bluuebunny/crossref_metadata_2025_split huggingface dataset:
Ice Condensation as a Planet Formation Mechanism
Authors: Ros Katrin 
Published: January 2014

AbstractParticles in protoplanetary discs grow rapidly to millimetre-sizes via coagulation, but further growth to centimetre-sized pebbles is not yet completely understood. We investigate particle growth by ice condensation in a model where we take the dynamical behaviour of vapour and ice particles into account, as well as the size evolution due to condensation and sublimation. Our results show that efficient growth from dust to pebbles is possible close to the water ice line at ~3 AU, with particles growing from millimetres to decimetres on a time scale of 10000 yr.
The Influence of Alfvén Ionization on Exoplanetary Atmospheres
Authors: Stark Craig R. , Helling Christiane , Diver Declan A. 
Published: January 2014

AbstractObservations of radio emission from exoplanets and brown dwarfs suggest that such objects harbour atmospheric magnetized plasmas. However, the degree of thermal ionization for such substellar objects is insufficient to qualify the ionized component as a plasma, posing the question: what ionization processes can efficiently produce the required plasma? We propose Alfvén ionization as a mechanism for producing localized pockets of ionized gas in the atmosphere, having sufficient degrees of ionization (≥10−7) that they constitute plasmas. We outline the criteria required for Alfvén ionization to occur and justify its applicability in substellar atmospheres. For the model atmospheres considered here, our results show that degrees of ionization ranging from 10−6−1 can be obtained.
Constraining Planetary Migration Mechanisms in Systems of Giant Planets
Authors: Dawson Rebekah I. , Murray-Clay Ruth A. , Johnson John Asher 
Published: January 2014

AbstractIt was once widely believed that planets formed peacefully in situ in their proto-planetary disks and subsequently remain in place. Instead, growing evidence suggests that many giant planets undergo dynamical rearrangement that results in planets migrating inward in the disk, far from their birthplaces. However, it remains debated whether this migration is caused by smooth planet-disk interactions or violent multi-body interactions. Both classes of model can produce Jupiter-mass planets orbiting within 0.1 AU of their host stars, also known as hot Jupiters. In the latter class of model, another planet or star in the system perturbs the Jupiter onto a highly eccentric orbit, which tidal dissipation subsequently shrinks and circularizes during close passages to the star. We assess the prevalence of smooth vs. violent migration through two studies. First, motivated by the predictions of Socrates et al. (2012), we search for super-eccentric hot Jupiter progenitors by using the “photoeccentric effect” to measure the eccentricities of Kepler giant planet candidates from their transit light curves. We find a significant lack of super- eccentric proto-hot Jupiters compared to the number expected, allowing us to place an upper limit on the fraction of hot Jupiters created by stellar binaries. Second, if both planet-disk and multi-body interactions commonly cause giant planet migration, physical properties of the proto-planetary environment may determine which is triggered. We identify three trends in which giant planets orbiting metal rich stars show signatures of planet-planet interactions: (1) gas giants orbiting within 1 AU of metal-rich stars have a range of eccentricities, whereas those orbiting metal- poor stars are restricted to lower eccentricities; (2) metal-rich stars host most eccentric proto-hot Jupiters undergoing tidal circularization; and (3) the pile-up of short-period giant planets, missing in the Kepler sample, is a feature of metal-rich stars and is largely recovered for giants orbiting metal-rich Kepler host stars. These two studies suggest that both disk migration and planet-planet interactions may be widespread, with the latter occurring primarily in metal-rich planetary systems where multiple giant planets can form. Funded by NSF-GRFP DGE-1144152.
Determination of Temperature in Solar Prominences/Filaments Using FISS Observations
Authors: Chae Jongchul , Park Hyungmin , Song Donguk 
Published: January 2014

AbstractUsing the Fast Imaging Solar Spectrograph of the 1.6 meter New Solar Telescope at Big Bear, we simultaneously took the spectral profiles of the Hα line and the Ca ii line at 854.2 nm from prominences beyond the solar limb and filaments on the disk. The spectral data were fitted by the slab model of radiative transfer with constant source function, either with zero background intensity profile (in prominences) or with carefully constructed background intensity profile (in filaments). These observations with different perspectives and different analyses produced consistent results: temperature inside prominences/filaments ranges from 4000 to 20000 K with a mean of about 9500 K. We expect that this kind of observation and analysis with higher spatial resolution and higher temporal resolution will allow us to study in detail the thermal structure and evolution of plasma in prominences.
A first look into the magnetic field configuration of prominence threads using spectropolarimetric data
Authors: Suárez D. Orozco , Ramos A. Asensio , Bueno J. Trujillo 
Published: January 2014

AbstractWe show preliminary results of an ongoing investigation aimed at determining the configuration of the magnetic field vector in the threads of a quiescent hedgerow solar prominence using high-spatial resolution spectropolarimetric observations taken in the He I 1083.0 nm multiplet. The data consist of a two-dimensional map of a quiescent hedgerow prominence showing vertical threads. The observations were obtained with the Tenerife Infrared Polarimeter attached to the German Vacuum Tower Telescope at the Observatorio del Teide (Spain). The He I 1083.0 nm Stokes signals are interpreted with an inversion code, which takes into account the key physical processes that generate and/or modify circular and linear polarization signals in the He I 1083.0 nm triplet: the Zeeman effect, anisotropic radiation pumping, and the Hanle effect. We present initial results of the inversions, i.e, the strength and orientation of the magnetic field vector along the prominence and in prominence threads.
Primary observations of solar filaments using the multi-channel imaging system of the New Vacuum Solar Telescope
Authors: Xu Zhi , Jin Zhen Y. , Xu Fang Y. , Liu Zhong ,   the NVST team
Published: January 2014

AbstractThe New Vacuum Solar Telescope (NVST) is a new generation ground-based solar facility of China. One of the post-focus instruments is the multi-channel high-resolution imaging system, which is designed to simultaneously observe the dynamic gas motion in the solar photosphere and chromosphere. Since October of 2010 it has been operational in the NVST and some necessary updates were performed in past 2 years. Here we first give a general introduction of this system, and then we exhibit one near-limb observation of solar filaments obtained using this system. By this communication, we would like to show the potential ability to perform the high resolution observation of solar filaments (prominences) using the multi-channel imaging system in the NVST.
Observations of flux rope formation prior to coronal mass ejections
Authors: Green Lucie M. , Kliem Bernhard 
Published: January 2014

AbstractUnderstanding the magnetic configuration of the source regions of coronal mass ejections (CMEs) is vital in order to determine the trigger and driver of these events. Observations of four CME productive active regions are presented here, which indicate that the pre-eruption magnetic configuration is that of a magnetic flux rope. The flux ropes are formed in the solar atmosphere by the process known as flux cancellation and are stable for several hours before the eruption. The observations also indicate that the magnetic structure that erupts is not the entire flux rope as initially formed, raising the question of whether the flux rope is able to undergo a partial eruption or whether it undergoes a transition in specific flux rope configuration shortly before the CME.
FIP bias in a sigmoidal active region
Authors: Baker D. , Brooks D. H. , Démoulin P. , van Driel-Gesztelyi Lidia , Green L. M. , Steed K. , Carlyle J. 
Published: January 2014

AbstractWe investigate first ionization potential (FIP) bias levels in an anemone active region (AR) - coronal hole (CH) complex using an abundance map derived from Hinode/EIS spectra. The detailed, spatially resolved abundance map has a large field of view covering 359″ × 485″. Plasma with high FIP bias, or coronal abundances, is concentrated at the footpoints of the AR loops whereas the surrounding CH has a low FIP bias, ~1, i.e. photospheric abundances. A channel of low FIP bias is located along the AR's main polarity inversion line containing a filament where ongoing flux cancellation is observed, indicating a bald patch magnetic topology characteristic of a sigmoid/flux rope configuration.
The contribution of X-ray polar blowout jets to the solar wind mass and energy
Authors: Poletto Giannina , Sterling Alphonse C. , Pucci Stefano , Romoli Marco 
Published: January 2014

AbstractBlowout jets constitute about 50% of the total number of X-ray jets observed in polar coronal holes. In these events, the base magnetic loop is supposed to blow open in what is a scaled-down representation of two-ribbon flares that accompany major coronal mass ejections (CMEs): indeed, miniature CMEs resulting from blowout jets have been observed. This raises the question of the possible contribution of this class of events to the solar wind mass and energy flux. Here we make a first crude evaluation of the mass contributed to the wind and of the energy budget of the jets and related miniature CMEs, under the assumption that small-scale events behave as their large-scale analogs. This hypothesis allows us to adopt the same relationship between jets and miniature-CME parameters that have been shown to hold in the larger-scale events, thus inferring the values of the mass and kinetic energy of the miniature CMEs, currently not available from observations. We conclude our work estimating the mass flux and the energy budget of a blowout jet, and giving a crude evaluation of the role possibly played by these events in supplying the mass and energy that feeds the solar wind.
Evolution of interplanetary coronal mass ejections and magnetic clouds in the heliosphere
Authors: Démoulin Pascal 
Published: January 2014

AbstractInterplanetary Coronal Mass Ejections (ICMEs), and more specifically Magnetic Clouds (MCs), are detected with in situ plasma and magnetic measurements. They are the continuation of the CMEs observed with imagers closer to the Sun. A review of their properties is presented with a focus on their magnetic configuration and its evolution. Many recent observations, both in situ and with imagers, point to a key role of flux ropes, a conclusion which is also supported by present coronal eruptive models. Then, is a flux rope generically present in an ICME? How to quantify its 3D physical properties when it is detected locally as a MC? Is it a simple flux rope? How does it evolve in the solar wind? This paper reviews our present answers and limited understanding to these questions.
The Chinese Giant Solar Telescope
Authors: Liu Zhong , Deng Yuanyong , Ji Haisheng 
Published: January 2014

AbstractChinese Giant Solar Telescope is the next generation ground-based solar telescope. The main science task of this telescope is to observe the ultra fine structures of the solar magnetic field and dynamic field. Due to the advantages in polarization detection and thermal controlling with a symmetrical circular system, the current design of CGST is a 6~8 meter circular symmetrical telescope. The results of simulations and analysis showed that the current design could meet the demands of most science cases not only in infrared bands but also in near infrared bands and even in visible bands. The prominences and the filaments are very important science cases of CGST. The special technologies for prominence observation will be developed, including the day time laser guide star and MCAO. CGST is proposed by all solar observatories and several institutes and universities in China. It is supported by CAS and NSFC (National Natural Science Foundation of China) as a long term astronomical project.
On Critical Heights and Longitudinal Magnetic Field Strength in Prominences
Authors: Alexeeva I. V. , Kim I. S. 
Published: January 2014

AbstractThe distributions of the measured longitudinal magnetic field strength, B″, and maximum height observed, h, are presented. 50 Mm, 30–35 G and 50 G respectively are found to be the critical h and B″ for the pre-eruption of quiescent prominences.
The spatial relation between EUV cavities and linear polarization signatures
Authors: Bak-Stȩślicka Urszula , Gibson Sarah E. , Fan Yuhong , Bethge Christian , Forland Blake , Rachmeler Laurel A. 
Published: January 2014

AbstractSolar coronal cavities are regions of rarefied density and elliptical cross-section. The Coronal Multi-channel Polarimeter (CoMP) obtains daily full-Sun coronal observations in linear polarization, allowing a systematic analysis of the coronal magnetic field in polar-crown prominence cavities. These cavities commonly possess a characteristic “lagomorphic” signature in linear polarization that may be explained by a magnetic flux-rope model. We analyze the spatial relation between the EUV cavity and the CoMP linear polarization signature.
24 synoptic maps 1974-1982 (ascending phase of cycle XXI) of 323 prominence average magnetic fields measured by the Hanle effect
Authors: Bommier Véronique 
Published: January 2014

AbstractThe poster was made of 323 average prominence magnetic fields reported on 24 synoptic maps. The paper first resumes the methods for the field derivation, and the different results of the whole program of these second generation Hanle effect observations. From their conclusions, it was possible to derive a unique field vector for each of the 323 prominences. The maps put in evidence a large scale structure of the prominence magnetic field, probably distorted by the differential rotation, which leads to a systematically small angle (on the order of 30°) between the field vector and the prominence long axis.
The solar physics FORWARD codes: Now with widgets!
Authors: Forland Blake , Gibson Sarah , Dove James , Kucera Therese 
Published: January 2014

AbstractWe have developed a suite of forward-modeling IDL codes (FORWARD) to convert analytic models or simulation data cubes into coronal observables, allowing a direct comparison with observations. Observables such as extreme ultraviolet, soft X-ray, white light, and polarization images from the Coronal Multichannel Polarimeter (CoMP) can be reproduced. The observer's viewpoint is also incorporated in the FORWARD analysis and the codes can output the results in a variety of forms in order to easily create movies, Carrington maps, or simply observable information at a particular point in the plane of the sky. We present a newly developed front end to the FORWARD codes which utilizes IDL widgets to facilitate ease of use by the solar physics community. Our ultimate goal is to provide as useful a tool as possible for a broad range of scientific applications.
A Statistical Study on Characteristics of Disappearing Prominences
Authors: Joshi Anand D. , Bong Su-Chan , Srivastava Nandita 
Published: January 2014

AbstractReal-time monitoring of filaments is essential for the prediction of their eruption and the ensuing coronal mass ejection (CME). We apply an automated algorithm for the detection and tracking of filaments in full-disc Hα images to obtain their physical attributes. This provides an accurate onset time of the eruption, and also allows us to study the physical characteristics of the erupting filaments in an objective manner.
On magnetic measurements in prominences
Authors: Kim I. S. , Bugaenko O. I. 
Published: January 2014

AbstractThe successes of magnetic measurements in faint objects located near very bright ones are strongly depending on the stray light in the telescope. We propose a mask with a variable transmission placed on the primary optics of a telescope. Our computations of the stray light in such a telescope indicate that the calculated coronagraphic factor of improvement, K, would increase at least by 2 orders of magnitude compared to the Lyot-type coronagraph.
3D dynamical structuring of a high latitude erupting prominence: II- Analysis of the coronal context and eruption
Authors: Koutchmy Serge , Filippov Boris , Tavabi Ehsan , Bazin Cyrille , Weiller Sylvain 
Published: January 2014

AbstractBoth the origin of the quiescent prominences and their eruption related to CMEs event are still a matter of extended studies. The case of high latitudes quiescent prominences producing slow CMEs can be considered as a potential component of the slow wind. A high latitude prominence was observed on November 13 - 14, 2011. A schematic representation of flux rope is proposed to describe the magnetic structure of the prominence prior to its eruption.
Dynamics in the filament of september 17 2010 and in its channel
Authors: Mein Nicole , Mein Pierre , Schmieder Brigitte , Malherbe Jean-Marie , Roudier Thierry 
Published: January 2014

AbstractDynamics of a filament is investigated in Hα. Counterstreaming flows are observed along the filament. Photospheric horizontal motions have been computed by using a Coherent Structure Tracking algorithm in the filament environment.
Structure and Dynamics of an Eruptive Prominence on the Quiet Sun
Authors: Su Yingna , Reeves Katharine K. , McCauley Patrick , van Ballegooijen Adriaan A. , DeLuca Edward E. 
Published: January 2014

AbstractWe present preliminary results on the investigation of one polar crown prominence that erupted on 2012 March 11. This prominence is viewed at the east limb by SDO/AIA and displays a simple vertical-thread structure. A bright U-shape (double horn-like) structure is observed surrounding the upper portion of the prominence before the eruption and becomes more prominent during the eruption. When viewed on the disk, STEREO_B shows that this prominence is composed of series of vertical threads and displays a loop-like structure during the eruption. We focus on the magnetic support of the prominence by studying the structure and dynamics before and during the eruption using observations from SDO and STEREO. We will also present preliminary DEM analysis of the cavity surrounding the prominence.
Prominence Formation and Destruction
Authors: Xia Chun , Antolin Patrick , Keppens Rony 
Published: January 2014

AbstractIn earlier work, we demonstrated the in-situ formation of a quiescent prominence in a sheared magnetic arcade by chromospheric evaporation and thermal instability in a multi-dimensional MHD model. Here, we improve our setup and reproduce the formation of a curtain-like prominence from first principles, while showing the coexistence of the growing, large-scale prominence with short-lived dynamic coronal rain in overlying loops. When the localized heating is gradually switched off, the central prominence expands laterally beyond the range of its self-created magnetic dips and falls down along the arched loops. The dipped loops recover their initially arched shape and the prominence plasma drains to the chromosphere completely.
Coronal Multi-channel Polarimeter at the Lomnicky Peak Observatory
Authors: Schwartz P. , Ambroz J. , Gömöry P. , Kozák M. , Kučera A. , Rybák J. , Tomczyk S. , Sewell S. , Aumiller P. , Summers R. , Sutherland L. , Watt A. 
Published: January 2014

AbstractCoronal Multi-channel Polarimeter (CoMP-S), developed by HAO/NCAR, has been introduced to regular operation at the Lomnicky Peak Observatory (High Tatras in northern Slovakia, 2633 m a.s.l.) of the Astronomical Institute of Slovak Academy of Sciences. We present here the technical parameters of the current version of the instrument and its potential for observations of prominences in the visual and near-IR spectral regions. The first results derived from observations of prominences in the Hα emission line taken during a coordinated observing campaign of several instruments in October 2012 are shown here.
Multisite phosphorylation of 14-3-3 proteins by calcium-dependent protein kinases
Authors: Swatek Kirby N. , Wilson Rashaun S. , Ahsan Nagib , Tritz Rebecca L. , Thelen Jay J. 
Published: January 2014

Plant 14-3-3 proteins are phosphorylated at multiple sites in vivo; however, the protein kinase(s) responsible are unknown. Of the 34 CPK (calcium-dependent protein kinase) paralogues in Arabidopsis thaliana, three (CPK1, CPK24 and CPK28) contain a canonical 14-3-3-binding motif. These three, in addition to CPK3, CPK6 and CPK8, were tested for activity against recombinant 14-3-3 proteins χ and ε. Using an MS-based quantitative assay we demonstrate phosphorylation of 14-3-3 χ and ε at a total of seven sites, one of which is an in vivo site discovered in Arabidopsis. CPK autophosphorylation was also comprehensively monitored by MS and revealed a total of 45 sites among the six CPKs analysed, most of which were located within the N-terminal variable and catalytic domains. Among these CPK autophosphorylation sites was Tyr463 within the calcium-binding EF-hand domain of CPK28. Of all CPKs assayed, CPK28, which contained an autophosphorylation site (Ser43) within a canonical 14-3-3-binding motif, showed the highest activity against 14-3-3 proteins. Phosphomimetic mutagenesis of Ser72 to aspartate on 14-3-3χ, which is adjacent to the 14-3-3-binding cleft and conserved among all 14-3-3 isoforms, prevented 14-3-3-mediated inhibition of phosphorylated nitrate reductase.
On the category of cofinite modules which is Abelian
Authors: Bahmanpour Kamal , Naghipour Reza , Sedghi Monireh 
Published: January 2014

Let

R
R

denote a commutative Noetherian (not necessarily local) ring and

I
I

an ideal of

R
R

of dimension one. The main purpose of this paper is to generalize, and to provide a short proof of, K. I. Kawasaki’s theorem that the category

M

(
R
,
I

)

c
o
f

\mathscr {M}(R, I)_{cof}

of

I
I

-cofinite modules over a commutative Noetherian local ring

R
R

forms an Abelian subcategory of the category of all

R
R

-modules. Consequently, this assertion answers affirmatively the question raised by R. Hartshorne in his article Affine duality and cofiniteness [Invent. Math. 9 (1970), 145-164] for an ideal of dimension one in a commutative Noetherian ring

R
R

.
LGBT Neighbourhoods and ‘New Mobilities’: Towards Understanding Transformations in Sexual and Gendered Urban Landscapes
Authors: Nash Catherine J. , Gorman‐Murray Andrew 
Published: January 2014

AbstractIn this article we apply insights from ‘new mobilities’ approaches to understand the shifting sexual and gendered landscapes of major cities in the global North. The empirical context is the purported ‘demise’ of traditional gay villages in Toronto, Canada and Sydney, Australia, and the emergence of ‘LGBT neighbourhoods’ elsewhere in the inner city. We reinterpret the historical geography of twentieth century LGBT lives and the associated ‘rise and fall’ of gay enclaves through the lens of the ‘politics of mobility’. In this reading, it is apparent that multifaceted movements — migration, physical and social mobility, and motility — underpin the formation of gay enclaves and recent transformations in sexual and gendered landscapes. After the second world war, LGBT communities in the global North were embedded in specific historical geographies of mobility and we trace these in the Canadian and Australian contexts. The ‘great gay migration’ from the 1960s to the 1980s has been joined by new LGBT constellations of mobility in the 2000s, and these have imprinted upon the sexual and gendered landscapes of Toronto and Sydney.