bluuebunny/crossref_metadata_2025_split huggingface dataset:
“Social policy and intelligence” Redux: a tribute to Edward Zigler
Authors: Sternberg Robert J. 
Published: September 2020

AbstractI present a theory of adaptive intelligence and discuss why I believe adaptive intelligence, rather than general intelligence, is the kind of intelligence upon which we should focus in today's world. Adaptive intelligence is the ability to adapt to, shape, and select real-world environments in ways that result in positive outcomes not only for oneself, but also for others and the world. Edward Zigler was among the first to recognize the importance of levels of adaptation to intellectual deficiency, arguing from early on that intellectual challenges needed to be recognized not just in terms of IQ but also in terms of adaptive functioning. Adaptive intelligence is compared to and contrasted with general intelligence, which is usually defined as the first factor in a factor analysis of psychometric tests. I first introduce the main issues in the article. Then I discuss how one even would decide what intelligence is. Next I discuss broader theories of intelligence and especially the theory of adaptive intelligence. Then I talk about the perishability of theories of intelligence and other things—to what extent are they set up so that people are willing and able to move beyond them? Finally, I discuss how individual outcomes do not necessarily predict collective outcomes.
A middle-aged man with adenoid cystic lung carcinoma: not every dyspnoea is the novel coronavirus, even during a pandemic
Authors: Chakrabarti Deep , Qayoom Sumaira , Kukreja Divya , Resu Abigail Veravolu , Rajan Shiv , Verma Mranalini , Gupta Rajeev , Bhatt Madan Lal Brahma 
Published: September 2020

AbstractBackground:A middle-aged gentleman presenting with dyspnoea was presumptively assumed to be a novel coronavirus suspect.Findings:Nasopharyngeal and oropharyngeal swabs were reported negative, and clinico-radiological workup revealed a case of adenoid cystic carcinoma (ACC) of the lung with metastases to the contralateral lung and the lumbar vertebrae.Conclusion:ACC is a rare malignancy of exocrine glands. Most commonly found in the minor salivary glands, they may rarely occur in other sites. Primary ACC of the lung is a rare histologic subtype that is encountered infrequently in clinical practice for which standard guidelines do not exist.
Confronting the Indian State: Islamism, secularism, and the Kashmiri Muslim question
Authors: Majid Iymon 
Published: September 2020

AbstractThis paper investigates the framework of Islamist politics of Jama'at e Islami in Indian-administered Kashmir. Even though Jama'at e Islami creates the notion of “other” in the Indian state and challenges it but Kashmir's provincial relationship with India also forces it to work within the limits set up by the same state. This paper, thus, conceptualizes the relationship between Indian state and Islamists in a Muslim Majority region that demands the right to self-determination. In doing so, the paper interrogates Jama'at e Islami's rhetorical opposition to the political doctrine of Indian secularism and raises queries about minority rights and their place in the Islamist project.
On the properties of the magnetic Chemically Peculiar B, A, and F-type stars
Authors: Yüce Kutluay , Adelman Saul J. , Pyper Diane M. , Dukes Robert J. 
Published: September 2020

AbstractWe present a preliminary analysis of the Strömgren uvby photometry of the magnetic CP stars obtained using the Four College Automated Photometric Telescope for its 21.5 years of operation ending in Fall 2012. We summarize the photometry for all the FCAPT mCP stars that have been published to date. We do not find any significant correlation between the amplitudes of variation in the uvby filters and the periods. A small number of stars show anomalous behaviour of the v filter which will be discussed in a future study.
Magnetic field and prominences of the young, solar-like, ultra-rapid rotator AP 149
Authors: Cang Tianqi , Petit Pascal , Folsom Colin , Donati Jean-Francois 
Published: September 2020

AbstractYoung solar analogs reaching the main sequence experience very strong magnetic activity, directly linked to their angular momentum loss through wind and mass ejections. We investigate here the surface and chromospheric activity of the ultra-rapid rotator AP 149 in the young open cluster alpha Persei. With a time-series of spectropolarimetric observations gathered over two nights with ESPaDOnS, we are able to reconstruct the surface distribution of brightness and magnetic field using the Zeeman-Doppler-Imaging (ZDI) method. Using the same data set, we also map the spatial distribution of prominences through tomography of H-alpha emission. We find that AP 149 shows a strong cool spot and magnetic field closed to the polar cap. This star is the first example of a solar-type star to have its magnetic field and prominences mapped together, which will help to explore the respective role of wind and prominences in the angular momentum evolution of the most active stars.
Observing the Sun with the Atacama Large Millimeter/submillimeter Array – from continuum to magnetic fields
Authors: Wedemeyer Sven , Szydlarski Mikolaj , Rodriguez Jaime de la Cruz , Jafarzadeh Shahin 
Published: September 2020

AbstractThe Atacama Large Millimeter/submillimeter Array offers regular observations of our Sun since 2016. After an extended period of further developing and optimizing the post-processing procedures, first scientific results are now produced. While the first observing cycles mostly provided mosaics and time series of continuum brightness temperature maps with a cadence of 1-2s, additional receiver bands and polarization capabilities will be offered in the future. Currently, polarization capabilities are offered for selected receiver bands but not yet for solar observing. An overview of the recent development, first scientific results and potential of solar magnetic field measurements with ALMA will be presented.
Fast downflows in a chromospheric filament
Authors: Sowmya K. , Lagg A. , Solanki S. K. , Castellanos Durán J. S. 
Published: September 2020

AbstractAn active region filament in the upper chromosphere is studied using spectropolarimetric data in He i 10830 Å from the GREGOR telescope. A Milne-Eddingon based inversion of the Unno-Rachkovsky equations is used to retrieve the velocity and the magnetic field vector of the region. The plasma velocity reaches supersonic values closer to the feet of the filament barbs and coexist with a slow velocity component. Such supersonic velocities result from the acceleration of the plasma as it drains from the filament spine through the barbs. The line-of-sight magnetic fields have strengths below 200 G in the filament spine and in the filament barbs where fast downflows are located, their strengths range between 100 - 700 G.
Analysis of the chromosphere and corona of low-activity early-M dwarfs
Authors: Scandariato Gaetano , Álvarez E. González , Maldonado J. , Mascareño A. Suárez ,   the HADES collaboration
Published: September 2020

AbstractWhile most of the exoplanets have been found orbiting around solar-type stars, low-mass stars have recently been recognized as ideal exo-life laboratory. Currently, stellar activity is one of the limiting factors for the characterization of Earth-twins and for assessing their habitability: understanding the activity of M dwarfs is thus crucial. In this contribution I present the spectroscopic analysis of the quiet early-M dwarfs monitored within the HADES (HArps-n red Dwarf Exoplanet Survey) radial velocity survey. The spectra allow us to analyze simultaneously the Ca ii H&K doublet and the Hydrogen Balmer series, while the intensive follow up gives us a large number of spectra ( 100) for each target. We complement this dataset with ground-based follow-up photometry and archival X-ray data. I present our results on the activity-rotation-stellar parameters and flux-flux relationships, and discuss the correlation of emission fluxes at low activity levels and the evolution timescales of active regions.
The magnetic structure and dynamics of a decaying active region
Authors: Kontogiannis Ioannis , Kuckein Christoph , González Manrique Sergio Javier , Felipe Tobias , Verma Meetu , Balthasar Horst , Denker Carsten 
Published: September 2020

AbstractWe study the evolution of the decaying active region NOAA 12708, from the photosphere up to the corona using high resolution, multi-wavelength GREGOR observations taken on May 9, 2018. We utilize spectropolarimetric scans of the 10830 Å spectral range by the GREGOR Infrared Spectrograph (GRIS), spectral imaging time-series in the Na ID2 spectral line by the GREGOR Fabry-Pérot Interferometer (GFPI) and context imaging in the Ca IIH and blue continuum by the High-resolution Fast Imager (HiFI). Context imaging in the UV/EUV from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) complements our dataset. The region under study contains one pore with a light-bridge, a few micro-pores and extended clusters of magnetic bright points. We study the magnetic structure from the photosphere up to the upper chromosphere through the spectropolarimetric observations in He II and Si I and through the magnetograms provided by the Helioseismic and Magnetic Imager (HMI). The high-resolution photospheric images reveal the complex interaction between granular-scale convective motions and a range of scales of magnetic field concentrations in unprecedented detail. The pore itself shows a strong interaction with the convective motions, which eventually leads to its decay, while, under the influence of the photospheric flow field, micro-pores appear and disappear. Compressible waves are generated, which are guided towards the upper atmosphere along the magnetic field lines of the various magnetic structures within the field-of-view. Modelling of the He i absorption profiles reveals high velocity components, mostly associated with magnetic bright points at the periphery of the active region, many of which correspond to asymmetric Si I Stokes-V profiles revealing a coupling between upper photospheric and upper chromospheric dynamics. Time-series of Na ID2 spectral images reveal episodic high velocity components at the same locations. State-of-the-art multi-wavelength GREGOR observations allow us to track and understand the mechanisms at work during the decay phase of the active region.
Multi-flux-rope system in solar active regions
Authors: Hou Yijun , Zhang Jun , Li Ting , Yang Shuhong 
Published: September 2020

AbstractMagnetic flux rope (MFR) is closely connected with solar eruptions, such as flares and coronal mass ejections. The classical scenario assumes a single MFR for each eruption, but it is reasonable to expect multiple MFRs in a complex active region (AR). Statistically investigating AR 11897, we verify the existence of multiple MFR proxies during the AR evolution. Recently, AR 12673 in 2017 September produced the two largest flares in Solar Cycle 24. The evolutions of the AR magnetic fields and the two large flares reveal that significant flux emergence and successive interactions between different emerging dipoles resulted in the formations of multiple MFRs and twisted loop bundles, which successively erupted like a chain reaction within several minutes before the peaks of the two flares. We propose that the eruptions of a multi-flux-rope system can rapidly release enormous magnetic energy and result in large flares in solar AR.
The impact of magnetism on tidal dynamics in the convective envelope of low-mass stars
Authors: Astoul A. , Mathis S. , Baruteau C. , Gallet F. , Strugarek A. , Augustson K. C. , Brun A. S. , Bolmont E. 
Published: September 2020

AbstractFor the shortest period exoplanets, star-planet tidal interactions are likely to have played a major role in the ultimate orbital evolution of the planets and on the spin evolution of the host stars. Although low-mass stars are magnetically active objects, the question of how the star’s magnetic field impacts the excitation, propagation and dissipation of tidal waves remains open. We have derived the magnetic contribution to the tidal interaction and estimated its amplitude throughout the structural and rotational evolution of low-mass stars (from K to F-type). We find that the star’s magnetic field has little influence on the excitation of tidal waves in nearly circular and coplanar Hot-Jupiter systems, but that it has a major impact on the way waves are dissipated.
The 3D structure of the penumbra at high resolution from the bottom of the photosphere to the middle chromosphere
Authors: Murabito Mariarita , Ermolli Ilaria , Giorgi Fabrizio , Stangalini Marco , Guglielmino Salvo L. , Jafarzadeh Shahin , Socas-Navarro Hector , Romano Paolo , Zuccarello Francesca 
Published: September 2020

AbstractSunspots are the most prominent feature of the solar magnetism in the photosphere. Although they have been widely investigated in the past, their structure remains poorly understood. Indeed, due to limitations in observations and the complexity of the magnetic field estimation at chromospheric heights, the magnetic field structure of sunspot above the photosphere is still uncertain. Improving the present knowledge of sunspot is important in solar and stellar physics, since spot generation is seen not only on the Sun, but also on other solar-type stars. In this regard, we studied a large, isolated sunspot with spectro-polarimeteric measurements that were acquired at the Fe I 6173 nm and Ca II 8542 nm lines by the spectropolarimeter IBIS/DST under excellent seeing conditions lasting more than three hours. Using the Non-LTE inversion code NICOLE, we inverted both line measurements simultaneously, to retrieve the three-dimensional magnetic and thermal structure of the penumbral region from the bottom of the photosphere to the middle chromosphere. Our analysis of data acquired at spectral ranges unexplored in previous studies shows clear spine and intra-spine structure of the penumbral magnetic field at chromopheric heights. Our investigation of the magnetic field gradient in the penumbra along the vertical and azimuthal directions confirms results reported in the literature from analysis of data taken at the spectral region of the He I 1083 nm triplet.
Ca II 854.2 nm spectropolarimetry compared with ALMA and with scattering polarization theory
Authors: Harvey J. W. ,   SOLIS Team
Published: September 2020

AbstractCa II 854.2 nm spectropolarimetric observations of the Sun are compared with nearly simultaneous ALMA observations. These two types of chromospheric observations show rough agreement but also several notable differences. High-sensitivity (≃ 0.01%) observations reveal ubiquitous linear polarization structures across the solar disk in the core of the 854.2 nm line that are consistent with previous theoretical studies.
Reversibility of Turbulent and Non-Collisional Plasmas: Solar Wind
Authors: Acosta Belén , Pastén Denisse , Moya Pablo S. 
Published: September 2020

AbstractWe have studied turbulent plasma as a complex system applying the method known as Horizontal Visibility Graph (HVG) to obtain the Kullback-Leibler Divergence (KLD) as a first approach to characterize the reversibility of the time series of the magnetic fluctuations. For this, we have developed the method on Particle In Cell (PIC) simulations for a magnetized plasma and on solar wind magnetic time series, considering slow and fast wind. Our numerical results show that low irreversibility values are verified for magnetic field time series associated with Maxwellian distributions. In addition, considering the solar wind plasma, our preliminary results seem to indicate that greater irreversibility degrees are reached by the magnetic field associated with slow solar wind.
Diagnosing chromospheric magnetic field through simultaneous spectropolarimetry in Hα and Ca II 854.2 nm
Authors: Nagaraju K. , Sankarasubramanian K. , Rangarajan K. E. 
Published: September 2020

AbstractMeasurement of magnetic field in this layer is challenging both from point of view of observations and interpretation of the data. We present in this work about spectropolarimetric observations of a pore, simultaneously in Ca ii (CaIR) at 854.2 nm (CaIR) and H α (656.28 nm). The observed region includes a small scale energetic event (SSEE) taking place in the region between the pore and the region which show opposite polarity to that of pore at the photosphere. The energetic event appears to be a progressive reconnection event as shown by the time evolution of the intensity profiles. Closer examination of the intensity profiles from the downflow regions suggest that the height of formation of CaIR is higher than that of Hi α, contrary to the current understanding about their height of formation. Preliminary results on the inversion of Stokes-I and V profiles of CaIR are also presented.
Linking radio flares with spots on the active binary UX Arietis
Authors: Hummel Christian A. , Beasley Anthony 
Published: September 2020

AbstractSigns of stellar activity such as large surface spots and radio flares are often related to binarity. UX Arietis is one of the most active members of the RS CVn class of binaries in which spin-up of a sub-giant/giant star by a close companion leads to the creation of magnetic fields. UX Arietis exhibits these signs of activity, originating mostly on the K0 sub-giant primary component. We measured the orbit with the CHARA interferometer and made images of a single large spot rotating in and out of view over a month in 2012. The rotation of the stars is synchronous with the orbit, and long-term photometric observations show that the spot or spots do not move much during intervals of a year. Our aim is to relate the positions of the stars and the spots on the primary to astrometry of the radio components observed during outbursts.
Coronal dimming as a proxy for stellar coronal mass ejections
Authors: Jin M. , Cheung M. C. M. , DeRosa M. L. , Nitta N. V. , Schrijver C. J. , France K. , Kowalski A. , Mason J. P. , Osten R. 
Published: September 2020

AbstractSolar coronal dimmings have been observed extensively in the past two decades and are believed to have close association with coronal mass ejections (CMEs). Recent study found that coronal dimming is the only signature that could differentiate powerful flares that have CMEs from those that do not. Therefore, dimming might be one of the best candidates to observe the stellar CMEs on distant Sun-like stars. In this study, we investigate the possibility of using coronal dimming as a proxy to diagnose stellar CMEs. By simulating a realistic solar CME event and corresponding coronal dimming using a global magnetohydrodynamics model (AWSoM: Alfvén-wave Solar Model), we first demonstrate the capability of the model to reproduce solar observations. We then extend the model for simulating stellar CMEs by modifying the input magnetic flux density as well as the initial magnetic energy of the CME flux rope. Our result suggests that with improved instrument sensitivity, it is possible to detect the coronal dimming signals induced by the stellar CMEs.
Diagnosing coronal magnetic fields with radio imaging-spectroscopy technique
Authors: Yan Yihua , Tan Baolin , Melnikov V. , Chen Xingyao , Wang Wei , Chen Linjie , Liu Fei ,   MUSER Team
Published: September 2020

AbstractMingantu Spectral Radioheliograph (MUSER) is an aperture-synthesis imaging telescope, dedicated to observe the Sun, operating on multiple frequencies in dm to cm range. The ability of MUSER to get images and measure Stokes I and V parameters simultaneously at many frequencies in a wide band is of fundamental importance. It allows one to approach/solve such important problems as measuring the strength, geometry and dynamics of magnetic field at coronal heights. Here we consider some of the recently developed radio physics methods to be used for solving the problems. These methods allow us to obtain information that is unattainable in other areas of the electromagnetic spectrum.
Statistical analysis of geomagnetic storms and their relation with the solar cycle
Authors: Reyes Paula , Pinto Victor A. , Moya Pablo S. 
Published: September 2020

AbstractGeomagnetic storms can be modeled as stochastic processes with log-normal probability distribution function over their minimum Dst index value measured during the main phase of each event. Considering a time series of geomagnetic storm events between 1957 and 2019 we have analyzed the probability of occurrence of small, moderate, strong and extreme events. The data were separated according to solar cycle (SC) and solar cycle phases and fitted through maximum likelihood method in order to compare rates of occurrence of the last Solar Cycle (SC24) with previous ones. Our results show that for Dst < – 100 nT events in SC24 are similar to those in SC20, obtaining ⁓42 vs 21 median rate storms per cycle with 95% confidence intervals using Bootstrap Method. As SC24 has been the least active solar cycle in over 200 years, we conclude that this method tends to overestimate geomagnetic storms occurrence rates even for small events.
Diagnostics of non-thermal-distributions from solar flare EUV line spectra
Authors: Dzifčáková Elena , Zemanová Alena , Dudík Jaroslav , Lörinčík Juraj 
Published: September 2020

AbstractSpectral line intensities observed by the Extreme Ultraviolet Variability Experiment (EVE) on board the Solar Dynamics Observatory (SDO) during 2012 March 9 M6.3 flare were used to diagnose a presence of a non-thermal electron distribution represented by a κ-distribution. The diagnosed electron densities ($\approx 2 \times {10^{11}}{\rm{c}}{{\rm{m}}^{ - 3}}$) are affected only a little by the presence of the non-thermal distribution, and are within the uncertainties of observation. On the other hand, the temperature diagnostics based on the line ratios involving different ionization degrees is strongly affected by the type of the electron distribution. The distribution functions diagnosed from relative Fe line intensities demonstrate the presence of strongly non-thermal distributions during the impulsive phase of the flare and later their gradual thermalization.
Early results from the solar-minimum 2019 total solar eclipse
Authors: Pasachoff Jay M. , Lockwood Christian A. , Inoue John L. , Meadors Erin N. , Voulgaris Aristeidis , Sliski David , Sliski Alan , Reardon Kevin P. , Seaton Daniel B. , Caplan Ronald M. , Downs Cooper , Linker Jon A. , Schneider Glenn , Rojo Patricio , Sterling Alphonse C. 
Published: September 2020

AbstractWe observed the 2 July 2019 total solar eclipse with a variety of imaging and spectroscopic instruments recording from three sites in mainland Chile: on the centerline at La Higuera, from the Cerro Tololo Inter-American Observatory, and from La Serena, as well as from a chartered flight at peak totality in mid-Pacific. Our spectroscopy monitored Fe X, Fe XIV, and Ar X lines, and we imaged Ar X with a Lyot filter adjusted from its original H-alpha bandpass. Our composite imaging has been compared with predictions based on modeling using magnetic-field measurements from the pre-eclipse month. Our time-differenced sites will be used to measure motions in coronal streamers.
Realistic 3D MHD modeling of self-organized magnetic structuring of the solar corona
Authors: Kitiashvili Irina N. , Wray Alan A. , Sadykov Viacheslav , Kosovichev Alexander G. , Mansour Nagi N. 
Published: September 2020

AbstractThe dynamics of solar magnetoconvection spans a wide range of spatial and temporal scales and extends from the interior to the corona. Using 3D radiative MHD simulations, we investigate the complex interactions that drive various phenomena observed on the solar surface, in the low atmosphere, and in the corona. We present results of our recent simulations of coronal dynamics driven by underlying magnetoconvection and atmospheric processes, using the 3D radiative MHD code StellarBox (Wray et al. 2018). In particular, we focus on the evolution of thermodynamic properties and energy exchange across the different layers from the solar interior to the corona.