bluuebunny/crossref_metadata_2025_split huggingface dataset:
An Asymmetric Keplerian Disk Surrounding the O-type Protostar IRAS 16547−4247
Authors: Zapata Luis A. , Garay Guido , Palau Aina , Rodríguez Luis F. , Fernández-López Manuel , Estalella Robert , Guzmán Andres 
Published: February 2019

Abstract
For the past few decades, there has been great interest in determining if even the most massive stars in our galaxy (namely the spectral O-type stars) are formed in a similar manner as the low- and intermediate-mass stars, that is, through the presence of accreting disks and powerful outflows. Here, using sensitive observations of the Atacama Large Millimeter/Submillimeter Array, we report a resolved Keplerian disk (with 15 synthesized beams across its major axis) surrounding the deeply embedded O-type protostar IRAS 16547−4247. The disk shows some asymmetries that could arise because the disk is unstable and fragmenting or because of different excitation conditions within the disk. The enclosed mass estimated from the disk Keplerian radial velocities is 25 ± 3 M
⊙. The molecular disk is at the base of an ionized thermal radio jet and is approximately perpendicular to the jet axis orientation. We additionally find the existence of a binary system of compact dusty objects at the center of the accreting disk, which indicates the possible formation of an O-type star and a companion of lower mass. This is not surprising due to the high binary fraction reported in massive stars. Subtracting the contribution of the dusty disk plus the envelope and the companion, we estimated a mass of 20 M
⊙ for the central star.
The Rotation-disk Connection in Young Brown Dwarfs: Strong Evidence for Early Rotational Braking
Authors: Moore Keavin , Scholz Aleks , Jayawardhana Ray 
Published: February 2019

Abstract
We use Kepler/K2 light curves to measure rotation periods of brown dwarfs and very low mass stars in the Upper Scorpius star-forming region. Our sample comprises a total of 104 periods. Depending on the assumed age of Upper Scorpius, about a third of them are for brown dwarfs. The median period is 1.28 day for the full sample and 0.84 day for the probable brown dwarfs. With this period sample, we find compelling evidence for early rotational braking in brown dwarfs, caused by the interaction between the central object and the disk. The median period for objects with disks is at least 50% longer than for those without. Two brown dwarfs show direct signs of “disk-locking” in their light curves, in the form of dips that recur on a timescale similar to the rotation period. Comparing the period samples for brown dwarfs at different ages, there is a clear need to include rotational braking into period evolution tracks between 1 and 10 Myr. A locked period over several Myr followed by spin-up due to contraction fits the observational data. We conclude that young brown dwarfs are affected by the same rotational regulation as stars, though they start off with significantly faster rotation, presumably set by initial conditions.
Asteroseismology of the Pre-main-sequence δ Scuti Pulsator IP Persei
Authors: Chen Xinghao , Li Yan 
Published: February 2019

Abstract
A grid of theoretical models are computed to fit the nine oscillation modes of IP Per detected earlier from a multi-site ground-based campaign. Fitting results show that there are two sets of theoretical models that could reproduce the observed frequencies more or less equally as well. In view of other available spectroscopic and photometric measurements, our best-fitting stellar parameters for IP Per are

km s−1,

,

M
⊙,

K,

,

dex,

R
⊙,

s, and age =

Myr. Meanwhile, IP Per is found to be a pre-main-sequence star where the CN cycle has not yet reached the equilibrium state. At present, 14% of C12 have been turned into N14. Based on the best-fitting model, f
6 is identified as a radial mode, f
1 and f
2 as two dipole modes, and f
3, f
4, f
5, f
7, f
8, and f
9 as six quadrupole modes.
Effects of Rotation and Magnetic Field on the Revival of a Stalled Shock in Supernova Explosions
Authors: Fujisawa Kotaro , Okawa Hirotada , Yamamoto Yu , Yamada Shoichi 
Published: February 2019

Abstract
We investigate axisymmetric steady solutions of (magneto)hydrodynamics equations that approximately describe accretion flows through a standing shock wave onto a protoneutron star and discuss the effects of rotation and magnetic field on the revival of the stalled shock wave in supernova explosions. We develop a new powerful numerical method to calculate the two-dimensional steady accretion flows self-consistently. We first confirm the results of preceding papers that there is a critical luminosity of irradiating neutrinos, above which there exists no steady solution in spherical models. If a collapsing star is rotating and/or has a magnetic field, the accretion flows are no longer spherical owing to the centrifugal force and/or Lorentz force, and the critical luminosity is modified. In fact, we find that the critical luminosity is reduced by about 50%–70% for very rapid rotations; the rotation frequencies are 0.2–0.45 s−1 at the radius of r = 1000 km (equivalent to spin periods ∼0.5–0.22 ms at r = 10 km) and about 20%–50% for strong toroidal magnetic fields (the strengths of which are 1.0 × 1012–3.0 × 1012 G at r = 1000 km), depending on the mass accretion rate. These results may also be interpreted as the existence of a critical specific angular momentum or critical magnetic field, above which there exists no steady solution and the standing shock wave will be revived for a given combination of mass accretion rate and neutrino luminosity.
Removal of Spectro-polarimetric Fringes by Two-dimensional Principal Component Analysis
Authors: Casini R. , Li W. 
Published: February 2019

Abstract
We investigate the application of two-dimensional Principal Component Analysis (2D PCA) to the problem of removal of polarization fringes from spectro-polarimetric data sets. We show how the transformation of the PCA basis through a series of carefully chosen rotations allows us to confine polarization fringes (and other stationary instrumental effects) to a reduced set of basis “vectors,” which at the same time are largely devoid of the spectral signal from the observed target. It is possible to devise algorithms for the determination of the optimal series of rotations of the PCA basis, thus opening the possibility of automating the procedure of defringing of spectro-polarimetric data sets. We compare the performance of the proposed method with the more traditional Fourier filtering of Stokes spectra.
Big Bang Nucleosynthesis with an Inhomogeneous Primordial Magnetic Field Strength
Authors: Luo Yudong , Kajino Toshitaka , Kusakabe Motohiko , Mathews Grant J. 
Published: February 2019

Abstract
We investigate the effect on the Big Bang nucleosynthesis (BBN) from the presence of a stochastic primordial magnetic field (PMF) whose strength is spatially inhomogeneous. We assume a uniform total energy density and a Gaussian distribution of field strength. In this case, domains of different temperatures exist in the BBN epoch due to variations in the local PMF. We show that in such a case, the effective distribution function of particle velocities averaged over domains of different temperatures deviates from the Maxwell–Boltzmann distribution. This deviation is related to the scale invariant strength of the PMF energy density ρ
Bc and the fluctuation parameter σ
B. We perform BBN network calculations taking into account the PMF strength distribution and deduce the element abundances as functions of the baryon-to-photon ratio η, ρ
Bc, and σ
B. We find that the fluctuations of the PMF reduce the 7Be production and enhance D production. We analyze the averaged thermonuclear reaction rates compared with those of a single temperature and find that the averaged charged-particle reaction rates are very different. Finally, we constrain the parameters ρ
Bc and σ
B from observed abundances of 4He and D and find that the 7Li abundance is significantly reduced. We also find that if the η value during BBN was larger than the present-day value due to a dissipation of the PMF or a radiative decay of exotic particles after BBN or if the stellar depletion of 7Li occurred, abundances of all light elements can be consistent with observational constraints.
Multi-wavelength Properties of Type 1 and Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey
Authors: Suh Hyewon , Civano Francesca , Hasinger Günther , Lusso Elisabeta , Marchesi Stefano , Schulze Andreas , Onodera Masato , Rosario David J. , Sanders David B. 
Published: February 2019

Abstract
We investigate the multi-wavelength properties of host galaxies of 3701 X-ray-selected active galactic nuclei (AGNs) out to z ∼ 5 in the Chandra-COSMOS Legacy Survey. Thanks to the extensive multi-wavelength photometry available in the COSMOS field, we derive AGN luminosities, host stellar masses, and star formation rates (SFRs) via a multi-component SED fitting technique. Type 1 and Type 2 AGNs follow the same intrinsic L
2–10 keV–L
6 μm relation, suggesting that mid-infrared emission is a reasonably good measure of the AGN accretion power regardless of obscuration. We find that there is a strong increase in Type 1 AGN fraction toward higher AGN luminosity, possibly due to the fact that Type 1 AGNs tend to be hosted by more massive galaxies. The AGN luminosity and SFR are consistent with an increase toward high stellar mass, while the M
stellar dependence is weaker toward the high-mass end, which could be interpreted as a consequence of quenching both star formation and AGN activity in massive galaxies. AGN host galaxies tend to have SFRs that are consistent with normal star-forming galaxies, independent of AGN luminosities. We confirm that black hole accretion rate and SFR are correlated up to z ∼ 5, when forming stars. The majority (∼73%) of our AGN sample are faint in the far-infrared, implying that the moderate-luminosity AGNs seem to be still active after the star formation is suppressed. It is not certain whether AGN activity plays a role in quenching the star formation. We conclude that both AGN activity and star formation might be more fundamentally related to host stellar mass.
The Large-scale Magnetic Field of a Thin Accretion Disk with Outflows
Authors: Li Jiawen , Cao Xinwu 
Published: February 2019

Abstract
The large-scale magnetic field threading an accretion disk plays an important role in launching jets/outflows. The field may probably be advected inward by the plasma in the accretion disk from the ambient environment (interstellar medium or a companion star). It has been suggested that the external field can be efficiently dragged inward in a thin disk with magnetic outflows. We construct a self-consistent global disk-outflow model in which the large-scale field is formed by the advection of the external field in the disk. The outflows are accelerated by this field corotating with the disk, which carries away most of the angular momentum of the disk and causes its structure to become significantly different from the conventional viscous disk structure. We find that the magnetic field strength in the inner region of the disk can be several orders of magnitude higher than the external field strength for a geometrically thin disk with H/R ∼0.1 if the ratio of the gas to magnetic pressure β
out ∼ 102 at the outer edge of the disk. The outflow velocity shows a layer-like structure, i.e., it decreases with radius where it is launched. The outflow can be accelerated up to ∼0.2–0.3c from the inner region of the disk, and the mass-loss rate in the outflows is ∼10%–70% of the mass accretion rate at the outer radius of the disk, which may account for the fast outflows that are observed in some active galactic nuclei.
Internal Gravity Waves in the Magnetized Solar Atmosphere. II. Energy Transport
Authors: Vigeesh G. , Roth M. , Steiner O. , Jackiewicz J. 
Published: February 2019

Abstract
In this second paper of the series on internal gravity waves (IGWs), we present a study of the generation and propagation of IGWs in a model solar atmosphere with diverse magnetic conditions. A magnetic field-free and three magnetic models that start with an initial, vertical, homogeneous field of 10, 50, and 100 G magnetic flux density, are simulated using the CO5BOLD code. We find that the IGWs are generated in similar manner in all four models in spite of the differences in the magnetic environment. The mechanical energy carried by IGWs is significantly larger than that of the acoustic waves in the lower part of the atmosphere, making them an important component of the total wave energy budget. The mechanical energy flux (106–103 W m−2) is a few orders of magnitude larger than the Poynting flux (103–101 W m−2). The Poynting fluxes show a downward component in the frequency range corresponding to the IGWs, which confirm that these waves do not propagate upward in the atmosphere when the fields are predominantly vertical and strong. We conclude that, in the upper photosphere, the propagation properties of IGWs depend on the average magnetic field strength and therefore these waves can be potential candidates for magnetic field diagnostics of these layers. However, their subsequent coupling to Alfvénic waves is unlikely in a magnetic environment permeated with predominantly vertical fields, and therefore they may not directly or indirectly contribute to the heating of layers above plasma-β less than 1.
In Search of the Thermal Eccentricity Distribution
Authors: Geller Aaron M. , Leigh Nathan W. C. , Giersz Mirek , Kremer Kyle , Rasio Frederic A. 
Published: February 2019

Abstract
About a century ago, Jeans (1919) discovered that if binary stars reach a state approximating energy equipartition, for example, through many dynamical encounters that exchange energy, their eccentricity distribution can be described by

. This is referred to as the thermal eccentricity distribution, and has been widely used for initial conditions in theoretical investigations of binary stars. However, observations suggest that the eccentricity distributions of most observed binaries, and particularly those with masses ≲5 M
⊙, are flatter than thermal and follow more closely to a uniform distribution. Nonetheless, it is often argued that dynamical interactions in a star cluster would quickly thermalize the binaries, which could justify imposing a thermal eccentricity distribution at birth for all binaries. In this paper, we investigate the validity of this assumption. We develop our own rapid semi-analytic model for binary evolution in star clusters, and also compare it with detailed N-body and Monte Carlo star cluster models. We show that, for nearly all binaries, dynamical encounters fail to convert an initially uniform eccentricity distribution to thermal within a star cluster’s lifetime. Thus, if a thermal eccentricity distribution is observed, it is likely imprinted upon formation rather than through subsequent long-term dynamical processing. Theoretical investigations that initialize all binaries with a thermal distribution will make incorrect predictions for the evolution of the binary population. Such models may overpredict the merger rate for binaries with modest orbital separations by a factor of about two.
Surveys of Clumps, Cores, and Condensations in Cygnus X. I. A New Catalog of ∼0.1 pc Massive Dense Cores
Authors: Cao 曹 Yue 越 , Qiu Keping , Zhang Qizhou , Wang Yuwei , Hu Bo , Liu Junhao 
Published: February 2019

Abstract
Using infrared to (sub)millimeter data from Spitzer, Herschel, the James Clerk Maxwell Telescope, and the IRAM 30 m telescope, we conducted an unbiased survey of the massive dense cores (MDCs) in the Cygnus X molecular cloud complex, aimed at characterizing the physical conditions of high-mass star formation (HMSF) at ∼0.1 pc scales. We created 5° × 6° images of the 70–1200 μm dust continuum, gas column density, and dust temperature of Cygnus X. A spatial relation between the dense regions (A
v ≥ 15) and the developed H ii regions was found, indicating the impact of the latter on the global structures of Cygnus X. With a 35 M
⊙ mass threshold implied by HMSF signposts, we identified 151 MDCs with sizes of ∼0.1 pc, masses of 35–1762 M
⊙, and temperatures of 8–35 K. Our MDC sample is statistically complete in Cygnus X and is three times larger than that in Motte et al. The MDCs were classified into IR-bright/IR-quiet ones based on their midinfrared fluxes, and a large “IR-quiet” proportion (90%) was found in our sample. Two possible scenarios were proposed to interpret accelerated HMSF and the incapability of HMSF of the IR-quiet MDCs. We also found 26 starless MDCs by their lack of compact emissions at 21–70 μm wavelengths, of which the most massive ones are probably the best candidates of initial HMSF sites in Cygnus X.
(Trans)gender outlaws?
Authors: rose hartline france 
Published: February 2019

Abstract
In July 2016, Norway enacted a law that allows for one to determine one’s juridical gender without the previously required medical sterilisation. Widely heralded as a significant step toward complete gender equality, this was seen by many as finally resulting in legal equality for those who are trans. However, the law’s potential to empower the trans movement may be quite limited, given the lack of options outside the male/female binary and the absence of improved access to gender-confirming medical technologies. Such limitations, this article argues, preclude the law from either sufficiently addressing the needs of many transpeople or meaningfully challenging prevailing gender norms. How, then, can the law be celebrated as a landmark achievement for trans rights in Norway? This article seeks to explain the apparent contradiction by considering the law’s founding principles as they apply to the trans political landscape in Norway, in order to illustrate how the law’s inception and application have been informed by particular interpretations of identity, gender, and sex. Moreover, it analyses the potential impact of the law’s shortcomings on the people for whom it was meant to represent, using a queer analytical approach to understand how the law can empower some trans whilst further marginalising others.
Response to Anti–PD-1 in Uveal Melanoma Without High-Volume Liver Metastasis
Authors: Johnson Douglas B. , Bao Riyue , Ancell Kristin K. , Daniels Anthony B. , Wallace Deborah , Sosman Jeffrey A. , Luke Jason J. 
Published: February 2019

Background: Uveal melanoma (UM) is an uncommon melanoma subtype with poor prognosis. Agents that have transformed the management of cutaneous melanoma have made minimal inroads in UM. Methods: We conducted a single-arm phase II study of pembrolizumab in patients with metastatic UM and performed bioinformatics analyses of publicly available datasets to characterize the activity of anti–PD-1 in this setting and to understand the mutational and immunologic profile of this disease. Results: A total of 5 patients received pembrolizumab in this study. Median overall survival was not reached, and median progression-free survival was 11.0 months. One patient experienced a complete response after one dose and 2 others experienced prolonged stable disease (20% response rate, 60% clinical benefit rate); 2 additional patients had rapidly progressing disease. Notably, the patients who benefited had either no liver metastases or small-volume disease, whereas patients with rapidly progressing disease had bulky liver involvement. We performed a bioinformatics analysis of The Cancer Genome Atlas for UM and confirmed a low mutation burden and low rates of T-cell inflammation. Note that the lack of T-cell inflammation strongly correlated with MYC pathway overexpression. Conclusions: Anti–PD-1–based therapy may cause clinical benefit in metastatic UM, seemingly more often in patients without bulky liver metastases. Lack of mutation burden and T-cell infiltration and MYC overexpression may be factors limiting therapeutic responses.ClinicalTrials.gov identifier: NCT02359851
SPECTROSCOPICALLY AND/OR STRUCTURALLY INTRIGUING PHTHALOCYANINES AND RELATED COMPOUNDS. PART 1. MONOMERIC SYSTEMS
Authors: Kobayashi Nagao 
Published: February 2019

The first part of the series of review papers on the properties of some synthetically and spectroscopically interesting studies of our group for the period 2007-2017 is presented. In particular, examples are shown on the analysis of spectroscopic data in conjunction with molecular orbital (MO) calculations. We have used mainly electronic absorption and natural and magnetic circular dichroism (CD and MCD) spectroscopic techniques, with occasional use of fluorescence, phosphorescence, and time-resolved EPR. Not only the spectra of (4n + 2)π systems, but also some 4nπ anti-aromatic systems are theoretically analyzed, which helps the reader to learn how to interprete the spectral data. In the first part and the second part of this review monomer systems are considered, and in the third - trimeric and tetrameric systems. <span style="opacity: 0;"> . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . </span>
ЗАЩИТА СТАЛИ ОТ КОРРОЗИИ В КИСЛЫХ СРЕДАХ ИНГИБИТОРАМИ «СОЛИНГ» ПРИ ПОВЫШЕННЫХ ТЕМПЕРАТУРАХ
Authors: Menshikov I.A. , Lukyanova N.V. , Shein A.B. 
Published: February 2019

В работе приведены результаты исследования защитного действия ряда ингибирующих композиций серии «СолИнг» на основе ацетиленовых спиртов и их смесей с азотсодержащими соединениями различного типа в растворах серной и соляной кислот в интервале температур 20-600С. Электрохимические исследования выполнены на малоуглеродистой стали Ст3. Поляризационные кривые снимали в трехэлектродной ячейке ходом из катодной области в анодную со скоростью развертки потенциала 10 мВ/мин, используя электрохимический измерительный комплекс SOLARTRON 1280 C. Исследованы защитные композиции: СолИнг ИК-1 на основе ненасыщенного спирта в смеси с серосодержащим амидом в водной среде; СолИнг ИК-2 на основе ненасыщенного спирта с добавками четвертичной соли аммония и комплексона; СолИнг ИК-3 на основе ненасыщенного спирта в системе органических растворителей, а также СолИнг ИК-4(А) на основе высокомолекулярного азотсодержащего ПАВ (молекулярной массы от 300 до 400) с добавками ненасыщенного спирта в системе органических растворителей и СолИнг ИК-4(Б) на основе высокомолекулярного азотсодержащего ПАВ с молекулярной массой до 300.Установлено, что во всём исследованном диапазоне температур композиции СолИнг ИК-2, ИК-4(А) и ИК-4(Б) обладают высоким защитным эффектом, что говорит об устойчивости адсорбционных слоёв ингибитора с повышением температуры. Композиции ИК-1 и ИК-3 обладают меньшим защитным эффектом, но в целом рост температуры не оказывает сильного негативного влияния на величину защитного эффекта. Устойчивость исследуемых композиций объясняется наличием в их составе ненасыщенных спиртов, проявляющих высокие защитные характеристики при повышенных температурах. На основе полученных результатов были рассчитаны эффективные энергии активации коррозионного процесса.