bluuebunny/crossref_metadata_2025_split huggingface dataset:
XIII.—On the Solid and Liquid Particles in Clouds
Authors: Aitken John 
Published: January 2013

Towards the end of May of this year I made my third visit to the Rigi Kulm, for the purpose of continuing my observations on the amount of dust in the atmosphere and other meteorological phenomena. It was with a feeling of no little satisfaction that I found myself at that elevated situation during broken weather, and under conditions very different from any previously experienced by me. On this occasion I had come in the hope of finding opportunities for making some observations on the conditions existing in clouds, in addition to the usual dust observations, and had brought with me the small instrument for observing the water particles in a fog, described in a previous communication to this Society. As the weather continued to be variable during the week of my visit, I was fortunate enough to succeed in making a number of interesting observations on the water particles in clouds, and also of comparing the conditions in clouds at this elevated situation with those previously observed in fogs at a low level.Before giving the results of my observations on the water particles, it may be desirable to make a few remarks on the solid or dust particles. When making the ordinary dust observations this year, it was frequently noticed that, when surrounded by clouds, the number of particles varied greatly at short intervals of time.
VIII. Memoir relating to the Naval Tactics of the late John Clerk, Esq. of Eldin; being a Fragment of an intended Account of his Life
Authors: Playfair John 
Published: January 2013

The author of the Naval Tactics is one of those men who, by the force of their own genius, have carried great improvements into professions which were not properly their own. The history both of the sciences and of the arts furnishes several remarkable examples of a similar nature. Fermat the rival, sometimes the superior of Descartes, one of the most inventive mathematicians of a most inventive age, was by profession a lawyer, and had only devoted to science the time that could be spared from the duties of a counsellor or a judge: about fifty years earlier, also, his countryman Vieta had made a like digression from the same employment, and hardly with inferior success.Perrault, who, in the façade of the Louvre, has left behind him so splendid a monument of architectural skill and taste, was a physician, and not only practised, but wrote books on medicine. Dr Herschell too, who has made more astronomical discoveries than any individual of the present age, betook himself to the study of the heavens as a relaxation from professional pursuits.
XV. Description of a Vegetable Impression found in the Quarry of Craigleith
Authors: Allan Thomas 
Published: January 2013

I some time ago had the honour to present to the Royal Society, a specimen of a very singular fossil which had been found in the freestone quarry of Craigleith, near this city. It presented the appearance so commonly met with in the sandstone of the coal-formation,—an impression of what has always been considered as the bark of a vegetable connected with the Palm-tribe; but it differed from any thing I had ever before seen of the kind, by having circular marks ranged in a line along the surface, being apparently the impressions of flowers or fruit. As neither of these grow directly from the stem of any plant now known, except among the Cactus genus, this impression might have been referred to it, had not the regularity of distance between these supposed flowers, pointed out the improbability; and it consequently must be referred to some one, the prototype of which is no longer known.The size of the specimen, of which the annexed engraving is a very exact representation, is twenty-one inches in length, and about fourteen broad; the widest part of the impression measures four inches, and the diameter of the circles a little more than three.
Searching for Type Ia Supernovae in Globular Clusters
Authors: Voss Rasmus 
Published: January 2013

AbstractGlobular clusters are known to have enhanced populations of binaries with compact objects, owing to the dynamical interactions taking place in their dense stellar environments. Both the single degenerate and double degenerate Type Ia supernova progenitors are expected to be similarly enhanced with respect to the field, but the theoretical predictions are highly uncertain. Here we discuss an archival survey aimed at constraining the fraction of Type Ia supernovae that explode inside globular clusters.
Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs
Authors: Marigo Paola 
Published: January 2013

AbstractCombining recent mass determinations of Galactic CO white dwarfs and their progenitors with the latest evolutionary models for Asymptotic Giant Branch (AGB) stars, I review the initial-final mass relation (IFMR) of low- and intermediate-mass stars. In particular, I analyze the impact on the IFMR produced by a few critical processes characterizing the AGB phase, namely: the second and third dredge-up events, hot-bottom burning, and mass loss. Their dependence on metallicity and related theoretical uncertainties are briefly discussed.
A Single Degenerate Model for Ultra Super-Chandrasekhar Mass Progenitors of Type Ia Supernovae – Young and Low Metallicity Environments –
Authors: Hachisu Izumi , Kato Mariko , Saio Hideyuki , Nomoto Ken'ichi 
Published: January 2013

AbstractSome Type Ia supernovae (SNe Ia) are suggested to have progenitor white dwarfs (WDs) with mass of up to 2.4–2.8 M⊙, highly exceeding the Chandrasekhar mass limit. We present a new single degenerate (SD) model for SNe Ia progenitors, in which the WD mass can increase by accretion up to 2.3 (2.7) M⊙ from the initial value of 1.1 (1.2) M⊙. The results are consistent with high luminosity SNe Ia such as SN 2003fg, SN 2006gz, SN 2007if, and SN 2009dc. There are three characteristic mass ranges of exploding WDs. In an extreme massive case, differentially rotating WDs explode as a SNe Ia soon after the WD mass exceeds 2.4 M⊙ because of a secular instability at T/|W|~0.14. For a mid mass range of MWD=1.5–2.4 M⊙, which is supported by differential rotation, it takes some spinning-down time until carbon is ignited to induce an SN Ia explosion. For a lower mass range of MWD=1.38–1.5 M⊙, they can be supported by rigid rotation until the angular momentum is lost. We also suggest the ultra super-Chandrasekhar mass SNe Ia are born in young and low metallicity environments.
Swift Observations of Novae
Authors: Page K. L. 
Published: January 2013

AbstractThe rapid response capability of Swift, together with the daily planning of its observing schedule, make it an ideal mission for following novae in the X-ray and UV bands. A number of both classical and recurrent novae have been extensively monitored throughout their supersoft phase. We report findings from these observations, including the high-amplitude flux variation often seen at the start of the supersoft emission, the optical plateau sometimes seen for recurrent novae, the differing relationships between the X-ray and UV variability, and the turn-on and turn-off times of the supersoft emission for the Swift sample of novae.
Spectral Features of KT Eri in its Nebular Phase
Authors: Arai Akira , Isoggai Mizuki , Imamura Kazuyoshi , Ikeda Yuji , Arasaki Takayuki , Kitao Eiji , Taguchi Gaku 
Published: January 2013

AbstractNon-spherically symmetric distributions of ejected gas are often observed in classical nova remnants. However, it is unclear if these asymmetries could be produced from nova explosions. Spectra in the nebular phase can provide information on the kinematics of ejected materials. Classical nova KT Eri was discovered on November 2009. It is considered a candidate for a recurrent nova based on the high expansion velocity and rapid decline of its light curve. In order to investigate the velocity field of ejected gas in the system, we performed optical spectroscopic observations from 2010 September to 2010 December at Koyama Astronomical Observatory. We noticed the strong [O III] and He II lines in the spectra on September 1, which suggests that the nova had already entered the nebular phase. It is notable that the [O III] lines showed complex profiles with at least six peaks on September 1. Those features can be de-convolved into four velocity components (−2,000 km s−1, −1,000 km s−1, +700 km s−1, and +1,800 km s−1) of doublet [O III] λ4959 and λ5007.
High Resolution XMM-Newton Data of Nova Outbursts using Warm & Hot Absorber Models
Authors: Balman Ş. , Pekön Y. 
Published: January 2013

AbstractWe reanalyze a selection of the XMM-Newton RGS (Reflection Grating Spectrometer) data of two classical novae; V4743 Sgr and V2491 Cyg. The high resolution nova spectra in the X-ray wavelengths show existence of absorption features (e.g., blue shifted). Our main aim is to model the absorption components detected in the high resolution spectra independently from the assumed continuum model. We assume that there is complex absorption of interstellar, photospheric, and of collisionally and/or photoionized gas origin in the moving material along the line of sight from a nova wind or ejecta. In addition to deriving the absorption properties, we obtain CNO abundances of elements in the ejecta/nova wind.
Symbiotic Stars as Possible Progenitors of SNe Ia: Binary Parameters and Overall Outlook
Authors: Mikołajewska J. 
Published: January 2013

AbstractSymbiotic stars are interacting binaries in which the first-formed white dwarf accretes and burns material from a red giant companion. This paper aims at presenting physical characteristics of these objects and discussing their possible link with progenitors of Type Ia supernovae.
Hydrodynamic Studies of the Evolution of Recurrent Novae to Supernova Ia Explosions
Authors: Starrfield S. , Timmes F. X. , Hix W. R. , Iliadis C. , Arnett W. D. , Meakin C. , Sparks W. M. 
Published: January 2013

AbstractWe have begun new studies of the evolution of thermonuclear runaways (TNRs) in the accreted envelopes of white dwarfs (WDs). Here we focus on the recent outbursts of RS Oph (2006), U Sco (2010) and T Pyx (2011). U Sco explodes about every 10 years and the ejected material from the WD is helium rich. It has a short orbital period for recurrent novae (RNe) but the secondary is likely to be evolved. The WD is thought to be close in mass to the Chandrasekhar limit. T Pyx has just suffered its first outburst since 1966 and it was predicted to never experience another outburst. It has a short orbital period and has formed dust in the ejecta as this paper was being written. One important question is the secular evolution of the WD. Do the repeated outbursts cause the WD to gain or lose mass? If it is gaining mass, it could eventually reach the Chandrasekhar limit and become a Type Ia supernova (SNe Ia) if it can hide the hydrogen and helium in the system. Here, we report on our latest studies of TNRs in accreted envelopes on WDs using a variety of initial WD masses, luminosities, and mass accretion rates. Of great importance to our conclusions, we assume a solar composition (Lodders abundance distribution). We use our 1-D hydro code, NOVA, that includes the Hix and Thielemann nuclear reaction network, the Iliadis reaction rate library, the Timmes equation of state, OPAL opacities, and the new convection of Arnett, Meakin, and Young. We report on the amount of ejected mass, evolution time to explode, and whether or not the WD is growing or losing mass.
X-ray Grating Observations of Recent Recurrent Novae
Authors: Orio Marina , Behar Ehud , Gallagher J. , Bianchini A. , Chiosi E. , Luna J. , Nelson T. , Rauch T. 
Published: January 2013

AbstractTwo recurrent novae (RNe) that do not host red giants were observed in outburst at the beginning of 2009 and 2010, respectively. The first nova was LMC 2009a, and the second one was U Scorpii. Nova LMC 2009a was a relatively slow RN, and it was quite luminous both at optical and X-ray wavelengths. U Sco is the fastest nova ever recorded. Its supersoft X-ray phase started a couple of weeks after optical maximum and lasted for about a month, while for Nova LMC 2009a this phase started four months after maximum and lasted for 5 months. For both novae, the first X-ray spectrum taken while the luminous supersoft X-ray source was beginning to emerge is remarkably similar with broad and prominent emission lines of nitrogen and carbon accounting for at least 30% of the X-ray flux. Blue-shifted absorption and red-shifted emission form apparent P-Cyg profiles. We attribute the emission features to the ejecta and show evidence that they are largely due to collisional ionization. In the case of U Sco the absorption lines were embedded in the emission features after the first observation. We find evidence that in U Scorpii we were observing the Thomson reflected spectrum at a distance of ≃ 3 R⊙ from the white dwarf rather than the atmosphere itself. For both novae, the peak temperature was remarkably high, probably close to 900,000 K for U Sco, and about 600,000 K for Nova LMC 2009a. We suggest that these two objects represent different stages of RNe secular evolution.
The Asymmetric Outflow of RS Ophiuchi
Authors: Mohamed S. , Booth R. , Podsiadlowski Ph. 
Published: January 2013

AbstractRS Ophiuchi (RS Oph) is a symbiotic binary consisting of a hot white dwarf accreting from the slow, dense stellar wind of a cool, red giant companion. The system belongs to, and is one of the best studied examples of, an even smaller subclass of binaries known as recurrent novae in which the white dwarf undergoes repeated thermonuclear outbursts. We present 3D smoothed particle hydrodynamics (SPH) models of mass transfer from the red giant to the white dwarf, followed by a nova outburst. We show that the outflow in the former is strongly concentrated towards the binary orbital plane. The nova ejecta is thus constrained in the equatorial directions, resulting in a bipolar outflow. The white dwarf in RS Oph is thought to be close to the Chandrasekhar mass, making the system a likely Type Ia supernova candidate. We discuss the role that such a highly structured circumstellar medium will play in the evolution of the supernova remnant.
Changes in the Dusty Environment of the Recurrent Nova RS Ophiuchi
Authors: Rushton M. T. , Helton L. A. , Kaminsky B. , Woodward C. E. , Pavlenko Ya. V. , Evans A. 
Published: January 2013

AbstractWe present Spitzer spectroscopy of the recurrent nova RS Ophiuchi obtained on several occasions between 2006 and 2009. The spectra show variability in the silicate dust features at 9.7 μm and 18 μm, which form in the wind of the red giant in the system. We fit the spectra with Dusty models and find changes in the dust temperature, due to changes in the luminosity of the central source. The mass-loss rate of the secondary is a few 10−7M⊙yr−1, typical of a red giant of its type.
Modeling of the IR Light Curves of the Symbiotic Recurrent Nova T CrB
Authors: Tatarnikova A. A. , Tatarnikov A. M. , Shenavrin V. I. 
Published: January 2013

AbstractWe analyze the results of our IR photometric monitoring of T CrB during 1987-2003 and describe the ellipsoidal variability of the Roche lobe filling cool component. We obtain limits to the binary inclination of i ∈ [50,60] deg and binary mass ratio q ∈ [0.4,2] (90 per cent confidence). The mass of the hot component is therefore 1.3-3 M⊙. If the hot component of T CrB is a white dwarf, its mass will be near the Chandrasekhar limit.
Survey for the Binary Progenitor in SN1006 and Update on SN1572
Authors: Ruiz–Lapuente Pilar , Hernández Jonay González , Tabernero Hugo , Montes David , Canal Ramon , Mendez Javier , Bedin Luigi 
Published: January 2013

AbstractWe have completed a survey down to R = 15 mag of the stars within a circle of 4 arcmin radius around the nominal center of the remnant of SN 1006, one of the three historical Type Ia supernovae (the other two being SN 1572 and SN 1604), in search of a possible surviving binary companion of the white dwarf whose explosion gave rise to the supernova. The stellar parameters (effective temperature, surface gravity, and metallicity), as well as the radial velocities of all the stars, have been measured from spectra obtained with the UVES spectrograph at the VLT, and from the former and the available photometry, distances have been determined. Chemical abundances of the Fe-peak elements Cr, Mn, Co, and Ni have also been measured to check for possible contamination of the stellar surface by the supernova ejecta. The limiting magnitude of the survey would allow us to find stellar companions of the red-giant type, subgiant stars, and main–sequence stars down to F5–6. Unlike in SN 1572, where a subgiant of type G0–1 has been proposed as the companion of SN 1572, for SN 1006 we can discard the possibility that SN 1006 had a red giant or subgiant companion.
Light-Echo Spectrum Reveals the Type of Tycho Brahe's 1572 Supernova
Authors: Usuda T. , Krause O. , Tanaka M. , Hattori T. , Goto M. , Birkmann S. M. , Nomoto K. 
Published: January 2013

AbstractWe successfully obtained the first optical spectra of the faint light echoes around Cassiopeia A and Tycho Brahe's supernova remnants (SNRs) with FOCAS and the Subaru Telescope. We conclude that Cas A and Tycho's SN 1572 belong to the Type IIb and normal Type Ia supernovae, respectively. Light echo spectra are important in order to obtain further insight into the supernova explosion mechanism of Tycho's SN 1572: how the Type Ia explosion actually proceeds, and whether accretion occurs from a companion or by the merging of two white dwarfs. The proximity of the SN 1572 remnant has allowed detailed studies, such as the possible identification of the binary companion, and provides a unique opportunity to test theories of the explosion mechanism and the nature of the progenitor. Future light-echo spectra, obtained in different spatial directions of SN 1572, will enable to construct a three-dimensional spectroscopic view of the explosion.
A sclerite-bearing stem group entoproct from the early Cambrian and its implications
Authors: Zhang Zhifei , Holmer Lars E. , Skovsted Christian B. , Brock Glenn A. , Budd Graham E. , Fu Dongjing , Zhang Xingliang , Shu Degan , Han Jian , Liu Jianni , Wang Haizhou , Butler Aodhán , Li Guoxiang 
Published: January 2013

AbstractThe Lophotrochozoa includes disparate tentacle-bearing sessile protostome animals, which apparently appeared in the Cambrian explosion, but lack an uncontested fossil record. Here we describe abundant well preserved material of Cotyledion tylodes Luo et Hu, 1999, from the Cambrian (Series 2) Chengjiang deposits, reinterpreted here as a stem-group entoproct. The entoproct affinity is supported by the sessile body plan and interior soft anatomy. The body consists of an upper calyx and a lower elongate stalk with a distal holdfast. The soft anatomy includes a U-shaped gut with a mouth and aboral anus ringed by retractable marginal tentacles. Cotyledion differs from extant entoprocts in being larger and having the calyx and the stalk covered by numerous loosely-spaced external sclerites. The description of entoprocts from the Chengjiang biota traces the ancestry of yet another lophotrochozoan phylum back to the Cambrian radiation and has important implications for the earliest evolution of lophotrochozoans.
1180 nm VECSEL with output power beyond 20 W
Authors: Ranta S. , Tavast M. , Leinonen T. , Van Lieu N. , Fetzer G. , Guina M. 
Published: January 2013

The highest power result for an optically‐pumped single‐chip vertical external‐cavity surface‐emitting laser with emission near 1180 nm is reported. The gain mirror was grown by molecular beam epitaxy and incorporated a strain compensated GaInAs/GaAs/GaAsP active region. An intra‐cavity diamond heat spreader was attached to the gain mirror for thermal management. In free‐running operation, the laser emitted more than 20 W at a mount temperature of about 12 °C. The output spectrum was centred between 1165–1190 nm depending on the mount temperature and pump power. By using an intra‐cavity birefringent filter, the full width at half‐maximum linewidth could be narrowed to ≤1 nm and at the same time achieved approximately 14 W of output power near 1178 nm. Moreover, the lasing wavelength could be tuned over more than 40 nm.
Wide stopband substrate integrated waveguide filter using corner cavities
Authors: Zhu F. , Hong W. , Chen J.X. , Wu K. 
Published: January 2013

A type of substrate integrated waveguide (SIW) ‘corner cavity’ is proposed. For each corner cavity, two transmission zeros (TZs) can be introduced and the location of either TZ can easily be controlled by adjusting suitable geometrical parameters. Using the corner cavities, a novel SIW filter with wide stopband characteristic is implemented. The central frequency of the filter is 20 GHz, and the first spurious appears at about 40 GHz, which is two times the central frequency. In addition, the measured stopband attenuation of the filter is better than 50 dB from 21.24 to 37.71 GHz.
High‐power‐tolerant InAlAs avalanche photodiode for 25 Gbit/s applications
Authors: Nada M. , Muramoto Y. , Yokoyama H. , Ishibashi T. , Matsuzaki H. 
Published: January 2013

A wide optical‐input dynamic range is demonstrated for an inverted p‐down InAlAs/InGaAs avalanche photodiode. The 3 dB down bandwidth maintains a value as high as 18 GHz for an input optical power level of up to + 2.5 dBm. Such high‐power tolerance meets the requirements of various future optical fibre communications systems such as 100 Gbit/s Ethernet which has a serial baud rate of 25 Gbit/s.
Multiple Dimensions of Spirituality in Recovery: A Lagged Mediational Analysis of Alcoholics Anonymous’ Principal Theoretical Mechanism of Behavior Change
Authors: Krentzman Amy R. , Cranford James A. , Robinson Elizabeth A. R. 
Published: January 2013

Alcoholics Anonymous (AA) states that recovery is possible through spiritual experiences and spiritual awakenings. Research examining spirituality as a mediator of AA's effect on drinking has been mixed. It is unknown whether such findings are due to variations in the operationalization of key constructs, such as AA and spirituality. To answer these questions, the authors used a longitudinal model to test 2 dimensions of AA as focal predictors and 6 dimensions of spirituality as possible mediators of AA's association with drinking. Data from the first 18 months of a 3-year longitudinal study of 364 alcohol-dependent individuals were analyzed. Structural equation modeling was used to replicate the analyses of Kelly et al. ( Alcohol Clin Exp Res. 2011;35:454–463) and to compare AA attendance and AA involvement as focal predictors. Multiple regression analyses were used to determine which spirituality dimensions changed as the result of AA participation. A trimmed, data-driven model was employed to test multiple mediation paths simultaneously. The findings of the Kelly et al. study were replicated. AA involvement was a stronger predictor of drinking outcomes than AA attendance. AA involvement predicted increases in private religious practices, daily spiritual experiences, and forgiveness of others. However, only private religious practices mediated the relationship between AA and drinking.