bluuebunny/crossref_metadata_2025_split huggingface dataset:
ZERO2HERO – Az alternatív felzárkóztatás
Authors: Bodnár Gabriella , Bakonyvári Dávid , Szilágyi Brigitta 
Published: February 2018

A Műegyetemre felvételt nyert hallgatók matematikai képességei, előismeretei igen eltérőek, sokan közülük komoly hiányosságokkal küzdenek. A bekerüléshez szükséges pontok megszerzéséért folytatott küzdelemben a megfelelő matematikai ismeretek elsajátítására már nem marad elegendő idő, energia. A diák a felvételi pontban kedvezőbb utakat járja be, ami a bekerülést követően fejti ki hatását. A középiskolában megszerezett tudást tekintve vegyes összetételű csoportok, ezen belül is a hiányzó alapok, jelentősen megnehezítik az egyetemi matematikaoktatást, számos problémát felvetve mind hallgatói, mind oktatói oldalról. Ily módon a hátrányokkal induló elsőéves esetét tekintve egy effajta lemaradás többet jelenthet az adott tantárgy nehezebb teljesítésénél, amin azt értjük, hogy adott ismeretanyag elsajátításához arányaiban több idő szükséges, mint a tantárgy ajánlott bemeneti szintjét jelentő tudással rendelkező évfolyamtársának. A helyzetet súlyosbítja, hogy a felsőoktatás jelenlegi keretei között kevésbé van mód differenciált oktatásra. Ezek a problémák a BME valamennyi karát érintik, így a Gazdaság- és Társadalomtudományi Karon folytatott képzésekre is kihatnak. 2016 augusztusában egy kéthetes szintrehozó tanfolyam keretén belül arra tettünk kísérletet, hogy a középiskolai anyag rendszerezésével, a tanultak átismétlésével segítsük az új hallgatók egyetemi tanulmányainak megkezdését. ***The mathematical capacities and previous knowledge of the students accepted at the Budapest University of Technology (BME) are very diverse; many of them face serious deficiencies. The fight for the points they are to collect in order to be accepted does not allow them to pay enough time and energy to acquire the adequate mathematical knowledge. The students choose the way more favourable for them in terms of the admission points, the effects of which will appear after they have been accepted. The groups that are mixed concerning the knowledge gained at secondary school as well as the missing grounds considerably make teaching mathematics more difficult at the universities, and raise several problems on both the students’ and the teachers’ side. Thus, in case a first-grade student faces this type of disadvantage, lagging behind means more than just a more difficult acquisition of the certain material; he/she will need proportionally more time to learn the certain subject than his/her peers being in possession of the knowledge equal to the suggested entrance level of the subject. This situation is further rendered by the fact that within the frames of today’s higher education there are very limited possibilities of differentiated instruction. Each of the departments of the BME is concerned by this problem, likewise the courses conducted at the Department for Economic and Social Sciences. In August 2016, within the frames of a two-week bridging-the-gap course we made a try to help the new students start their university studies by repeating the adequate topics.
Korszerű IKT eszközök alkalmazása az SNI- s tanulók fejlesztésében
Authors: Biró Kinga 
Published: February 2018

Az információs és kommunikációs technológiák (IKT) ma már a mindennapi élet részévé váltak. Hatással vannak a társadalom számos területére, beleértve az oktatást, a képzést és a foglalkoztatást, de ezek mellett értékes eszköz a fogyatékossággal és a sajátos igényekkel élő emberek számára. A sajátos nevelési igényű (SNI) gyermekek oktatásában fontos szerepet játszik az IKT. Az oktatás hatékonyságát növeli, ha az információ több kommunikációs csatornán keresztül áramlik. Kutatásomban bemutatom az SNI- s tanulók integrálásának lehetséges módjait, akadályait a többségi nevelési-oktatási intézményben, majd ismertetem a fejlesztésük során alkalmazható korszerű digitális eszközöket. Az IKT használatának fő célja, hogy a SNI- s tanulók oktatásában egyenlő feltételeket teremtsünk az oktatási minden területén. ***Information and Communication Technologies (ICT) have become part of everyday life. They have an impact on many areas of society, including education, training and employment, but they are a valuable tools for people with disabilities and people with special needs also. ICT has an important role in education of students with special educational (SEN). The effectiveness of education increases if the information flows through multiple communication channels. In my research I demonstrate the possible ways, obstacles of the SEN student’s integration in the mainstream education systems, then I review the modern digital tools that can be used in their development. The main purpose of ICT use is to create equal conditions for the SEN students with special educational needs in all areas of education.
A pedagógus minősítési rendszer a jogszabályi változások tükrében (2013-2017)
Authors: Lunczer Erika Katalin 
Published: February 2018

E tanulmány célja a pedagógus-életpályamodellhez kapcsolódó minősítési rendszer vizsgálata. Kutatásom elsőként elméleti síkon folyt, hiszen a pedagógusminősítés rendszere egyrészt a jogszabályi környezet által biztosított tartalmi elemekből és eljárásrendből, másrészt a központilag meghatározott, egységes követelményeket és értékeléseket magába foglaló módszertanból áll. Először vázlatosan felvonultatom a pedagógus minősítési rendszer elemeit, majd a pedagógusminősítések elindulásának lépéseit. Az elméleti háttér vizsgálata során végül a hazai rendszerhez közvetlenül kötődő jogi normákra, azok változásaira és következményeire (az Oktatási Hivatal által közzétett támogató segédanyagok, Útmutatók formálódására) fókuszáltam. Az elemzéshez táblázatos formában vázlatok készültek, melyekből egyértelműen látható volt az áttanulmányozott jogszabályok időbeli változása. ***This study examines the qualification system connected to the teacher life career model. I conducted my research primarily at the theoretical level since the system of teacher qualification system consists on one hand of the content elements and procedures set by the legal environment and the centrally defined methodology containing the uniform requirements and evaluations on the other. First I draw a sketch of the elements of the teacher qualification system, then of the first steps of the qualification procedure. During examining the theoretical background, I focused at the legal norms directly connected to the domestic system, their changes and the consequences of these (exerted on the evolution of the supporting materials and Guides published by the Educational Authority). To support my analysis, I made rough diagrams showing the chronological changes in the examined legal rules.
A New Dark Vortex on Neptune
Authors: Wong Michael H. , Tollefson Joshua , Hsu Andrew I. , Pater Imke de , Simon Amy A. , Hueso Ricardo , Sánchez-Lavega Agustín , Sromovsky Lawrence , Fry Patrick , Luszcz-Cook Statia , Hammel Heidi , Delcroix Marc , Kleer Katherine de , Orton Glenn S. , Baranec Christoph 
Published: February 2018

Abstract
An outburst of cloud activity on Neptune in 2015 led to speculation about whether the clouds were convective in nature, a wave phenomenon, or bright companions to an unseen dark vortex (similar to the Great Dark Spot studied in detail by Voyager 2). The Hubble Space Telescope (HST) finally answered this question by discovering a new dark vortex at 45 degrees south planetographic latitude, named SDS-2015 for “southern dark spot discovered in 2015.” SDS-2015 is only the fifth dark vortex ever seen on Neptune. In this paper, we report on imaging of SDS-2015 using HST’s Wide Field Camera 3 across four epochs: 2015 September, 2016 May, 2016 October, and 2017 October. We find that the size of SDS-2015 did not exceed 20 degrees of longitude, more than a factor of two smaller than the Voyager dark spots, but only slightly smaller than previous northern-hemisphere dark spots. A slow (1.7–2.5 deg/year) poleward drift was observed for the vortex. Properties of SDS-2015 and its surroundings suggest that the meridional wind shear may be twice as strong at the deep level of the vortex as it is at the level of cloud-tracked winds. Over the 2015–2017 period, the dark spot’s contrast weakened from about

to about

, while companion clouds shifted from offset to centered, a similar evolution to some historical dark spots. The properties and evolution of SDS-2015 highlight the diversity of Neptune’s dark spots and the need for faster cadence dark spot observations in the future.
The Radial Velocity Variability of the K-giant γ Draconis: Stellar Variability Masquerading as a Planet
Authors: Hatzes A. P. , Endl M. , Cochran W. D. , MacQueen P. J. , Han I. , Lee B.-C. , Kim K.-M. , Mkrtichian D. , Döllinger M. , Hartmann M. , Karjalainen M. , Dreizler S. 
Published: February 2018

Abstract
We present precise stellar radial velocity (RV) measurements of γ Dra taken from 2003 to 2017. The data from 2003 to 2011 show coherent, long-lived variations with a period of 702 days. These variations are consistent with the presence of a planetary companion having m sin i = 10.7 M
Jup whose orbital properties are typical for giant planets found around evolved stars. An analysis of the Hipparcos photometry, Ca ii S-index measurements, and measurements of the spectral line shapes during this time show no variations with the RV of the planet, which seems to “confirm” the presence of the planet. However, RV measurements taken from 2011–2017 seem to refute this. From 2011–2013, the RV variations virtually disappear, only to return in 2014 but with a noticeable phase shift. The total RV variations are consistent either with amplitude variations on timescales of ≈10.6 year, or the beating effect between two periods of 666 and 801 days. It seems unlikely that both these signals stem from a two-planet system. A simple dynamical analysis indicates that there is only a 1%–2% chance that the two-planet system is stable. Rather, we suggest that this multi-periodic behavior may represent a new form of stellar variability, possibly related to oscillatory convective modes. If such intrinsic stellar variability is common around K giant stars and is attributed to planetary companions, then the planet occurrence rate among these stars may be significantly lower than thought.
Diffusive Tidal Evolution for Migrating Hot Jupiters
Authors: Wu 武延 Yanqin 庆 
Published: February 2018

Abstract
I consider a Jovian planet on a highly eccentric orbit around its host star, a situation produced by secular interactions with its planetary or stellar companions. The tidal interactions at every periastron passage exchange energy between the orbit and the planet’s degree-2 fundamental-mode. Starting from zero energy, the f-mode can diffusively grow to large amplitudes if its one-kick energy gain is ≥10−5 of the orbital energy. This requires a pericenter distance of ≤4 tidal radii (or 1.6 Roche radii). If the f-mode has a non-negligible initial energy, diffusive evolution can occur at a lower threshold. The first effect can stall the secular migration as the f-mode can absorb orbital energy and decouple the planet from its secular perturbers, parking all migrating jupiters safely outside the zone of tidal disruption. The second effect leads to rapid orbit circularization as it allows an excited f-mode to continuously absorb orbital energy as the orbit eccentricity decreases. So without any explicit dissipation, other than the fact that the f-mode will damp nonlinearly when its amplitude reaches unity, the planet can be transported from a few au to ∼0.2 au in ∼104 years. Such a rapid circularization is equivalent to a dissipation factor Q ∼ 1, and it explains the observed deficit of super-eccentric Jovian planets. Lastly, the repeated f-mode breaking likely deposits energy and angular momentum in the outer envelope and avoids thermally ablating the planet. Overall, this work boosts the case for hot Jupiter formation through high-eccentricity secular migration.
A Model for the Onset of Self-gravitation and Star Formation in Molecular Gas Governed by Galactic Forces. I. Cloud-scale Gas Motions
Authors: Meidt Sharon E. , Leroy Adam K. , Rosolowsky Erik , Kruijssen J. M. Diederik , Schinnerer Eva , Schruba Andreas , Pety Jerome , Blanc Guillermo , Bigiel Frank , Chevance Melanie , Hughes Annie , Querejeta Miguel , Usero Antonio 
Published: February 2018

Abstract
Modern extragalactic molecular gas surveys now reach the scales of star-forming giant molecular clouds (GMCs; 20–50 pc). Systematic variations in GMC properties with galaxy environment imply that clouds are not universally self-gravitating objects, decoupled from their surroundings. Here we re-examine the coupling of clouds to their environment and develop a model for 3D gas motions generated by forces arising with the galaxy gravitational potential defined by the background disk of stars and dark matter. We show that these motions can resemble or even exceed the motions needed to support gas against its own self-gravity throughout typical galactic disks. The importance of the galactic potential in spiral arms and galactic centers suggests that the response to self-gravity does not always dominate the motions of gas at GMC scales, with implications for observed gas kinematics, virial equilibrium, and cloud morphology. We describe how a uniform treatment of gas motions in the plane and in the vertical direction synthesizes the two main mechanisms proposed to regulate star formation: vertical pressure equilibrium and shear/Coriolis forces as parameterized by Toomre Q ≈ 1. As the modeled motions are coherent and continually driven by the external potential, they represent support for the gas that is distinct from that conventionally attributed to turbulence, which decays rapidly and thus requires maintenance, e.g., via feedback from star formation. Thus, our model suggests that the galaxy itself can impose an important limit on star formation, as we explore in a second paper in this series.
The Einstein@Home Gamma-ray Pulsar Survey. II. Source Selection, Spectral Analysis, and Multiwavelength Follow-up
Authors: Wu J. , Clark C. J. , Pletsch H. J. , Guillemot L. , Johnson T. J. , Torne P. , Champion D. J. , Deneva J. , Ray P. S. , Salvetti D. , Kramer M. , Aulbert C. , Beer C. , Bhattacharyya B. , Bock O. , Camilo F. , Cognard I. , Cuéllar A. , Eggenstein H. B. , Fehrmann H. , Ferrara E. C. , Kerr M. , Machenschalk B. , Ransom S. M. , Sanpa-Arsa S. , Wood K. 
Published: February 2018

Abstract
We report on the analysis of 13 gamma-ray pulsars discovered in the Einstein@Home blind search survey using Fermi Large Area Telescope (LAT) Pass 8 data. The 13 new gamma-ray pulsars were discovered by searching 118 unassociated LAT sources from the third LAT source catalog (3FGL), selected using the Gaussian Mixture Model machine-learning algorithm on the basis of their gamma-ray emission properties being suggestive of pulsar magnetospheric emission. The new gamma-ray pulsars have pulse profiles and spectral properties similar to those of previously detected young gamma-ray pulsars. Follow-up radio observations have revealed faint radio pulsations from two of the newly discovered pulsars and enabled us to derive upper limits on the radio emission from the others, demonstrating that they are likely radio-quiet gamma-ray pulsars. We also present results from modeling the gamma-ray pulse profiles and radio profiles, if available, using different geometric emission models of pulsars. The high discovery rate of this survey, despite the increasing difficulty of blind pulsar searches in gamma rays, suggests that new systematic surveys such as presented in this article should be continued when new LAT source catalogs become available.
Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars
Authors: Wadiasingh Zorawar , Baring Matthew G. , Gonthier Peter L. , Harding Alice K. 
Published: February 2018

Abstract
Hard, nonthermal, persistent pulsed X-ray emission extending between 10 and ∼150 keV has been observed in nearly 10 magnetars. For inner-magnetospheric models of such emission, resonant inverse Compton scattering of soft thermal photons by ultrarelativistic charges is the most efficient production mechanism. We present angle-dependent upscattering spectra and pulsed intensity maps for uncooled, relativistic electrons injected in inner regions of magnetar magnetospheres, calculated using collisional integrals over field loops. Our computations employ a new formulation of the QED Compton scattering cross section in strong magnetic fields that is physically correct for treating important spin-dependent effects in the cyclotron resonance, thereby producing correct photon spectra. The spectral cutoff energies are sensitive to the choices of observer viewing geometry, electron Lorentz factor, and scattering kinematics. We find that electrons with energies ≲15 MeV will emit most of their radiation below 250 keV, consistent with inferred turnovers for magnetar hard X-ray tails. More energetic electrons still emit mostly below 1 MeV, except for viewing perspectives sampling field-line tangents. Pulse profiles may be singly or doubly peaked dependent on viewing geometry, emission locale, and observed energy band. Magnetic pair production and photon splitting will attenuate spectra to hard X-ray energies, suppressing signals in the Fermi-LAT band. The resonant Compton spectra are strongly polarized, suggesting that hard X-ray polarimetry instruments such as X-Calibur, or a future Compton telescope, can prove central to constraining model geometry and physics.
Electron-density-sensitive Line Ratios of Fe xiii– xvi from Laboratory Sources Compared to CHIANTI
Authors: Weller M. E. , Beiersdorfer P. , Soukhanovskii V. A. , Scotti F. , LeBlanc B. P. 
Published: February 2018

Abstract
We present electron-density-sensitive line ratios for Fe xiii– xvi measured in the spectral wavelength range of 200–440 Å and an electron density range of (1–4) × 1013 cm−3. The results provide a test at the high-density limit of density-sensitive line ratios useful for astrophysical studies. The measurements were performed on the National Spherical Torus Experiment-Upgrade, where electron densities were measured independently by the laser Thomson scattering diagnostic. Spectra were collected with a flat-field grazing-incidence spectrometer, which provided a spectral resolution of up to 0.3 Å, i.e., high resolution across the broad wavelength range. The response of the instrument was relatively calibrated using spectroscopic techniques in order to improve accuracy. The line ratios are compared to other laboratory sources and the latest version of CHIANTI (8.0.2), and an agreement within 30% is found.
Chemical and Physical Picture of IRAS 16293–2422 Source B at a Sub-arcsecond Scale Studied with ALMA
Authors: Oya Yoko , Moriwaki Kana , Onishi Shusuke , Sakai Nami , López–Sepulcre Ana , Favre Cécile , Watanabe Yoshimasa , Ceccarelli Cecilia , Lefloch Bertrand , Yamamoto Satoshi 
Published: February 2018

Abstract
We have analyzed the OCS, H2CS, CH3OH, and HCOOCH3 data observed toward the low-mass protostar IRAS 16293–2422 Source B at a sub-arcsecond resolution with ALMA. A clear chemical differentiation is seen in their distributions; OCS and H2CS are extended with a slight rotation signature, while CH3OH and HCOOCH3 are concentrated near the protostar. Such a chemical change in the vicinity of the protostar is similar to the companion (Source A) case. The extended component is interpreted by the infalling-rotating envelope model with a nearly face-on configuration. The radius of the centrifugal barrier of the infalling-rotating envelope is roughly evaluated to be (30–50) au. The observed lines show the inverse P-Cygni profile, indicating the infall motion within a few 10 au from the protostar. The nearly pole-on geometry of the outflow lobes is inferred from the SiO distribution, and thus, the infalling and outflowing motions should coexist along the line of sight to the protostar. This implies that the infalling gas is localized near the protostar and the current launching points of the outflow have an offset from the protostar. A possible mechanism for this configuration is discussed.
Cracking the Conundrum of F-supergiant Coronae
Authors: Ayres Thomas R. 
Published: February 2018

Abstract

Chandra X-ray and HST far-ultraviolet (FUV) observations of three early-F supergiants have shed new light on a previous puzzle involving a prominent member of the class: α Persei (HD 20902: F5 Ib). The warm supergiant is a moderately strong, hard coronal (

K) X-ray source, but has 10 times weaker “subcoronal” Si iv 1393 Å (

K) emissions than early-G supergiants of similar high-energy properties. The α Per X-ray excess was speculatively ascribed to a close-in hyperactive G-dwarf companion, which could have escaped previous notice, lost in the glare of the bright star. However, a subsequent dedicated multi-wavelength imaging campaign failed to find any evidence for a resolved secondary. The origin of the α Per high-energy dichotomy then devolved to (1) an unresolved companion or (2) intrinsic coronal behavior. Exploring the second possibility, the present program has found that early-F supergiants do appear to belong to a distinct coronal class, characterized by elevated X-ray/FUV ratios, although sharing some similarities with Cepheid variables in their transitory X-ray “high states.” Remarkably, the early-F supergiants now are seen to align with the low-activity end of the X-ray/FUV sequence defined by late-type dwarfs, suggesting that the disjoint behavior relative to the G supergiants might be attributed to thinner outer atmospheres on the F types, as in dwarfs, but in this case perhaps caused by a weakened “ionization valve” effect due to overly warm photospheres.
HelMod in the Works: From Direct Observations to the Local Interstellar Spectrum of Cosmic-Ray Electrons
Authors: Boschini M. J. , Torre S. Della , Gervasi M. , Grandi D. , Jóhannesson G. , La Vacca G. , Masi N. , Moskalenko I. V. , Pensotti S. , Porter T. A. , Quadrani L. , Rancoita P. G. , Rozza D. , Tacconi M. 
Published: February 2018

Abstract
The local interstellar spectrum (LIS) of cosmic-ray (CR) electrons for the energy range 1 MeV to 1 TeV is derived using the most recent experimental results combined with the state-of-the-art models for CR propagation in the Galaxy and in the heliosphere. Two propagation packages, GALPROP and HelMod, are combined to provide a single framework that is run to reproduce direct measurements of CR species at different modulation levels, and at both polarities of the solar magnetic field. An iterative maximum-likelihood method is developed that uses GALPROP-predicted LIS as input to HelMod, which provides the modulated spectra for specific time periods of the selected experiments for model-data comparison. The optimized HelMod parameters are then used to adjust GALPROP parameters to predict a refined LIS with the procedure repeated subject to a convergence criterion. The parameter optimization uses an extensive data set of proton spectra from 1997 to 2015. The proposed CR electron LIS accommodates both the low-energy interstellar spectra measured by Voyager 1 as well as the high-energy observations by PAMELA and AMS-02 that are made deep in the heliosphere; it also accounts for Ulysses counting rate features measured out of the ecliptic plane. The interstellar and heliospheric propagation parameters derived in this study agree well with our earlier results for CR protons, helium nuclei, and anti-protons propagation and LIS obtained in the same framework.