, India
Authors: Azam Mohd Farooq , Ramanathan AL. , Wagnon P. , Vincent C. , Linda A. , Berthier E. , Sharma P. , Mandal A. , Angchuk T. , Singh V.B. , Pottakkal J.G. 
Published: March 2016

AbstractWe present the updated glaciological mass balance (MB) of Chhota Shigri Glacier, the longest continuous annual MB record in the Hindu-Kush Karakoram Himalaya (HKH) region. Additionally, 4 years of seasonal MBs are presented and analyzed using the data acquired at an automatic weather station (AWS-M) installed in 2009 on a lateral moraine (4863ma.s.l.). The glaciological MB series since 2002 is first recalculated using an updated glacier hypsometry and then validated against geodetic MB derived from satellite stereo-imagery between 2005 (SPOT5) and 2014 (Pléiades). Chhota Shigri Glacier lost mass between 2002 and 2014 with a cumulative glaciological MB of –6.72mw.e. corresponding to a mean annual glacier-wide MB (Ba) of –0.56mw.e. a–1. Equilibrium-line altitude (ELA0) for the steady-state condition is calculated as ~4950ma.s.l., corresponding to an accumulation–area ratio (AAR0) of ~61%. Analysis of seasonal MBs between 2009 and 2013 with air temperature from AWS-M and precipitation from the nearest meteorological station at Bhuntar (1050ma.s.l.) suggests that the summer monsoon is the key season driving the interannual variability of Ba for this glacier. The intensity of summer snowfall events controls the Ba evolution via controlling summer glacier-wide MB (Bs).
TYPE II SUPERNOVA ENERGETICS AND COMPARISON OF LIGHT CURVES TO SHOCK-COOLING MODELS
Authors: Rubin Adam , Gal-Yam Avishay , De Cia Annalisa , Horesh Assaf , Khazov Danny , Ofek Eran O. , Kulkarni S. R. , Arcavi Iair , Manulis Ilan , Yaron Ofer , Vreeswijk Paul , Kasliwal Mansi M. , Ben-Ami Sagi , Perley Daniel A. , Cao Yi , Cenko S. Bradley , Rebbapragada Umaa D. , Woźniak P. R. , Filippenko Alexei V. , Clubb K. I. , Nugent Peter E. , Pan Y.-C. , Badenes C. , Howell D. Andrew , Valenti Stefano , Sand David , Sollerman J. , Johansson Joel , Leonard Douglas C. , Horst J. Chuck , Armen Stephen F. , Fedrow Joseph M. , Quimby Robert M. , Mazzali Paulo , Pian Elena , Sternberg Assaf , Matheson Thomas , Sullivan M. , Maguire K. , Lazarevic Sanja 
Published: March 2016

ABSTRACT
During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band SN II light curves that are well-monitored during their rise, with

detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1–3 days. We show that the energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the 2011 model of Rabinak & Waxman, while the progenitor radius cannot be determined based on R-band data alone. We find that SN II explosion energies span a range of E/M = (0.2–20) × 1051 erg/(10

), and have a mean energy per unit mass of

erg/(10

), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of 56Ni produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the decline rate (

), the decline rate is weakly correlated with the rise time, and the rise time is not significantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events.
EN ROUTE TO DESTRUCTION: THE EVOLUTION IN COMPOSITION OF ICES IN COMET D/2012 S1 (ISON) BETWEEN 1.2 AND 0.34 AU FROM THE SUN AS REVEALED AT INFRARED WAVELENGTHS*
Authors: DiSanti M. A. , Bonev B. P. , Gibb E. L. , Paganini L. , Villanueva G. L. , Mumma M. J. , Keane J. V. , Blake G. A. , Russo N. Dello , Meech K. J. , Vervack R. J. , McKay A. J. 
Published: March 2016

ABSTRACT
We report production rates for H2O and eight trace molecules (CO, C2H6, CH4, CH3OH, NH3, H2CO, HCN, C2H2) in the dynamically new, Sun-grazing Comet C/2012 S1 (ISON), using high-resolution spectroscopy at Keck II and the NASA IRTF on 10 pre-perihelion dates encompassing heliocentric distances R
h = 1.21–0.34 AU. Measured water production rates spanned two orders of magnitude, consistent with a long-term heliocentric power law Q(H2O)

. Abundance ratios for CO, C2H6, and CH4 with respect to H2O remained constant with R
h and below their corresponding mean values measured among a dominant sample of Oort Cloud comets. CH3OH was also depleted for R
h > 0.5 AU, but was closer to its mean value for R
h ≤ 0.5 AU. The remaining four molecules exhibited higher abundance ratios within 0.5 AU: for R
h > 0.8 AU, NH3 and C2H2 were consistent with their mean values while H2CO and HCN were depleted. For R
h < 0.5 AU, all four were enriched, with NH3, H2CO, and HCN increasing most. Spatial profiles of gas emission in ISON consistently peaked sunward of the dust continuum, which was asymmetric antisunward and remained singly peaked for all observations. NH3 within 0.5 AU showed a broad spatial distribution, possibly indicating its release in the coma provided that optical depth effects were unimportant. The column abundance ratio NH2/H2O at 0.83 AU was close to the “typical” NH/OH from optical wavelengths, but was higher within 0.5 AU. Establishing its production rate and testing its parentage (e.g., NH3) require modeling of coma outflow.
THE SOLAR INTERNETWORK. II. FLUX APPEARANCE AND DISAPPEARANCE RATES
Authors: Gošić M. , Rubio L. R. Bellot , Iniesta J. C. del Toro , Suárez D. Orozco , Katsukawa Y. 
Published: March 2016

ABSTRACT
Small-scale internetwork magnetic fields are important ingredients of the quiet Sun. In this paper we analyze how they appear and disappear on the solar surface. Using high resolution Hinode magnetograms, we follow the evolution of individual magnetic elements in the interior of two supergranular cells at the disk center. From up to 38 hr of continuous measurements, we show that magnetic flux appears in internetwork regions at a rate of 120 ± 3 Mx cm−2 day−1 (3.7 ± 0.4 × 1024 Mx day−1 over the entire solar surface). Flux disappears from the internetwork at a rate of 125 ± 6 Mx cm−2 day−1 (3.9 ± 0.5 × 1024 Mx day−1) through fading of magnetic elements, cancelation between opposite-polarity features, and interactions with network patches, which converts internetwork elements into network features. Most of the flux is lost through fading and interactions with the network, at nearly the same rate of about 50 Mx cm−2 day−1. Our results demonstrate that the sources and sinks of internetwork magnetic flux are well balanced. Using the instantaneous flux appearance and disappearance rates, we successfully reproduce the time evolution of the total unsigned flux in the two supergranular cells.
LIFETIMES AND ACCRETION RATES OF PROTOPLANETARY DISKS
Authors: Li Min , Xiao Lin 
Published: March 2016

ABSTRACT
Protoplanetary disks originate in the collapse of molecular cloud cores. The formation and evolution of disks are influenced by the properties of molecular cloud cores. In this paper we investigate the dependence of disk lifetimes and accretion rates on cloud core properties. We find that the lifetime increases as the angular velocities and the mass of cloud cores increase and that the lifetime decreases as the core temperature increases. We have calculated the distribution of disk lifetimes and disk fractions with stellar age. Our calculations show that the lifetime is in the range of 1–15 Myr and that the typical lifetime is 1–3 Myr. There are a few disks with lifetimes greater than 10 Myr and

of the disks have lifetimes less than 1 Myr. We also fit the disk fraction by an exponential decay curve with characteristic time ∼3.7 Myr. Our results explain the observations of disk lifetimes. We also find that the accretion rate does not change significantly with ω and generally decreases with

. At the early evolution of the disks, the

relation is about

. Since the effects of the photoevaporation are weak at this stage, this relation is the consequence of the cloud core properties. At the late evolution of the disks, the

relation is about

. For low accretion rates at this stage, the

relation results from the effects of X-ray photoevaporation. The calculated

relations are consistent with the observations.
HIGH-CADENCE, HIGH-CONTRAST IMAGING FOR EXOPLANET MAPPING: OBSERVATIONS OF THE HR 8799 PLANETS WITH VLT/SPHERE SATELLITE-SPOT-CORRECTED RELATIVE PHOTOMETRY
Authors: Apai Dániel , Kasper Markus , Skemer Andrew , Hanson Jake R. , Lagrange Anne-Marie , Biller Beth A. , Bonnefoy Mickaël , Buenzli Esther , Vigan Arthur 
Published: March 2016

ABSTRACT
Time-resolved photometry is an important new probe of the physics of condensate clouds in extrasolar planets and brown dwarfs. Extreme adaptive optics systems can directly image planets, but precise brightness measurements are challenging. We present VLT/SPHERE high-contrast, time-resolved broad H-band near-infrared photometry for four exoplanets in the HR 8799 system, sampling changes from night to night over five nights with relatively short integrations. The photospheres of these four planets are often modeled by patchy clouds and may show large-amplitude rotational brightness modulations. Our observations provide high-quality images of the system. We present a detailed performance analysis of different data analysis approaches to accurately measure the relative brightnesses of the four exoplanets. We explore the information in satellite spots and demonstrate their use as a proxy for image quality. While the brightness variations of the satellite spots are strongly correlated, we also identify a second-order anti-correlation pattern between the different spots. Our study finds that KLIP reduction based on principal components analysis with satellite-spot-modulated artificial-planet-injection-based photometry leads to a significant (∼3×) gain in photometric accuracy over standard aperture-based photometry and reaches 0.1 mag per point accuracy for our data set, the signal-to-noise ratio of which is limited by small field rotation. Relative planet-to-planet photometry can be compared between nights, enabling observations spanning multiple nights to probe variability. Recent high-quality relative H-band photometry of the b–c planet pair agrees to about 1%.
MODELING GD-1 GAPS IN A MILKY WAY POTENTIAL
Authors: Carlberg R. G. 
Published: March 2016

ABSTRACT
The GD-1 star stream is currently the best available for identifying density fluctuations, “gaps,” along its length as a test of the LCDM prediction of large numbers of dark matter sub-halos orbiting in the halo. Density variations of some form are present, since the variance of the density along the stream is three times that expected from the empirically estimated variation in the filtered mean star counts. The density variations are characterized with filters that approximate the shape of sub-halo, gravitationally induced stream gaps. The filters locate gaps and measure their amplitude, leading to a measurement of the distribution of gap widths. To gain an understanding of the factors influencing the gap width distribution, a suite of collisionless n-body simulations for a GD-1-like orbit in a Milky-Way-like potential provides a dynamically realistic statistical prediction of the gap distribution. The simulations show that every location in the stream has been disturbed to some degree by a sub-halo. The small gaps found via the filtering are largely noise. Larger gaps, those longer than 1 kpc, or 10° for GD-1, are the source of the excess variance. The suite of stream simulations shows that sub-halos at the predicted inner halo abundance or possibly somewhat higher can produce the required large-scale density variations.
EVOLUTION OF THE PROTON VELOCITY DISTRIBUTION DUE TO STOCHASTIC HEATING IN THE NEAR-SUN SOLAR WIND
Authors: Klein Kristopher G. , Chandran Benjamin D. G. 
Published: March 2016

ABSTRACT
We investigate how the proton distribution function evolves when the protons undergo stochastic heating by strong, low-frequency, Alfvén-wave turbulence under the assumption that β is small. We apply our analysis to protons undergoing stochastic heating in the supersonic fast solar wind and obtain proton distributions at heliocentric distances ranging from 4 to 30 solar radii. We find that the proton distribution develops non-Gaussian structure with a flat core and steep tail. For

, the proton distribution is well approximated by a modified Moyal distribution. Comparisons with future measurements from Solar Probe Plus could be used to test whether stochastic heating is occurring in the solar-wind acceleration region.
DIFFICULTY IN THE FORMATION OF COUNTER-ORBITING HOT JUPITERS FROM NEAR-COPLANAR HIERARCHICAL TRIPLE SYSTEMS: A SUB-STELLAR PERTURBER
Authors: Xue Yuxin , Suto Yasushi 
Published: March 2016

ABSTRACT
Among 100 transiting planets with a measured projected spin–orbit angle λ, several systems are suggested to be counter-orbiting. While these cases may be due to the projection effect, the mechanism that produces a counter-orbiting planet has not been established. A promising scenario for counter-orbiting planets is the extreme eccentricity evolution in near-coplanar hierarchical triple systems with eccentric inner and outer orbits. We examine this scenario in detail by performing a series of systematic numerical simulations, and consider the possibility of forming hot Jupiters (HJs), especially a counter-orbiting one under this mechanism with a distant sub-stellar perturber. We incorporate quadrupole and octupole secular gravitational interaction between the two orbits, and also short-range forces (correction for general relativity, star and inner planetary tide, and rotational distortion) simultaneously. We find that most systems are tidally disrupted and that a small fraction of the surviving planets turn out to be prograde. The formation of counter-orbiting HJs in this scenario is possible only in a very restricted parameter region, and thus is very unlikely in practice.
EFFECT OF ADIABATIC FOCUSING ON THE DIFFUSION OF ENERGETIC CHARGED PARTICLES
Authors: Wang Yang , Qin Gang 
Published: March 2016

ABSTRACT
An approximate analytic description of a diffusion coefficient, including the effect of adiabatic focusing, has been developed. This description is formulated with the aid of stochastic differential equations and the steady perturbation solution of the Fokker–Plank transport equation. The analytical formula is based on three important assumptions. First, the pitch-angle diffusion coefficient is set to be separable from the spatial coordinate and the pitch-angle cosine. Second, the spatial dependence of the ratio between the mean-free path and focusing length is assumed to be weak. Third, the pitch-angle distribution relaxes quickly to a steady state. The new analytic formula could be applied to calculate the spatial diffusion coefficient in the interplanetary and interstellar space.
A MIXTURE EVOLUTION SCENARIO OF THE AGN RADIO LUMINOSITY FUNCTION
Authors: Yuan Zunli , Wang Jiancheng , Zhou Ming , Mao Jirong 
Published: March 2016

ABSTRACT
We propose a mixture evolution scenario to model the evolution of the radio luminosity function (RLF) of steep-spectrum AGNs (active galactic nuclei), based on a Bayesian method. In this scenario, the shape of the RLF is determined by both the density and luminosity evolution. Our models indicate that the density evolution is positive until a redshift of

, at which point it becomes negative, while the luminosity evolution is positive to a higher redshift (

for model B and

for model C), where it becomes negative. Our mixture evolution model works well, and the modeled RLFs are in good agreement with previous determinations. The mixture evolution scenario can naturally explain the luminosity-dependent evolution of the RLFs.
La résistance aux antifongiques : importance en médecine humaine et vétérinaire
Authors: Guillot Jacques , Dannaoui Éric 
Published: March 2016

Resistance to antifungal drugs : importance in human and veterinary medicine.
Infections caused by pathogenic fungi are a significant global problem : a situation exacerbated by the limited availability of antifungal options, especially in veterinary Medicine. Like other microorganisms, fungi exist in populations that are adaptable. Under the selection pressure by antifungal drugs, drug-sensitive fungal populations frequently evolve resistance. Antifungal drug resistance appears to essentially be due to point mutations in either drug targets or transcription factors. Phenotypic methods for identification of antifungal resistance should be considered as reliable procedures, and the determination of minimum inhibition concentrations (MIC) by reference techniques is the gold standard to detect resistant clinical isolates. This text reviews the present state of the detection of resistance in fungal pathogens (Malassezia pachydermatis, Cryptococcus spp. and
Aspergillus fumigatus) and its relevance to clinical practice in veterinary Medicine.
La visión checa del Nuevo mundo en los siglos XVI-XIX
Authors: Kašpar Oldřich 
Published: March 2016

El interés del hombre checo por el mundo hispanoamericano en general tiene raíces profundas, cuyos inicios remontan al primer decenio del siglo XVI. En el año 1506, en la ciudad de Pilsen, al oeste de Bohemia (hoy día conocida más bien por su famoso tipo de cerveza) el tipógrafo de origen eslovaco Mikulá{ Bakaláˇr [tˇetina publicó un tratado interesante Spis o nových zemích a o Novém svˇetˇe (Tratado sobre las nuevas tierras y el Nuevo Mundo ...), primera información sobre América en la lengua checa descubierta hasta ahora.1 El libro es una compilación de traducciones libres de diversas fuentes, cu- ya parte fundamental la constituye el famoso escrito de Americo Vespucio (1454–1512) Mundus Novus, en latín complementado con informaciones procedentes de la relación de Cristóbal Colón (1451–1506) sobre su primer viaje y otros textos menos conocidos.2Veamos, pues, aunque sea brevemente lo que el Tratado relata por ejemplo sobre el aspecto de los indios americanos, es decir, de los habitantes de las islas caribeñas
Production of peroxy nitrates in boreal biomass burning plumes over Canada during the BORTAS campaign
Authors: Busilacchio Marcella , Di Carlo Piero , Aruffo Eleonora , Biancofiore Fabio , Dari Salisburgo Cesare , Giammaria Franco , Bauguitte Stephane , Lee James , Moller Sarah , Hopkins James , Punjabi Shalini , Andrews Stephen , Lewis Alistair C. , Parrington Mark , Palmer Paul I. , Hyer Edward , Wolfe Glenn M. 
Published: March 2016

Abstract. The observations collected during the BOReal forest fires on Tropospheric oxidants over the Atlantic using Aircraft and Satellites (BORTAS) campaign in summer 2011 over Canada are analysed to study the impact of forest fire emissions on the formation of ozone (O3) and total peroxy nitrates ∑PNs, ∑ROONO2). The suite of measurements on board the BAe-146 aircraft, deployed in this campaign, allows us to calculate the production of O3 and of  ∑PNs, a long-lived NOx reservoir whose concentration is supposed to be impacted by biomass burning emissions. In fire plumes, profiles of carbon monoxide (CO), which is a well-established tracer of pyrogenic emission, show concentration enhancements that are in strong correspondence with a significant increase of concentrations of ∑PNs, whereas minimal increase of the concentrations of O3 and NO2 is observed. The ∑PN and O3 productions have been calculated using the rate constants of the first- and second-order reactions of volatile organic compound (VOC) oxidation. The ∑PN and O3 productions have also been quantified by 0-D model simulation based on the Master Chemical Mechanism. Both methods show that in fire plumes the average production of ∑PNs and O3 are greater than in the background plumes, but the increase of ∑PN production is more pronounced than the O3 production. The average ∑PN production in fire plumes is from 7 to 12 times greater than in the background, whereas the average O3 production in fire plumes is from 2 to 5 times greater than in the background. These results suggest that, at least for boreal forest fires and for the measurements recorded during the BORTAS campaign, fire emissions impact both the oxidized NOy and O3,  but (1 ∑PN production is amplified significantly more than O3 production and (2) in the forest fire plumes the ratio between the O3 production and the ∑PN production is lower than the ratio evaluated in the background air masses, thus confirming that the role played by the ∑PNs produced during biomass burning is significant in the O3 budget. The implication of these observations is that fire emissions in some cases, for example boreal forest fires and in the conditions reported here, may influence more long-lived precursors of O3 than short-lived pollutants, which in turn can be transported and eventually diluted in a wide area.