bluuebunny/crossref_metadata_2025_split huggingface dataset:
Mengulik Pemikiran Alfred N. Whitehead Tentang Kebudayaan
Authors: Sudarminta Justin 
Published: November 2020

Abstract: This article attempts to formulate Alfred N. Whitehead’s thoughts on culture. Even though he never specifically wrote on culture, his thoughts on it can be gleaned and constructed from his major books. The article will be divided into three parts. First, by borrowing some ideas from David L. Hall’s book The Civilization of Experience: A Whiteheadian Theory of Culture, I shall try to formulate what Whitehead means by culture. Second, I shall describe what Hall termes “cultural aims” and “cultural interests” in the perspective of Whitehead’s thought. Third, I shall address some important points in Whitehead’s critique of modern culture and the alternative he proposed. Finally, I shall point out some major conclusions that can be derived from our study of Whitehead’s thoughts on culture.
Keywords: Culture, cultural aims, cultural interests, modern culture, civilized society, art, adventure, beauty, truth, peace.
Abstrak: Tulisan ini berupaya merumuskan pemikiran Whitehead tentang kebudayaan. Kendati ia tidak pernah secara khusus menulis tentang kebudayaan, namun pemikirannya dapat diulik dan coba dirumuskan dari berbagai karya pokoknya. Tulisan akan dibagi menjadi tiga bagian. Pertama, dengan memanfaatkan kajian yang pernah dibuat oleh David L. Hall dalam bukunya The Civilization of Experience. A Whiteheadian Theory of Culture, penulis akan merumuskan pengertian kebudayaan menurut Whitehead. Kedua, penulis akan memaparkan apa yang oleh Hall disebut “cita-cita budaya” dan “kepentingan budaya” dalam perpektif pemikiran Whitehead. Ketiga, penulis akan membahas beberapa butir penting dari kritik Whitehead terhadap budaya modern berikut alternatif yang ia tawarkan. Tulisan ini akan ditutup dengan beberapa kesimpulan yang dapat ditarik dari kajian mengenai pemikiran Whitehead tentang kebudayaan.
Kata-kata Kunci: Kebudayaan, cita-cita budaya, kepentingan budaya, budaya modern, masyarakat berkeadaban, seni, petualangan , keindahan, kebenaran, kedamaian.
Pandangan Johann Baptist Metz Tentang Politik Perdamaian Berbasis Compassio
Authors: Kleden Paul Budi 
Published: November 2020

Abstract: The plurality of cultures and religions is one of the most difficult challenges our world has to face at present. Tensions in various forms have become daily news, which puts into question our ability and willingness to share this planet earth as our common place to live together. There is not only a need to develop the best strategy to live together, but also to find fundamental arguments for conviviality. This article presents the ideas of Johann Baptist Metz, a German theologian, on a politic based on compassion. Memoria passionis, remembering the suffering, especially that of others, is the basis for constructing a new politics of peace.
Keywords: Politics, compassion, plurality, victim, suffering, memory.

Abstrak: Salah satu dari tantangan terbesar yang sedang dihadapi masyarakat dunia dewasa ini adalah ketidaksanggupan berbagai kelompok untuk menanggapi pluralitas kebudayaan dan agama. Kemajemukan bukanlah realitas baru. Yang baru adalah intensitas pengalaman kemajemukan itu. Berbagai ketegangan hingga konflik berdarah menjadi berita harian yang mempertanyakan kemampuan dan kesediaan kita untuk berbagi hidup di atas bumi ini dengan orang-orang yang berbeda budaya dan agama. Menghadapi masalah ini, kita tidak hanya perlu mengembangkan strategi yang paling baik untuk dapat hidup bersama secara damai dan adil, tetapi juga membutuhkan pengembangan argumen-argumen yang memberikan pendasaran bagi strategi tersebut. Artikel ini hendak memperkenalkan pandangan Johann Baptist Metz, seorang teolog berkebangsaan Jerman, tentang politik yang berbasiskan compassio. Memoria passionis, mengenang penderitaan, khususnya penderitaan orang lain, merupakan dasar untuk membangun sebuah politik perdamaian bagi dunia.

Kata-kata Kunci: Politik, compassio, pluralitas, korban, penderitaan, kenangan.
Analisis Kelayakan Usaha dan Strategi Pengembangan Industri Kecil Tempe di Kelurahan Setia Negara Kecamatan Siantar Sitalasari
Authors: Putri Wahyuni Arnold  , Pinondang Nainggolan  , Darwin Damanik  
Published: November 2020

Sektor industri mengambil bahan baku dari sektor primer dan mengubahnya menjadi produk pengguna akhir. Contoh bisnis sektor industri termasuk produksi kecil pembuatan tempe. Usaha industri besar memliki sifat produktif dan memenuhi kriteria berupa memiliki kekayaan diatas 10 miliar termasuk dengan kekayaan tanah, maupun bangunan usaha yang digunakan sebagai tempat usaha. Usaha industri besar ini bisa mendapatkan kredit atau pinjaman dari bank dimana nilainya lebih dari 5 miliar rupiah. Sedangkan usaha industri menengah bisa berdiri sendiri dan didirikan oleh perorangan atau badan usaha dan bukan menjadi anak perusahaan atau cabang perusahaan. Untuk kriterianya sudah diatur dalam Undang-undang Nomor 20 Tahun 2008 dimana kekayaan bersihnya mencapai lebih dari 500 juta dan paling banyak adalah 10 miliar. Dan usaha industri kecil adalah usaha dalam bidang ekonomi yang produktif dan mampu berdiri sendiri dan bisa didirikan oleh perorangan atau badan usaha namun tidak menjadi anak perusahaan atau cabang perusahaan. Kriteria dari usaha kecil ini diatur dalam Undang - undang Nomor 20 tahun 2008 yang mana memiliki kekayaan lebih dari 50 juta. Dalam menyusun penelitian ilmiah diperlukan strategi dan langkah - langkah yang benar sesuai dengan tujuan penelitian. Hal ini dimaksudkan agar hasil penelitian dapat dipertanggungjawabkan secara ilmiah. Penelitian ini dilaksanakan dengan menggunakan satu metode. Dalam penelitianini, peneliti menggunakan metode kuantitatif. Profil Usaha Industri Kecil Tempe di Kelurahan Setia Negara Kecamatan Siantar Sitalasari yaitu dikelola oleh laki-laki sebanyak 60% dan dikelola oleh perempuan sebanyak 40%, dikelola oleh penduduk berusia 30-40 tahun sebanyak 30%, usia 41-50 tahun sebanyak 40%, usia 51-60 tahun sebanyak 20% dan usia > 60 tahun sebanyak 10%, dikelola oleh penduduk berpendidikan SD sebanyak 30%, sebanyak 20% dikelola oleh penduduk berpendidikan SMP dan sebanyak 50% dikelola oleh penduduk berpendidikan SMA/SMK, sudah berdiri lama dengan lama usaha < 10 tahun sebanyak 40%, lama usaha 11-20 tahun 10%, lama usaha 21-30 tahun 30%, lama usaha 31-40 tahun 20%
Saccadic scanpath length: an index for human threat conditioning
Authors: Xia Yanfang , Melinscak Filip , Bach Dominik R. 
Published: November 2020

AbstractThreat-conditioned cues are thought to capture overt attention in a bottom-up process. Quantification of this phenomenon typically relies on cue competition paradigms. Here, we sought to exploit gaze patterns during exclusive presentation of a visual conditioned stimulus, in order to quantify human threat conditioning. To this end, we capitalized on a summary statistic of visual search during CS presentation, scanpath length. During a simple delayed threat conditioning paradigm with full-screen monochrome conditioned stimuli (CS), we observed shorter scanpath length during CS+ compared to CS- presentation. Retrodictive validity, i.e., effect size to distinguish CS+ and CS-, was maximized by considering a 2-s time window before US onset. Taking into account the shape of the scan speed response resulted in similar retrodictive validity. The mechanism underlying shorter scanpath length appeared to be longer fixation duration and more fixation on the screen center during CS+ relative to CS- presentation. These findings were replicated in a second experiment with similar setup, and further confirmed in a third experiment using full-screen patterns as CS. This experiment included an extinction session during which scanpath differences appeared to extinguish. In a fourth experiment with auditory CS and instruction to fixate screen center, no scanpath length differences were observed. In conclusion, our study suggests scanpath length as a visual search summary statistic, which may be used as complementary measure to quantify threat conditioning with retrodictive validity similar to that of skin conductance responses.
A Geometric Origin for Quasi-periodic Oscillations in Black Hole X-Ray Binaries
Authors: Rana Prerna , Mangalam A. 
Published: November 2020

Abstract
We expand the relativistic precession model to include nonequatorial and eccentric trajectories and apply it to quasi-periodic oscillations (QPOs) in black hole X-ray binaries (BHXRBs) and associate their frequencies with the fundamental frequencies of the general case of nonequatorial (with Carter's constant,

) and eccentric (

) particle trajectories, around a Kerr black hole. We study cases with either two or three simultaneous QPOs and extract the parameters {e, r

p
, a, Q}, where r

p
is the periastron distance of the orbit, and a is the spin of the black hole. We find that the orbits with

should have e ≲ 0.5 and r

p
∼ 2–20 for the observed range of QPO frequencies, where a ∈ [0, 1], and that the spherical trajectories {e = 0,

} with Q = 2–4 should have r

s
∼ 3–20. We find nonequatorial eccentric solutions for both M82 X-1 and GROJ 1655-40. We see that these trajectories, when taken together, span a torus region and give rise to a strong QPO signal. For two simultaneous QPO cases, we found equatorial eccentric orbit solutions for XTEJ 1550-564, 4U 1630-47, and GRS 1915+105, and spherical orbit solutions for BHXRBs M82 X-1 and XTEJ 1550-564. We also show that the eccentric orbit solution fits the Psaltis–Belloni–Klis correlation observed in BHXRB GROJ 1655-40. Our analysis of the fluid flow in the relativistic disk edge suggests that instabilities cause QPOs to originate in the torus region. We also present some useful formulae for trajectories and frequencies of spherical and equatorial eccentric orbits.
Relativistic Shear Boundary Layer and the Gamma-Ray Emission of GW170817
Authors: Spisak Jacob , Liang Edison , Fu Wen , Boettcher Markus 
Published: November 2020

Abstract
We present an analysis of the radiation characteristics of kinetic shear boundary layers created by relativistic plasma jets. Using a model of electromagnetic field data based on particle-in-cell simulations of an electron–ion plasma, we solve the motion of individual test electrons and compute their instantaneous radiated power and peak frequency. By analyzing a large number of test electrons in this manner, we find two distinct electron populations present around the shear boundary layer. The most highly radiative electrons execute looping motion due to crossed electric and magnetic fields as they are accelerated along the bulk flow of the jet, and eventually cross the shear boundary interface at steep angles. Electrons that never cross the shear boundary interface radiate much less energy as a group. Summing over all of the highly radiative electrons, we compute the distribution of the total radiated energy as a function of the angle relative to the bulk flow. This result has important potential implications for the observed radiation output of short gamma-ray bursts viewed at large angles from the jet axis, such as the neutron star merger event GW170817/GRB 170817A.
The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). II. Molecular Outflows in the Extreme Early Stages of Protocluster Formation
Authors: Li Shanghuo , Sanhueza Patricio , Zhang Qizhou , Nakamura Fumitaka , Lu Xing , Wang Junzhi , Liu Tie , Tatematsu Ken’ichi , Jackson James M. , Silva Andrea , Guzmán Andrés E. , Sakai Takeshi , Izumi Natsuko , Tafoya Daniel , Li Fei , Contreras Yanett , Morii Kaho , Kim Kee-Tae 
Published: November 2020

Abstract
We present a study of outflows at extremely early stages of high-mass star formation obtained from the ALMA Survey of 70 μm dark High-mass clumps in Early Stages (ASHES). Twelve massive 3.6−70 μm dark prestellar clump candidates were observed with the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6. Forty-three outflows are identified toward 41 out of 301 dense cores using the CO and SiO emission lines, yielding a detection rate of 14%. We discover six episodic molecular outflows associated with low- to high-mass cores, indicating that episodic outflows (and therefore episodic accretion) begin at extremely early stages of protostellar evolution for a range of core masses. The time span between consecutive ejection events is much smaller than those found in more evolved stages, which indicates that the ejection episodicity timescale is likely not constant over time. The estimated outflow dynamical timescale appears to increase with core masses, which likely indicates that more massive cores have longer accretion timescales than less massive cores. The lower accretion rates in these 70 μm dark objects compared to the more evolved protostars indicate that the accretion rates increase with time. The total outflow energy rate is smaller than the turbulent energy dissipation rate, which suggests that outflow-induced turbulence cannot sustain the internal clump turbulence at the current epoch. We often detect thermal SiO emission within these 70 μm dark clumps that is unrelated to CO outflows. This SiO emission could be produced by collisions, intersection flows, undetected protostars, or other motions.
Caltech–NRAO Stripe 82 Survey (CNSS). III. The First Radio-discovered Tidal Disruption Event, CNSS J0019+00
Authors: Anderson M. M. , Mooley K. P. , Hallinan G. , Dong D. , Phinney E. S. , Horesh A. , Bourke S. , Cenko S. B. , Frail D. , Kulkarni S. R. , Myers S. 
Published: November 2020

Abstract
We present the discovery of a nuclear transient with the Caltech–NRAO Stripe 82 Survey (CNSS), a dedicated radio transient survey carried out with the Karl G. Jansky Very Large Array (VLA). This transient, CNSS J001947.3+003527, exhibited a turn-on over a timescale of ≲1 yr, increasing in flux density at 3 GHz from <0.14 mJy in 2014 February to 4.4 ± 0.1 mJy in 2015 March, reaching a peak luminosity of

around 2015 October. The association of CNSS J0019+00 with the nucleus (Gaia and our very-long baseline interferometry positions are consistent to within 1 pc) of a nearby S0 Seyfert galaxy at 77 Mpc, together with the radio spectral evolution, implies that this transient is most likely a tidal disruption event (TDE). Our equipartition analysis indicates the presence of a ∼15,000 km s−1 outflow, having energy ∼1049 erg. We derive the radial density profile for the circumnuclear material in the host galaxy to be proportional to R
−2.5. All of these properties suggest resemblance with radio-detected thermal TDEs like ASASSN-14li and XMMSL1 J0740-85. No significant X-ray or optical emission is detected from CNSS J0019+00, although this may simply be due to the thermal emission being weak during our late-time follow-up observations. From the CNSS survey we have obtained the first unbiased measurement of the rate of radio TDEs, R(>500μJy) of about 2 × 10−3 deg−2, or equivalently a volumetric rate of about 10 Gpc−3 yr−1. This rate implies that all-sky radio surveys such as the VLA Sky Survey and those planned with ASKAP, will find many tens of radio TDEs over the next few years.
Clumping in the Winds of Wolf–Rayet Stars
Authors: Chené André-Nicolas , St-Louis Nicole , Moffat Anthony F. J. , Gayley Kenneth G. 
Published: November 2020

Abstract
We attempt to determine the driver for clumping in hot-star winds by extending the measure of the spectral variability level of Galactic Wolf–Rayet stars to by far the hottest known among them, the WN2 star WR 2 and the WO2 stars WR 102 and WR 142. These three stars have T
⋆ = 140 and 200 kK, the last two being well above the bulk of WR stars with T
⋆ ∼ 40–120 kK. This full temperature range for WR stars is much broader than that of their O-star progenitors (∼30–50 kK), so is better suited to look for any temperature dependence of wind clumping. We have obtained multiple observations with high signal-to-noise, moderate-resolution spectroscopy in search of small-scale variability in the strong emission lines from the dense winds of these three extreme stars, and find a very low-level of variability in both stars. Temperature and terminal velocity are correlated, so faster winds show a lower variability, though this trend goes against any predictions made involving Line Deshadowing Instability (LDI) only, implying that instabilities intrinsic to LDI are not the main source of wind clumping. Instead, it could be taken as support for the suggestion that clumps are caused by a subsurface convection zone (SSCZ) at T ∼ 170 kK, since such an SSCZ would have little opportunity to operate under the hydrostatic surface of these hottest WR stars. It is still possible, however, that an SSCZ-related driver could interact with nonlinear line instability effects to enhance or possibly even produce clumps.
HCN J = 4–3, HNC J = 1–0, H13CN J = 1–0, and HC3N J = 10–9 Maps of Galactic Center Region. II. Physical Properties of Dense-gas Clumps and Probability of Star Formation
Authors: Tanaka Kunihiko , Nagai Makoto , Kamegai Kazuhisa , Iino Takahiro , Sakai Takeshi 
Published: November 2020

Abstract
We report a statistical analysis exploring the origin of the overall low star formation efficiency (SFE) of the Galactic central molecular zone (CMZ) and the SFE diversity among the CMZ clouds using a wide-field HCN J = 4–3 map, whose optically thin critical density (

) is the highest among the tracers ever used in CMZ surveys. Logistic regression is performed to empirically formulate star formation probability of 195 HCN clumps, 13 of which contain star formation signatures. The explanatory parameters in the best-fit model are reduced into the virial parameter

without significant contribution from other parameters, whereas the performance of the model without

is no better than that using randomly generated data. The threshold

is 6, which translates into a volume density (

) of

with the

–

correlation. The scarcity of the low-

clumps, whose fraction to all HCN clumps is 0.1, can be considered as one of the immediate causes of the suppressed SFE. No correlation between the clump size or mass and star formation probability is found, implying that HCN J = 4–3 does not immediately trace the mass of star-forming gas above a threshold density. Meanwhile, star-forming and non-star-forming clouds are degenerate in the physical parameters of the CS

= 1–0 clouds, highlighting the efficacy of the HCN

= 4–3 line to probe star-forming regions in the CMZ. The timescale of the high-

to low-

transition is

, which is consistent with the tidal compression and X1/X2 orbit transition models but possibly does not fit the cloud–cloud collision picture.
Mysterious Globular Cluster System of the Peculiar Massive Galaxy M85
Authors: Ko Youkyung , Lee Myung Gyoon , Park Hong Soo , Sohn Jubee , Lim Sungsoon , Hwang Narae , Park Byeong-Gon 
Published: November 2020

Abstract
We present a study on the stellar population and kinematics of globular clusters (GCs) in the peculiar galaxy M85. We obtain optical spectra of 89 GCs at 8 kpc < R < 160 kpc using the MMT/Hectospec. We divide them into three groups, blue/green/red GCs (B/G/RGCs), with their (g − i)0 colors. All GC subpopulations have mean ages of about 10 Gyr, but showing differences in metallicities. The BGCs and RGCs are the most metal-poor ([Z/H] ∼ −1.49) and metal-rich ([Z/H] ∼ −0.45), respectively, and the GGCs are in between. We find that the inner GC system exhibits a strong overall rotation that is entirely due to a disklike rotation of the RGC system. The BGC system shows little rotation. The GGCs show kinematic properties clearly distinct among the GC subpopulations, having higher mean velocities than the BGCs and RGCs and being aligned along the major axis of M85. This implies that the GGCs have an origin different from the other GC subpopulations. The rotation-corrected velocity dispersion of the RGC system is much lower than that of the BGC system, indicating the truncation of the red halo of M85. The BGCs have a flat velocity dispersion profile out to R = 67 kpc, reflecting the dark matter extent of M85. Using the velocity dispersion of the BGC system, we estimate the dynamical mass of M85 to be 3.8 × 1012
M
⊙. We infer that M85 has undergone merging events lately, resulting in the peculiar kinematics of the GC system.
Vis–NIR Reflectance Microspectroscopy of IDPs
Authors: Maupin Romain , Djouadi Zahia , Brunetto Rosario , Lantz Cateline , Aléon-Toppani Alice , Vernazza Pierre 
Published: November 2020

Abstract
Visible near-infrared (Vis–NIR) reflectance spectroscopy is a powerful nondestructive technique allowing the parent bodies identification of cosmomaterials such as meteorites, micrometeorites, and interplanetary dust particles (IDPs) studied in the laboratory. Previous studies showed that meteorites do not represent the full diversity of the solar system small bodies. We present here an experimental setup we developed for measuring Vis–NIR microspectroscopy of individual IDPs. We acquired diffuse Vis–NIR reflectance spectra of 15 particles ranging 7–31 μm in size. We discuss the requirements, the abilities, as well as the limitations of the technique. For sizes smaller than 17 μm, the slopes increase with decreasing particles sizes, while for sizes larger than 17 μm, the slopes are randomly distributed. The visible reflectance levels do not appear to be affected by the size of the IDPs, and show a bimodal distribution. Among the studied particles, we identified an IDP (L2079C18) exhibiting a feature at 0.66 μm, which is similar to the one observed by remote sensing on the surface of hydrated asteroids. This is the first detection of a hydration band in the reflectance spectrum of an IDP that could indicate a possible link between hydrated IDPs with hydrated asteroid surfaces.