bluuebunny/crossref_metadata_2025_split huggingface dataset:
The relationship between depression with anxious distress DSM-5 specifier and mixed depression: a network analysis
Authors: Tundo Antonio , Musetti Laura , Del Grande Claudia , de Filippis Rocco , Proietti Luca , Marazziti Donatella , Gibertoni Dino , Dell’Osso Liliana 
Published: March 2020

AbstractIntroductionEpidemiological, clinical, and treatment response characteristics of major depression with anxious distress (ADS) are quite similar to those of mixed depression, but no study investigated the symptom interplay of these conditions.ObjectiveTo analyze the correlations among symptom criteria for major depression with ADS and for mixed depression using a network analysis.MethodsTwo hundred and forty-one outpatients with major depression were consecutively recruited. DSM-5 criteria for major depression with ADS or with mixed features (MF) and Koukopoulos’ criteria for mixed depression (MXD) were assessed using a structured clinical interview.ResultsA total of 58.9% of patients met DSM-5 criteria for major depression with ADS, 48.5% for MXD, and 2.5% for major depression with MF, so that the symptoms of this specifier were excluded from the network analysis. The most frequent symptoms were difficulty concentrating due to worries (57.7%), feeling keyed up or on edge (51%) (major depression with ADS), and psychic agitation or inner tension (51%) (MXD). Psychic agitation or inner tension had a central position in the network and bridged MXD to major depression with ADS through feeling keyed up or on edge.ConclusionsCriteria for major depression with ADS and for MXD are partially overlapping, with psychic agitation or inner tension and feeling keyed up or on edge that feature in both conditions and are difficult to distinguish in clinical practice. The clarification of the relationship between these two psychopathological conditions could bring important implications for diagnosis, prognosis, and treatment of depressive episodes.
Silent cyber assessment framework
Authors: Cartagena S. , Gosrani V. , Grewal J. , Pikinska J. 
Published: March 2020

Abstract
The (re)insurance industry is faced with a growing risk related to the development of information technology (IT). This growth is creating an increasingly digitally interconnected world with more and more dependence being placed on IT systems to manage processes. This is generating opportunities for new insurance products and coverages to directly address the risks that companies face. However, it is also changing the risk landscape of existing classes of business within non-life insurance where there is inherent risk of loss as a result of IT events that cannot be or have not been excluded in policy wordings or are changing the risk profile of traditional risks. This risk of losses to non-cyber classes of business resulting from cyber as a peril that has not been intentionally included (often by not clearly excluding it) is defined as non-affirmative cyber risk, and the level of understanding of this issue and the cyber peril exposure from non-cyber policies varies across the market. In contract wordings, the market has remained relatively “silent” across most lines of business about potential losses resulting from IT-related events, either by not addressing the potential issue or excluding via exclusions. Some classes of business recognise the exposure by use of write-backs. Depending on the line of business, the approach will vary as to how best to turn any “silent” exposure into a known quantity either by robust exclusionary language, pricing or exposure monitoring. This paper proposes a framework to help insurance companies address the issue of non-affirmative cyber risk across their portfolios. Whilst the framework is not intended to be an all-encompassing solution to the issue, it has been developed to help those tasked with addressing the issue to be able to perform a structured analysis of the issue. Each company’s analysis will need to tailor the basis of the framework to fit their structure and underwriting procedures. Ultimately, the framework should be used to help analysts engage with management on this issue so that the risk is understood, and any risk mitigation actions can be taken if required. In the appendix, we present a worked example to illustrate how companies could implement the framework. The example is entirely fictional, is focused on non-life specialty insurance, and is intended only to help demonstrate one possible way in which to apply the framework.
Review of asteroid-family and meteorite-type links
Authors: Jenniskens Peter 
Published: March 2020

AbstractThe materials of large asteroids and asteroid families are sampled by meteorites that fall to Earth. The cosmic ray exposure age of the meteorite identifies the collision event from which that meteorite originated. The inclination of the orbit on which the meteoroid impacted Earth measures the inclination of the source region, while the semi-major axis of the orbit points to the delivery resonance, but only in a statistical sense. To isolate the sources of our meteorites requires multiple documented falls for each cosmic ray exposure peak. So far, only 36 meteorites have been recovered from observed falls. Despite these low numbers, some patterns are emerging that suggest CM chondrites originated from near the 3:1 resonance from a low-inclined source (perhaps the Sulamitis family), LL chondrites came to us from the ν6 resonance (perhaps the Flora family), there is an H chondrite source at high inclination (Phocaea?), and one group of low shock-stage L chondrites originates from the inner main belt. Other possible links are discussed.
The Near Earth Asteroid associations
Authors: Jopek Tadeusz J. 
Published: March 2020

AbstractWe searched for associations (not for families) amongst the near Earth asteroids (NEAs) and, similarly as in our previous studies (Jopek 2011; Jopek 2015),AQ: Please provide reference detail for Jopek 2012. a dozen groups of 10 or more members was found with high statistical reliability. We present some details of our most numerous finding: association (2061) Anza which, at the moment, incorporates 191 members.
Trojans distribution in the Solar system
Authors: Kazantsev Anatolii , Kazantseva Lilia 
Published: March 2020

AbstractOrbits of potential Trojans of different planets in the solar system were selected from the MPC catalog on February, 2017. The evolution of those orbits was calculated. The bodies on librating orbits around the points L4 and L5 were determined. The quantities of real Trojans in the MPC catalog are as follows: Mars - 5, Jupiter - over 4500, Saturn - none, Uranus - 2, Neptune - 15. A reasoned explanation of such distribution of Trojans in the solar system is proposed.
Photometry and spin rates of 4 NEAs recently observed by the Mexican Asteroid Photometry Campaign
Authors: Saucedo J. C. , Ayala-Gómez S. A. , Contreras M. E. , Haro-Corzo S. A. R. , Loera-González P. A. , Olgun L. , Valdés-Sada P. A. 
Published: March 2020

AbstractWe present photometric observations of (4055) Magellan, (143404) 2003 BD44, 2014 JO25 and (3122) Florence, four potentially hazardous Near Earth Asteroids (NEAs). The data were taken near their approaches to Earth by 3 observatories participating in the Mexican Asteroid Photometry Campaign (CMFA). The results obtained: light curves, spin rates, amplitudes and errors, are in general agreement with those obtained by others. During the day of a NEAs maximum approach to our planet, its light curve may present significant changes. In the spin rate, however, only minute changes are observed. 2014 JO25 is briefly discussed in this regard.
Prevalence of radio jets associated with quasar outflows and feedback
Authors: Jarvis Miranda E. 
Published: March 2020

AbstractWe have identified that radio jets are commonly associated with “radiative mode” feedback in quasars. By performing a systematic multi-wavelength study of z < 0.2 quasars, we have found that 70–80% of our sample of ‘radio-quiet’ type 2 quasars, which host kpc-scale ionized gas outflows, exhibit radio jet structures. Here, we discuss our results on the pilot sample of 10 objects that combine high resolution (∼ 0.25 - 1 arcsec) radio imaging at 1-7 GHz with optical IFU observations. Our results demonstrate that it is extremely common for jets to be spatially and kinematically linked to kpc-scale ionized gas kinematics in such quasars. Therefore, radio jets may be an important driver of outflows during ‘radiative mode’ feedback, apparently blurring the lines between the traditional divisions of feedback modes.
The intermediate-power population of radio galaxies: morphologies and interactions
Authors: Worrall Diana M. , Duffy Ryan T. , Birkinshaw Mark 
Published: March 2020

AbstractRadio galaxies of intermediate power dominate the radio-power injection in the Universe as a whole, due to the break in the radio luminosity function, and so are of special interest. The population spans FR I, FR II, and hybrid morphologies, resides in a full range of environmental richness, and sources of all ages are amenable to study. We describe structures and interactions, with emphasis on sources with deep high-resolution Chandra X-ray data. As compared with low-power sources there is evidence that the physics changes, and the work done in driving shocks can exceed that in evacuating cavities. A range of morphologies and phenomena is identified.
Dust and polarization of cold clumps
Authors: Juvela Mika 
Published: March 2020

AbstractThe Planck catalogue of Galactic cold clumps, PGCC, contains sources of ongoing and future star formation. The data show clear variations also in their dust properties.We use Planck polarization measurements to investigate the polarization fraction in PGCC clumps and the relative orientation of filamentary structures and magnetic fields (Alina et al. 2017). The decrease of polarization fraction as a function of column density can be related to the field geometry but also suggest some loss of grain alignment.PGCCs have been studied with ground-based observations (Liu et al. 2018). The first SCUBA-2/POL-2 polarization studies have targeted the infrared dark cloud G35.39-0.33. The magnetic field is found to be mostly perpendicular to the main filament. The plane-of-the-sky field strength is
$\sim 50\mu \,{\rm{G}}$
, a noticeable support against gravity. The polarization fraction decreases with increasing column density. This matches predictions of RAT grain alignment models but the relative contribution of the field morphology is hard to quantify (Juvela et al. 2018).We continue to use MHD simulations to study the same phenomena, with synthetic observations of clumps and filaments.
Signposts of shock-induced magnetic field compression in star-forming environments
Authors: Wiesemeyer Helmut 
Published: March 2020

AbstractIn star-forming environments, shock-compressed magnetic fields occur in cloud-cloud collisions, in molecular clouds exposed to supernova remnants (SNRs), and in photo-dissociation regions (PDRs). Besides their dynamical role, they increase the cosmic ray flux above the Galactic average, and the trapped particles contribute to the heating of the shocked gas. The associated dust emission is polarized perpendicularly to the sky plane projection of the field, Bsky. In edge-on viewed shock planes, highly ordered polarization patterns are expected. In search of such a signature, the dust emission from the Orion bar (a prototypical PDR) and from a molecular cloud/SNR interface (IC443-G) was studied with a λ870μm polarimeter at the APEX (Wiesemeyer etal 2014 and references therein). While our polarization map of OMC1 confirms the hourglass shape of Bsky (e.g., Schleuning 1998, Houde etal 2004), a deep integration towards the Orion bar reveals an alignment of Bsky with the shock forming in response to the wind and to the ionizing radiation from the Trapezium cluster (Fig. 1). This structure suggests a compressed magnetic field accelerating cosmic-ray particles, a scenario proposed by [Pellegrini et al. (2009)] to explain the high excitation temperature of rotationally warm H2 and CO (Shaw et al. 2009, Peng et al. 2012, respectively).
Observations of magnetic fields in Herbig Ae/Be stars
Authors: Schöller Markus , Hubrig Swetlana 
Published: March 2020

AbstractModels of magnetically driven accretion reproduce many observational properties of T Tauri stars. For the more massive Herbig Ae/Be stars, the corresponding picture has been questioned lately, in part driven by the fact that their magnetic fields are typically one order of magnitude weaker. Indeed, the search for magnetic fields in Herbig Ae/Be stars has been quite time consuming, with a detection rate of about 10% (e.g. Alecian et al. 2008), also limited by the current potential to detect weak magnetic fields. Over the last two decades, magnetic fields were found in about twenty objects (Hubrig et al. 2015) and for only two Herbig Ae/Be stars was the magnetic field geometry constrained. Ababakr, Oudmaijer & Vink (2017) studied magnetospheric accretion in 56 Herbig Ae/Be stars and found that the behavior of Herbig Ae stars is similar to T Tauri stars, while Herbig Be stars earlier than B7/B8 are clearly different. The origin of the magnetic fields in Herbig Ae/Be stars is still under debate. Potential scenarios include the concentration of the interstellar magnetic field under magnetic flux conservation, pre-main-sequence dynamos during convective phases, mergers, or common envelope developments. The next step in this line of research will be a dedicated observing campaign to monitor about two dozen HAeBes over their rotation cycle.
Seeking for magnetic fields in rotating disk/jets with ALMA polarimetry
Authors: Bacciotti Francesca , Girart Josep Miquel , Padovani Marco 
Published: March 2020

AbstractThe Atacama Large Millimeter/submillimeter Array (ALMA) is providing important advances in studies of star formation. In particular, polarimetry can reveal the disk magnetic configuration, a crucial ingredient in many processes, as, for example, the transport of angular momentum. We analized ALMA Band 7 (870 μm) polarimetric data at 0.”2 resolution for the young rotating disk/jet systems DG Tau and CW Tau, to find magnetic signatures. From the Stokes I, U, Q maps, we derive the linear polarization intensity,
$P = \sqrt {{Q^2} + {U^2}} $
, the linear polarization fraction, and the polarization angle. The alignment of the latter with the disk minor axis (Fig. 1) shows that self-scattering of dust thermal emission rather than magnetic alignment dominates the polarization in both targets (Bacciotti et al. 2018). However, several dust properties can be diagnosed comparing the polarization data with the models of self-scattering (e.g. Kataoke et al. 2017, Yang et al. 2017). The maximum grain size turns out to be in the range 50 - 70 μm for DG Tau and 100 - 150 μm for CW Tau. The asymmetry of the polarized intensity in DG Tau, observed for the first time around a T Tauri star, indicates that the disk is flared. Moreover, the observed belt-like feature may betray the presence of a disk substructure. In contrast, the polarization maps of CW Tau indicate that here the grains have settled to the disk midplane. Polarimetry is thus very important in studies of the dust evolution.
The accretion process in the magnetic Herbig Ae star HD 104237
Authors: Schöller Markus , Pogodin Mikhail A. 
Published: March 2020

AbstractAfter successfully retrieving the known rotation period P = 42.076 d in the Herbig Ae star HD 101412 using spectroscopic signatures of accretion tracers (Schöller et al.2016), we have studied magnetospheric accretion in the Herbig Ae SB2 system HD 104237 using spectroscopic parameters of the He i 10830, Paγ, and He i 5876 lines, formed in the accretion region. Employing 21 spectra obtained with ISAAC and X-shooter, we found that the temporal behavior of these parameters can be explained by a variable amount of matter being accreted in the region between the star and the observer. Using a periodogram analysis, we examined the possible origin of the accretion flow in HD 104237 and considered the following four scenarios: matter flows from the circumbinary envelope, mass exchange between the system’s components, magnetospheric accretion (MA) from the disk onto the star, and fast high-latitude accretion from a disk wind onto a weakly magnetized star. Based on a correlation analysis, we were able to show that the primary component is responsible for the observed emission line spectrum of the system. Since we do not find any correlation of the spectroscopic parameters with the phase of the orbital period (P ≍ 20 d), we can reject the first two scenarios. We found a variation period of about 5 d, which likely represents the stellar rotation period of the primary and favors the MA scenario.
Magnetic fields and massive star formation
Authors: Zhang Qizhou 
Published: March 2020

AbstractMassive stars (
${\rm{M}} > \,8{M_ \odot }$
) often form in parsec-scale molecular clumps that collapse and fragment, leading to the birth of a cluster of stellar objects. The role of magnetic fields during the formation of massive dense cores is still not clear. The steady improvement in sensitivity of (sub)millimeter interferometers over the past decade enabled observations of dust polarization of large samples of massive star formation regions. We carried out a polarimetric survey with the Submillimeter Array of 14 massive star forming clumps in continuum emission at a wavelength of 0.89 mm. This unprecedentedly large sample of massive star forming regions observed by a submillimeter interferometer before the advent of ALMA revealed compelling evidence of strong magnetic influence on the gas dynamics from 1 pc to 0.1 pc scales. We found that the magnetic fields in dense cores tend to be either parallel or perpendicular to the mean magnetic fields in their parental molecular clumps. Furthermore, the main axis of protostellar outflows does not appear to be aligned with the mean magnetic fields in the dense core where outflows are launched. These findings suggest that from 1 pc to 0.1 pc scales, magnetic fields are dynamically important in the collapse of clumps and the formation of dense cores. From the dense core scale to the accretion disk scale of ∼102 au, however, gravity and angular momentum appear to be more dominant relative to the magnetic field.
On the History and Present Situation
Authors: Peebles P. J. E. 
Published: March 2020

AbstractA common thought in the 1950s was that galaxies rotate because they are remnants of primeval currents, as in turbulence. But this idea is quite unacceptable in an expanding universe described by general relativity theory. Since we are no smarter now than in the 1950s the lesson I draw is that we do well on occasion to pause to consider whether we might be missing something. An example is the pure disk galaxies that are so common nearby and so rare in simulations. We have something to learn from this.
Emerging Angular Momentum Physics from Kinematic Surveys
Authors: Colless Matthew 
Published: March 2020

AbstractI review the insights emerging from recent large kinematic surveys of galaxies at low redshift, with particular reference to the SAMI, CALIFA and MaNGA surveys. These new observations provide a more comprehensive picture of the angular momentum properties of galaxies over wide ranges in mass, morphology and environment in the present-day universe. I focus on the distribution of angular momentum within galaxies of various types and the relationship between mass, morphology and specific angular momentum. I discuss the implications of the new results for models of galaxy assembly.
The Fundamental Physics of Angular Momentum Evolution in a ΛCDM Scenario
Authors: Pedrosa Susana 
Published: March 2020

AbstractGalaxy formation is a very complex process in which many different physical mechanisms intervene. Within the LCDM paradigm processes such as gas inflows and outflows, mergers and interactions contribute to the redistribution of the angular momentum content of the structures. Recent observational results have brought new insights and also triggered several theoretical studies. Some of these new contributions will be analysed here.
Magnetism in the Early Universe
Authors: Kahniashvili Tina , Brandenburg Axel , Kosowsky Arthur , Mandal Sayan , Roper Pol Alberto 
Published: March 2020

AbstractBlazar observations point toward the possible presence of magnetic fields over intergalactic scales of the order of up to ∼1 Mpc, with strengths of at least ∼10−16 G. Understanding the origin of these large-scale magnetic fields is a challenge for modern astrophysics. Here we discuss the cosmological scenario, focussing on the following questions: (i) How and when was this magnetic field generated? (ii) How does it evolve during the expansion of the universe? (iii) Are the amplitude and statistical properties of this field such that they can explain the strengths and correlation lengths of observed magnetic fields? We also discuss the possibility of observing primordial turbulence through direct detection of stochastic gravitational waves in the mHz range accessible to LISA.
Constraining magnetic fields in galaxy clusters
Authors: Bonafede Annalisa , Stuardi Chiara , Savini Federica , Vazza Franco , Brüggen Marcus 
Published: March 2020

AbstractMagnetic fields originate small-scale instabilities in the plasma of the intra-cluster medium, and may have a key role to understand particle acceleration mechanisms. Recent observations at low radio frequencies have revealed that synchrotron emission from galaxy clusters is more various and complicated than previously thought, and new types of radio sources have been observed. In the last decade, big steps forward have been done to constrain the magnetic field properties in clusters thanks to a combined approach of polarisation observations and numerical simulations that aim to reproduce Faraday Rotation measures of sources observed through the intra-cluster medium. In this contribution, I will review the results on magnetic fields reached in the last years, and I will discuss the assumptions that have been done so far in light of new results obtained from cosmological simulations. I will also discuss how the next generation of radio instruments, as the SKA, will help improving our knowledge of the magnetic field in the intra-cluster medium.
Large-scale transport of solar and stellar magnetic flux
Authors: Işık Emre 
Published: March 2020

AbstractSurface flux transport (SFT) models have been successful in reproducing how magnetic flux at the solar photosphere evolves on large scales. SFT modelling proved to be useful in reconstructing secular irradiance variations of the Sun, and it can be potentially used in forward modelling of brightness variations of Sun-like stars. We outline our current understanding of solar and stellar SFT processes, and suggest that nesting of activity can play an important role in shaping large-scale patterns of magnetic fields and brightness variability.
Solar Irradiance: Instrument-Based Advances
Authors: Kopp Greg 
Published: March 2020

AbstractVariations of the total solar irradiance (TSI) over long periods of time provide natural Earth-climate forcing and are thus important to monitor. Variations over a solar cycle are at the 0.1 % level. Variations on multi-decadal to century timescales are (fortunately for our climate stability) very small, which drives the need for highly-accurate and stable measurements over correspondingly long periods of time to discern any such irradiance changes. Advances to TSI-measuring space-borne instruments are approaching the desired climate-driven measurement accuracies and on-orbit stabilities. I present a summary of the modern-instrument improvements enabling these measurements and present some of the solar-variability measurement results from recent space-borne instruments, including TSI variations on timescales from solar flares and large-scale convection to solar cycles.