bluuebunny/crossref_metadata_2025_split huggingface dataset:
Ultracool Dwarfs Observed with the Spitzer Infrared Spectrograph. I. An Accurate Look at the L-to-T Transition at ∼300 Myr from Optical Through Mid-infrared Spectrophotometry
Authors: Suárez Genaro , Metchev Stanimir , Leggett Sandy K. , Saumon Didier , Marley Mark S. 
Published: October 2021

Abstract
We present Spitzer IRS 5–14 μm spectra and 16 μm and 22 μm photometry of the T2.5 companion to the ∼300 Myr old G0V star HN Peg. We incorporate previous 0.8–5 μm observations to obtain the most comprehensive spectral energy distribution (SED) of an intermediate-gravity L/T-transition dwarf that, together with an accurate Gaia EDR3 parallax of the primary, enables us to derive precise fundamental parameters. We find that young (≈0.1–0.3 Gyr) early-T dwarfs on average have ≈140 K lower effective temperatures, ≈20% larger radii, and similar bolometric luminosities compared to ≳1 Gyr old field dwarfs with similar spectral types. Our accurate infrared spectrophotometry offers new detail at wavelengths where the dominant carbon-bearing molecules have their strongest transitions: at 3.4 μm for methane and at 4.6 μm for carbon monoxide. We assess the performance of various widely available photospheric models and find that models with condensates and/or clouds better reproduce the full SED of this moderately young early-T dwarf. However, cloud-free models incorporating a more general convective instability treatment reproduce at least the low-resolution near-infrared spectrum similarly well. Our analysis of R ≈ 2300 J-band spectra shows that the near-infrared potassium absorption lines in HN Peg B have similar strengths to those seen in both younger and older T2–T3 dwarfs. We conclude that while alkali lines are well established as surface gravity indicators for L-type or warmer stars, they are insensitive to surface gravity in early-T dwarfs.
Survival Times of Supramassive Neutron Stars Resulting from Binary Neutron Star Mergers
Authors: Beniamini Paz , Lu Wenbin 
Published: October 2021

Abstract
A binary neutron star (BNS) merger can lead to various outcomes, from indefinitely stable neutron stars, through supramassive neutron stars (SMNSs) or hypermassive neutron stars supported only temporarily against gravity, to black holes formed promptly after the merger. Up-to-date constraints on the BNS total mass and the neutron star equation of state suggest that a long-lived SMNS may form in ∼0.45–0.9 of BNS mergers. A maximally rotating SMNS needs to lose ∼(3–6) × 1052 erg of its rotational energy before it collapses, on a fraction of the spin-down timescale. An SMNS formation imprints on the electromagnetic counterparts to the BNS merger. However, a comparison with observations reveals tensions. First, the distribution of collapse times is too wide and that of released energies too narrow (and the energy itself too large) to explain the observed distributions of internal X-ray plateaus, invoked as evidence for SMNS-powered energy injection. Second, the immense energy injection into the blast wave should lead to extremely bright radio transients, which previous studies found to be inconsistent with deep radio observations of short gamma-ray bursts (GRBs). Furthermore, we show that upcoming all-sky radio surveys will constrain the extracted energy distribution, independently of a GRB jet formation. Our results can be self-consistently understood, provided that most BNS merger remnants collapse shortly after formation (even if their masses are low enough to allow for SMNS formation). This naturally occurs if the remnant retains half or less of its initial energy by the time it enters solid-body rotation.
Planck Galactic Cold Clumps at High Galactic Latitude—a Study with CO Lines
Authors: Xu Fengwei , Wu Yuefang , Liu Tie , Liu Xunchuan , Zhang Chao , Esimbek Jarken , Qin Sheng-Li , Li Di , Wang Ke , Yuan Jinghua , Meng Fanyi , Zhang Tianwei , Eden David , Tatematsu K. , Evans Neal J. , Goldsmith Paul. F. , Zhang Qizhou , Henkel C. , Yi Hee-Weon , Lee Jeong-Eun , Saajasto Mika , Kim Gwanjeong , Juvela Mika , Sahu Dipen , Hsu Shih-Ying , Liu Sheng-Yuan , Dutta Somnath , Lee Chin-Fei , Zhang Chuan-Peng , Xu Ye , Ju Binggang 
Published: October 2021

Abstract
Gas at high Galactic latitude is a relatively little noticed component of the interstellar medium. In an effort to address this, 41 Planck Galactic Cold Clumps at high Galactic latitude (HGal; ∣b∣ > 25°) were observed in 12CO, 13CO, and C18O J = 1−0 lines, using the Purple Mountain Observatory 13.7 m telescope. 12CO (1−0) and 13CO (1−0) emission was detected in all clumps, while C18O (1−0) emission was only seen in 16 clumps. The highest and average latitudes are 71.°4 and 37.°8, respectively. Fifty-one velocity components were obtained, and then each was identified as a single clump. Thirty-three clumps were further mapped at 1′ resolution, and 54 dense cores were extracted. Among dense cores, the average excitation temperature T
ex of 12CO is 10.3 K. The average line widths of thermal and nonthermal velocity dispersions are 0.19 and 0.46 km s−1, respectively, suggesting that these cores are dominated by turbulence. Distances of the HGal clumps given by Gaia dust reddening are about 120–360 pc. The ratio of X
13/X
18 is significantly higher than that in the solar neighborhood, implying that HGal gas has a different star formation history compared to the gas in the Galactic disk. HGal cores with sizes from 0.01 to 0.1 pc show no notable Larson’s relation, and the turbulence remains supersonic down to a scale of slightly below 0.1 pc. None of the HGal cores that bear masses from 0.01 to 1 M
⊙ are gravitationally bound, and all appear to be confined by outer pressure.
Is Flare Ribbon Fine Structure Related to Tearing in the Flare Current Sheet?
Authors: Wyper P. F. , Pontin D. I. 
Published: October 2021

Abstract
Observations of solar flare ribbons show significant fine structure in the form of breaking wavelike perturbations and spirals. The origin of this structure is not well understood, but one possibility is that it is related to the tearing instability in the flare current sheet. Here we study this connection by constructing an analytical 3D magnetic field representative of an erupting flux rope with a flare current sheet below it. We introduce small-scale flux ropes representative of those formed during a tearing instability in the current layer, and use the squashing factor on the solar surface to identify the shape of the presumed flare ribbons and fine structure. Our analysis suggests there is a direct link between flare ribbon fine structure and flare current sheet tearing, with the majority of the ribbon fine structure related to oblique tearing modes. Depending upon the size, location, and twist of the small-scale flux ropes, breaking wavelike and spiral features within the hooks and straight sections of the flare ribbon can be formed that are qualitatively similar to observations. We also show that the handedness of the spirals/waves must be the same as the handedness of the hooks of the main ribbon. We conclude that tearing in the flare current layer is a likely explanation for spirals and wavelike features in flare ribbons.
“Ashfall” Induced by Molecular Outflow in Protostar Evolution
Authors: Tsukamoto Yusuke , Machida Masahiro N. , Inutsuka Shu-ichiro 
Published: October 2021

Abstract
Dust growth and its associated dynamics play key roles in the first phase of planet formation in young stellar objects. Observations have detected signs of dust growth in very young protoplanetary disks. Furthermore, signs of planet formation, gaps in the disk at a distance of several tens of au from the central protostar, are also reported. From a theoretical point of view, however, planet formation in the outer regions is difficult due to the rapid inward drift of dust, called the radial drift barrier. Here, on the basis of three-dimensional magnetohydrodynamical simulations of disk evolution with dust growth, we propose a mechanism called the “ashfall” phenomenon, induced by a powerful molecular outflow driven by a magnetic field that may circumvent the radial drift barrier. We find that the large dust that grows to a size of about a centimeter in the inner region of a disk is entrained by an outflow from the disk. Then, large dust decoupled from gas is ejected from the outflow due to centrifugal force, enriching the grown dust in the envelope and eventually falls onto the outer edge of the disk. The overall process is similar to the behavior of ashfall from volcanic eruptions. In the ashfall phenomenon, the Stokes number of dust increases by reaccreting to the less dense disk outer edge. This may allow the dust grains to overcome the radial drift barrier. Consequently, the ashfall phenomenon can provide a crucial assist for making the formation of the planetesimals in outer regions of the disk possible, and hence the formation of wide-orbit planets and gaps.
Split Peas in a Pod: Intra-system Uniformity of Super-Earths and Sub-Neptunes
Authors: Millholland Sarah C. , Winn Joshua N. 
Published: October 2021

Abstract
The planets within compact multiplanet systems tend to have similar sizes, masses, and orbital period ratios, like “peas in a pod.” This pattern was detected when considering planets with radii between 1 and 4 R
⊕. However, these same planets show a bimodal radius distribution, with few planets between 1.5 and 2 R
⊕. The smaller “super-Earths” are consistent with being stripped rocky cores, while the larger “sub-Neptunes” likely have gaseous H/He envelopes. Given these distinct structures, it is worthwhile to test for intra-system uniformity separately within each category of planets. Here, we find that the tendency for intra-system uniformity is twice as strong when considering planets within the same size category than it is when combining all planets together. The sub-Neptunes tend to be

1.7

−
0.3

+
0.6

times larger than the super-Earths in the same system, corresponding to an envelope mass fraction of about 2.6% for a 5 M
⊕ planet. For the sub-Neptunes, the low-metallicity stars are found to have planets with more equal sizes, with modest statistical significance (p ∼ 0.005). There is also a modest (∼2σ) tendency for wider-orbiting planets to be larger, even within the same size category.
Molecules and Outflows in NML Cygni: New Insights from a 1 mm Spectral Line Survey
Authors: Singh A. P. , Edwards J. L. , Humphreys R. M. , Ziurys L. M. 
Published: October 2021

Abstract
A sensitive (1σ rms ≤ 3 mK) 1 mm spectral survey (214.5–285.5 GHz) of the oxygen-rich circumstellar envelope of the red hypergiant NML Cygni (NML Cyg) has been conducted using the Sub-millimeter Telescope (SMT) of the Arizona Radio Observatory (ARO). Over 100 spectral lines were detected, arising from 17 different molecules, including the carbon-bearing species CO, HCN, HCO+, CN, and HNC; sulfur- and silicon-containing compounds H2S, SO, SO2, SiO, and SiS; and more exotic NaCl and AlO. The 1 mm spectrum of NML Cyg closely resembles that of VY Canis Majoris (VY CMa) suggesting that the chemistries of hypergiant stars are similar. The line profiles in NML Cyg consist of multiple velocity features, particularly evident in SO2 and SO. In addition to a spherical wind at the star’s systemic velocity, the spectra suggest an asymmetric, blueshifted component near V
LSR = −21 ± 3 km s−1 and a collimated, redshifted component near 15 ± 3 km s−1, positioned ∼34° and ∼12°, respectively, from the line of sight. The red- and blueshifted flows appear to be randomly oriented, and likely trace sporadic mass loss events. Their LSR velocities align closely with those of 22 GHz water masers, suggesting an NE–SE orientation. The winds may also be associated with the asymmetric nebula in F555W HST images but extending to 5″ (∼600R
*). NML Cyg appears to be another example of rare, massive stars with collimated, episodic ejections, analogous to Betelgeuse and VY CMa, lending support for an important new mass loss mechanism—surface activity.
Constraints on Weak Supernova Kicks from Observed Pulsar Velocities
Authors: Willcox Reinhold , Mandel Ilya , Thrane Eric , Deller Adam , Stevenson Simon , Vigna-Gómez Alejandro 
Published: October 2021

Abstract
Observations of binary pulsars and pulsars in globular clusters suggest that at least some pulsars must receive weak natal kicks at birth. If all pulsars received strong natal kicks above 50 km s−1, those born in globular clusters would predominantly escape, while wide binaries would be disrupted. On the other hand, observations of transverse velocities of isolated radio pulsars indicate that only 5 ± 2% have velocities below 50 km s−1. We explore this apparent tension with rapid binary population synthesis modeling. We propose a model in which supernovae with characteristically low natal kicks (e.g., electron-capture supernovae) only occur if the progenitor star has been stripped via binary interaction with a companion. We show that this model naturally reproduces the observed pulsar speed distribution and without reducing the predicted merging double neutron star yield. We estimate that the zero-age main-sequence mass range for noninteracting progenitors of electron-capture supernovae should be no wider than ≈0.2 M
⊙.
Novel Model of an Ultra-stripped Supernova Progenitor of a Double Neutron Star
Authors: Jiang Long , Tauris Thomas M. , Chen Wen-Cong , Fuller Jim 
Published: October 2021

Abstract
Recent discoveries of double neutron star (DNS) mergers and ultra-stripped supernovae (SNe) raise the questions of their origin and connection. We present the first 1D model of a DNS progenitor system that is calculated self-consistently until an ultra-stripped iron core collapse. We apply the MESA code starting from a post-common-envelope binary consisting of a 1.35 M
⊙ NS and a 3.20 M
⊙ zero-age main-sequence helium star and continue the modeling via Case BB Roche-lobe overflow until the infall velocity of the collapsing iron core exceeds 1000 km s−1. The exploding star has a total mass of ∼1.90 M
⊙, consisting of a ∼0.29 M
⊙ He-rich envelope embedding a CO core of ∼1.61 M
⊙ and an iron-rich core of ∼1.50 M
⊙. The resulting second-born NS has an estimated mass of ∼1.44 M
⊙, and we discuss the fate of the post-SN system, as well as the mild recycling of the first-born NS. Depending on the initial conditions, this family of systems is anticipated to reproduce the DNS mergers detected by the LIGO network.
Pluto’s Resonant Orbit Visualized in 4D
Authors: Zaveri Nihaal , Malhotra Renu 
Published: October 2021

Abstract
Orbital resonance phenomena are notoriously difficult to communicate in words due to the complex dynamics arising from the interplay of gravity and orbital angular momentum. A well known example is Pluto’s 3:2 mean motion resonance with Neptune. We have developed a python software tool to visualize the full three-dimensional aspects of Pluto’s resonant orbital dynamics over time. The visualizations include still images and animated movies. By contrasting Pluto’s resonant dynamics with the dynamics of a nearby non-resonant orbit, this tool enables better understanding and exploration of complex planetary dynamics phenomena.
Making a Global Image of the World: Science, Cosmography and Navigation in Times of the First Circumnavigation of Earth, 1492-1522
Authors: Sánchez Antonio 
Published: October 2021

The voyages of exploration and discovery during the period of European maritime expansion and the immense amount of information and artefacts they produced about our knowledge of the world have maintained a difficult, if not non-existent, relationship with the main historiographical lines of the history of early modern science. This article attempts to problematize this relationship based on a historical account that seeks to highlight the scientific and institutional mechanisms that made the Magellan-Elcano voyage, the first modern voyage, possible. The text argues that this voyage was the first modern voyage because it allowed the construction of a new scientific and cartographic image of the globe and contributed to our understanding of the world as a global world, altering the foundations on which modern European economic and geographic thought was based. In that sense, the voyage was something extraordinary, but not completely unexpected. It responded to a complex process of expansionary policy and technical development that dated back to the 15th century, which in 1519 was sufficiently articulated to carry out a great feat.
On the Translation of Founding Narratives into Cartographic Images: America in Le Testu’s Cosmographie Universelle (1556)
Authors: Martínez Carolina 
Published: October 2021

This article analyzes the links between the first travel accounts of the New World and the production of cartographic images of America in Guillaume Le Testu’s Cosmographie Universelle (1556). Produced in 1556 and dedicated to Admiral of France Gaspard de Coligny, the Norman pilot’s manuscript atlas was created in the context of growing French colonial interest in Terra Brasilis. The transposition of America’s founding narratives into cartographic images as presented in Le Testu’s Cosmographie is interpreted here as an act of translation lato sensu. The translation of the continent’s travel accounts in the strictest sense of the word, and the adaptation of New World information to new audiences and political contexts are also examined in the analysis of this manuscript nautical atlas.
Paris en chantier : exhumer le carnaval par le trou des Halles
Authors: Bauchard Vincent 
Published: October 2021

La destruction des Halles de Paris en 1971 est vécue par la population parisienne comme une véritable agression de la part des pouvoirs publics. De ce chantier interminable laissant un gouffre béant en plein cœur de la capitale plusieurs années durant, nous ne trouvons plus beaucoup de traces. Le « Trou des Halles » semble s'être progressivement effacé dans la mémoire collective. Quelques cinéastes ont pourtant essayé de conserver ce souvenir, en tournant leurs films au moment même où le Paris d'avant-guerre disparaissait. En 1973, Philippe Haudiquet signe un court documentaire sur la destruction des Halles, sobrement intitulé Les Halles, 1973. En 1974, Marco Ferreri met en scène, dans le trou même, une parodie de western, Touche pas à la femme blanche ! et Pierre Tchernia imagine une guerre fantaisiste entre des défenseurs du patrimoine, réfugiés dans les sous-sols de Paris, et le Ministre des Travaux Publics. Témoins privilégiés d'une « folie de l'urbanisation » des années 1970, ces trois films prennent position contre les pouvoirs publics en convoquant, chacun à leur manière, les formes populaires du carnaval.
The anthropometric, physical, and relative age characteristics of an English Premiership rugby union academy
Authors: Dimundo Francesco , Cole Matthew , Blagrove Richard C. , McAuley Alexander B. T. , Till Kevin , Hall Mike , Pacini Daniele , Kelly Adam L. 
Published: October 2021

Long-term athlete development is a primary focus for the England Rugby Football Union (RFU). The purpose of this study was to explore the anthropometric, physical, and relative age characteristics of rugby union academy players based on age group and playing position. Seventy-eight participants were examined for height, body mass, 10 and 20 m sprint, countermovement jump, reactive strength index, aerobic capacity, isometric hip extension, dominant handgrip strength, and birth quartile (BQ) across three age categories (i.e., under-16, under-18, and under-21) and two positions (forwards and backs). ANOVA and Kruskall–Wallis analysis were used to examine differences across each age category and position. TukeyHSD and Dunn’s test with Bonferroni correction was used for further post-hoc analysis. BQ distributions were compared against national norms using chi-square analysis. Results revealed that both older forwards (P=0.005) and backs (P=0.002) had significantly greater body mass, maximal aerobic capacity, and power compared to younger players. However, older forwards had slower 10 m sprint times compared to younger forwards. Moreover, relatively older players were significantly overrepresented across all age groups when compared to relatively younger players. Findings suggest that: (a) players should aim to develop greater parameters of body mass and aerobic capacity; (b) forwards should aim to develop acceleration and strength; (c) backs should aim to develop power and quickness; (d) players need to develop anthropometric and physical qualities and differences are apparent by age and position; and, (e) coaches should consider relative age when recruiting and developing young players.
Key words: Talent identification; Talent development; Expertise; Physical development; Physiological profile; Rugby football
Influência do tolueno na modificação química das fibras de bagaço de cana-de-açúcar
Authors: Maia Tatiana Faria , Mulinari Daniella Regina 
Published: October 2021

Nesta pesquisa foi estudada a influência do tolueno na modificação química das fibras de bagaço de cana-de-açúcar por esterificação por meio de sistema anidrido para uso em compósitos. Também foi avaliada a quantidade de catalisador na reação de esterificação. A modificação química das fibras provenientes do bagaço de cana de açúcar foi avaliada pela técnica de Espectroscopia de Infravermelho (FTIR). Os resultados revelaram que o tolueno influenciou na modificação química realizada nas fibras. A técnica de FTIR evidenciou esta modificação química.
Viktor Petrovich Salnikov is 75
Authors: Захарцев С.И. , Комаров С.А. , Хабибулин А.Г. 
Published: October 2021

Статья посвящена юбилею доктора юридических наук, профессора, академика, заслуженного деятеля науки Российской Федерации, почетного сотрудника органов внутренних дел, многолетнего члена экспертного совета ВАК, бывшего начальника Санкт-Петербургского университета МВД России генерал-лейтенанта милиции в отставке – Виктора Петровича Сальникова.
The article is dedicated to the anniversary of the Doctor of Law, Professor, Academician, Honored Scientist of the Russian Federation, Honorary Officer of the Internal Affairs Bodies, a long-term member of the Expert Council of the Higher Attestation Commission, former head of the St. Petersburg University of the Ministry of Internal Affairs of Russia, retired police lieutenant general – Viktor Petrovich Salnikov.
Análise do custo da prestação do serviço de coleta de lixo do Município de Ouro Verde do Oeste - PR
Authors: Lima Luis Carlos de , Dall'Asta Denis 
Published: October 2021

O presente trabalho tem por objetivo fazer pesquisa e analisar as informações dos custos da cobrança de coleta lixo do município de Ouro Verde do Oeste – PR, para proposição de medidas a se obter uma tabela de valores para cobrança justa. Com isso buscou-se a elaboração de um levantamento por meio de estudo técnico para obter um resultado para análise onde poderá verificar se há equilíbrio de valores lançados e recolhidos conforme cálculos efetuados pelo coeficiente da tabela de em vigor, verificando se a cobrança é justa. Os resultados alcançados serão apresentados a e ficarão disponíveis ao Município de Ouro Verde do Oeste-PR, para análise, estudo e possível intervenção futura caso seja necessário, com opções em e alternativas a firmar convênios ou parceria com a Companhia de energia elétrica ou com a Companhia de Saneamento efetuando a cobrança na fatura mensal, aumentando a proporção do valor arrecadado do lançamento anual já que o município não arrecada o total lançado, ficando débitos a receber no exercício seguinte. Este estudo foi elaborado tendo como base as informações obtidas "in loco" e o método utilizado para o desenvolvimento deste trabalho foi a coleta de dados por meio de planilhas de controle e perguntas aos funcionários que executam o referido serviço lotados na Secretaria de Viação e Obras, habitação e urbanismo, informações obtidas no Departamento de Recursos Humanos referente os funcionários que executam o serviço na área da coleta, informações dos imóveis edificados fornecidas pelo Departamento de Receita e Cadastro Técnico Imobiliário Fiscal do Município onde por meio de seu Cadastro Imobiliário possui relação dos imóveis edificados que são cobrados a taxa de coleta anual do lixo e resíduos