bluuebunny/crossref_metadata_2025_split huggingface dataset:
İstanbul ve Çevresinde Veba-yı Bakari (1886-1891)
Authors: Tan Seda 
Published: January 2024

Sığır vebası, en eski hayvan hastalıklarındandır. En çok, hassas türler olan sığır ve mandalara etki ettiği bilinir. Bulaşıcılığı ve ölüm oranı çok yüksek olan hastalık Anadolu coğrafyasında çağlar boyunca çok sayıda kırıma neden olduktan sonra ancak Cumhuriyet devrinde etkeni ile birlikte ortadan kaldırılabilmiştir. Anadolu tarihinin en uzun ve önemli kesitlerinden birisini temsil eden Osmanlılar devri boyunca ise hayvan varlığıyla sağlığını tehdit eden hastalıkların başında yer almıştır. Buna karşılık akademik literatürde diğer hayvan hastalıklarıyla birlikte insan hastalıklarının gölgesindedir. Hâlbuki hane ekonomisinin çift hayvanlarına dayandığı tarım odaklı ekonomilerde başta sığır vebası olmak üzere salgın hayvan hastalıkları, yalnız hayvan varlığı ve gönenciyle değil, sosyoekonomik hayatın bütünüyle ilgili deneyimlerdir. İnsan refahı ile şehirlerin huzur ve güvenliği bu travmatik deneyimden bağımsız düşünülemez.
Ele alınan çalışma hayvan mobilitesinin görece arttığı bir dönemde, Osmanlı sosyoekonomik hayatının istikrarı bakımından belirgin bir tehdit oluşturan ve Osmanlı İmparatorluğunun kalbi niteliğindeki başkentinde meydana gelen büyük bir sığır vebası salgınına odaklanmaktadır. 1886-1890, 1891 yıllarında en büyük tahribatını gerçekleştiren söz konusu salgın çalışmada yayılım coğrafyası, kronolojisi ve mücadele uygulamaları bağlamında değerlendirilmeye çalışılmıştır. Bu çerçevede kaynak, intikal, korunma/önleme gibi başlıklar çalışmanın odak noktalarını oluşturmuşlardır. Çalışmanın ana kaynağı ise birinci el kaynak niteliğindeki Osmanlı arşiv vesikalarıdır. Makale, dönemi ve hastalığın tarihçesini konu edinen doğrudan ve dolaylı diğer literatürle de desteklenmiştir.
İzmir-Yeşilova Höyüğü ve Geç Neolitik Dönem’de Kıyı Ege Mimarisi
Authors: Derin Zafer 
Published: January 2024

Bornova Ovası’nın ortasında, Yeşilova Höyüğü kazı çalışmalarıyla birlikte Yassıtepe Höyüğü ve İpeklikuyu Höyüğü’nü de kapsayan, yaklaşık 1200 metre çapındaki alanda ‘İzmir’in Prehistorik Yerleşim Alanı’ ortaya çıkartılmıştır. Yaklaşık 70 bin metrekareden fazla bir alana yayılan Yeşilova Höyüğü’nde ilk yerleşimin günümüzden en az 8500 yıl önce Neolitik Çağ’ın başında başlamış olduğu, Neolitik Dönem’den Roma Dönemi’ne kadar birçok kültürün yaşadığı kazı çalışmaları sonucu ortaya konulmaktadır. Höyükteki ilk yerleşime ait kalıntı ve buluntular, bugünkü ova seviyesinin yaklaşık 4-5 metre altında killi ana toprağın üzerinde yer almaktadır. Yerleşimin kültür dolgusu ise yaklaşık 3-3,5 metredir. Kültür dolgusu 4 kültür katından oluşmaktadır. Kültür katları, yüzeyden başlayarak; I. Kat Roma Dönemi, II. Kat Tunç Çağ, III. Kat Kalkolitik Çağ (1-2 Tabakaları) ve IV. Kat Neolitik Çağ (1a,b,c-8 Tabakaları) olarak saptanmıştır. Dört kültür katında gelişim gösteren höyük genellikle tahribatlardan sonra yeniden inşa edildikleri anlaşılan 15 mimari kata sahiptir.
Yeşilova Höyüğü’nde Neolitik Çağ’ın başında başlayan yerleşim, Neolitik Çağ’ın sonuna doğru en zengin dönemine ulaşmıştır. Neolitik yerleşimin MÖ 6000-5700 yılları arasındaki son dönemini temsil eden, kalıntılarıyla en çok verinin elde edildiği yerleşim katlarında, birbirlerinden ayrı inşa edilen mekânlarda genellikle gündelik yaşama ilişkin işlikler ortaya çıkartılmıştır. Yeşilova Höyüğü Geç Neolitik Dönem mimarisi Kıyı Ege kültürlerine özgü niteliklere sahiptir. Mimari özellikler ve plan bakımından İç Batı Anadolu’dan farklıdır.
Demir Çağı Kappadokia’sında İlk Tapınak: Oluz Höyük İbadethane ve Ateşgedesi
Authors: Dönmez Şevket , Saba Mona 
Published: January 2024

Amasya ili sınırları içinde, şehir merkezine yirmi beş kilometre mesafede yer alan Oluz Höyük’te 2007 yılından beri sürmekte olan kazı çalışmaları Kalkolitik Dönem’den Orta Çağ’a kadar buluntu veren bu önemli merkezin dinsel bir yapılanma içinde olduğunu gözler önüne sermektedir. Hitit Büyük Krallığı’nın çöküş dönemine tanıklık eden tabakalarda ele geçen dini ayinlere ait deliller, Phryg Dönemi yerleşiminin merkezini teşkil eden Kubaba Sunağı erken dönemlere ait dinî bulguları oluştururken, Oluz Höyük’ün önemli dinî bir merkez olarak ortaya çıkışı Anadolu’nun Akhamenid (Pers) İmparatorluğu egemenliğine girdiği döneme rastlamaktadır.
Oluz Höyük’te, 2B Mimari Tabakasında (MÖ 450-300) ele geçen, Akhamenid (Pers) Dönemi’ne tarihlenen önemli ve eşsiz arkeolojik bulgular, Pers kökenli olup kutsal ateşe tek tapınım noktası olarak saygı gösteren ve arkaik monoteizme işaret eden bir zümrenin yerleşmiş olduğuna kanıt teşkil etmektedir. Bu makale, mimari kanıtları, kutsal ateşin yandığı Ateşgede ve inananların ritüellerini, mekân ve işlevdeki ortak ilişkilerini yerine getirdikleri ibadethane birlikteliğinde tartışmaktadır. Basit ve gösterişsiz mimariye sahip bir Ateşgede ve onunla fiziki bağlantısı olmasa da konumsal ilişkisi bulunan bir İbadethane yapısının varlığı, sonraki dönemlerde Hıristiyanlık ve İslamiyet gibi tek tanrılı dinlerde ortak nokta olacak bir toplanma mekânında cemaat oluşturulması fikrinin ortaya çıkışı ile ilgili olmalıdır. Bu durumu dini pratiklerin tapınak mekânına etkisi olarak da açıklayabiliriz. Bu yeni dini mimari Demir Çağı’nda yeni bir inanç sistemi ile birlikte Anadolu coğrafyasında ortaya çıkmıştır. Oluz Höyük 2B Mimari Tabakası tapınağı ile birlikte Perslerde ve Anadolu’da kutsal yapı kavramının başlamış olduğu düşünülebilir. Oluz Höyük 2B Mimari Tabakasında bahsi geçen bu zümre tarafından hayata geçirilmiş Kutsal Alan, İbadethane ve bu yapıları bir araya getiren Pers Yolu makalenin konusunu oluşturmaktadır.
Large-scale Effect of an Accretion Burst in the High-Mass Young Stellar Object G358.93-0.03-MM1
Authors: Miao Dan , Chen Xi , Bayandina Olga S. , Sobolev Andrej M. , Li Wan-jun , Sugiyama Koichiro 
Published: January 2024

Abstract
The high-mass young stellar object G358.93-0.03-MM1 underwent a rapid accretion burst event from 2019 January to June, resulting in flares observed in most class II methanol maser transitions starting in mid-January. In contrast, the 22.235 GHz water maser flare started in mid-April. To investigate the physical origin of this significant difference, we made the Karl G. Jansky Very Large Array observations toward the G358.93-0.03 region on 2019 March 23 and April 4 and obtained the intensity and spatial distribution images of the water maser as well as the continuum emissions at Ku and K bands on the epoch close to the water maser flare. A comparative analysis, incorporating previously reported detections in February (pre-water maser flare) and June (post-water maser flare), reveals the time lag between the accretion burst and water maser flare. These observations confirm the variations of the propagation speed of a heatwave induced by the accretion burst in different directions: the heatwave is decelerated in dense regions (e.g., the disk and jet), whereas in directions from G358-MM1 to water maser components, the heatwave speed is supposed to be close to the speed of light. Variations in flux density and spatial positions were detected for water masers and continuum emissions, indicating that the accretion burst event originating from G358-MM1 affects not only the immediate environment within a dense structure of 0.″2 (1400 au at a source distance of 6.75 kpc) around MM1 itself, but also exerts influence on broader-scale regions extending up to approximately 3″ (21,000 au).
The Dependence of the Structure of Planet-opened Gaps in Protoplanetary Disks on Radiative Cooling
Authors: Zhang Minghao , Huang Pinghui , Dong Ruobing 
Published: January 2024

Abstract
Planets can excite density waves and open annular gas gaps in protoplanetary disks. The depth of gaps is influenced by the evolving angular momentum carried by density waves. While the impact of radiative cooling on the evolution of density waves has been studied, a quantitative correlation to connect gap depth with the cooling timescale is lacking. To address this knowledge gap, we employ the grid-based code Athena++ to simulate disk-planet interactions, treating cooling as a thermal relaxation process. We establish quantitative dependencies of steady-state gap depth (Equation 36) and width (Equation 41) on planetary mass, Shakura–Sunyaev viscosity, disk scale height, and thermal relaxation timescale (β). We confirm previous results that gap opening is the weakest when the thermal relaxation timescale is comparable to the local dynamical timescale. Significant variations in gap depth, up to an order of magnitude, are found with different β. In terms of width, a gap is at its narrowest around β = 1, approximately 10%–20% narrower compared to the isothermal case. When β ∼ 100, it can be ∼20% wider, and higher viscosity enhances this effect. We derive possible masses of the gas gap-opening planets in AS 209, HD 163296, MWC 480, and HL Tau, accounting for the uncertainties in the local thermal relaxation timescale.
MAMMOTH-Subaru. III. Lyα Halo Identified by Stacking ∼3300 Lyα Emitters at z = 2.2–2.3
Authors: Zhang Haibin , Cai Zheng , Liang Yongming , Ma Ke , Kashikawa Nobunari , Li Mingyu , Wu Yunjing , Li Qiong , Johnson Sean D. , Ouchi Masami , Fan Xiaohui 
Published: January 2024

Abstract
In this paper, we present a Lyα halo (LAH) identified by stacking ∼3300 Lyα emitters (LAEs) at z = 2.2–2.3. We carry out imaging observations and data reduction with Subaru/Hyper Suprime-Cam. Our total survey area is ∼12 deg2 and the imaging depths are 25.5–27.0 mag. Using the imaging data, we select 1240 and 2101 LAE candidates at z = 2.2 and 2.3, respectively. We carry out spectroscopic observations of our LAE candidates and data reduction with Magellan/IMACS to estimate the contamination rate of our LAE candidates. We find that the contamination rate of our sample is low (8%). We stack our LAE candidates with a median stacking method to identify the LAH at z = 2. We show that our LAH is detected until ∼100 kpc at the 2σ significance level and likely extended to ∼200 kpc at a surface brightness level of ∼10−20 erg s−1 cm−2 arcsec−2. Compared to those of previous studies, our LAH is brighter at radii of ∼25–100 kpc, which is not likely caused by the contamination in our sample but by the different redshifts, fields, and selection methods instead. To investigate how central galaxies affect surrounding LAHs, we divide our LAEs into subsamples based on the Lyα luminosity (L
Lyα
), rest-frame Lyα equivalent width (EW0), and UV magnitude (M
uv). We stack the subsamples and find that higher L
Lyα
, smaller EW0, and brighter M
uv cause more extended halos. Our results suggest that more massive LAEs generally have more extended LAHs.
JADES: Resolving the Stellar Component and Filamentary Overdense Environment of Hubble Space Telescope (HST)-dark Submillimeter Galaxy HDF850.1 at z = 5.18
Authors: Sun Fengwu , Helton Jakob M. , Egami Eiichi , Hainline Kevin N. , Rieke George H. , Willmer Christopher N. A. , Eisenstein Daniel J. , Johnson Benjamin D. , Rieke Marcia J. , Robertson Brant , Tacchella Sandro , Alberts Stacey , Baker William M. , Bhatawdekar Rachana , Boyett Kristan , Bunker Andrew J. , Charlot Stephane , Chen Zuyi , Chevallard Jacopo , Curtis-Lake Emma , Danhaive A. Lola , DeCoursey Christa , Ji Zhiyuan , Lyu Jianwei , Maiolino Roberto , Rujopakarn Wiphu , Sandles Lester , Shivaei Irene , Übler Hannah , Willott Chris , Witstok Joris 
Published: January 2024

Abstract
HDF850.1 is the brightest submillimeter galaxy (SMG) in the Hubble Deep Field. It is known as a heavily dust-obscured star-forming galaxy embedded in an overdense environment at z = 5.18. With nine-band NIRCam images at 0.8–5.0 μm obtained through the JWST Advanced Deep Extragalactic Survey, we detect and resolve the rest-frame UV–optical counterpart of HDF850.1, which splits into two components because of heavy dust obscuration in the center. The southern component leaks UV and Hα photons, bringing the galaxy ∼100 times above the empirical relation between infrared excess and UV continuum slope (IRX–β
UV). The northern component is higher in dust attenuation and thus fainter in UV and Hα surface brightness. We construct a spatially resolved dust-attenuation map from the NIRCam images, well matched with the dust continuum emission obtained through millimeter interferometry. The whole system hosts a stellar mass of 1010.8±0.1
M
⊙ and star formation rate (SFR) of 102.8±0.2
M
⊙ yr−1, placing the galaxy at the massive end of the star-forming main sequence at this epoch. We further confirm that HDF850.1 resides in a complex overdense environment at z = 5.17–5.30, which hosts another luminous SMG at z = 5.30 (GN10). The filamentary structures of the overdensity are characterized by 109 Hα-emitting galaxies confirmed through NIRCam slitless spectroscopy at 3.9–5 μm, of which only eight were known before the JWST observations. Given the existence of a similar galaxy overdensity in the GOODS-S field, our results suggest that 50% ± 20% of the cosmic star formation at z = 5.1–5.5 occur in protocluster environments.
A Direct Comparison between the Use of Double Gray and Multiwavelength Radiative Transfer in a General Circulation Model with and without Radiatively Active Clouds
Authors: Malsky Isaac , Rauscher Emily , Roman Michael T. , Lee Elspeth K. H. , Beltz Hayley , Savel Arjun , Kempton Eliza M.-R. , Cinque L. 
Published: January 2024

Abstract
Inhomogeneous cloud formation and wavelength-dependent phenomena are expected to shape hot Jupiter atmospheres. We present a general circulation model with multiwavelength “picket fence” radiative transfer and radiatively active, temperature-dependent clouds, and compare the results to those of a double gray routine. The double gray method inherently fails to model polychromatic effects in hot Jupiter atmospheres, while picket fence captures these non-gray aspects and performs well compared to fully wavelength-dependent methods. We compare both methods with radiatively active clouds and cloud-free models, assessing the limitations of the double gray method. Although there are broad similarities, the picket fence models have larger dayside–nightside temperature differences, nonisothermal upper atmospheres, and multiwavelength effects in the presence of radiatively active clouds. We model the well-known hot Jupiters HD 189733 b and HD 209458 b. For the hotter HD 209458 b, the picket fence method prevents clouds from thermostating dayside temperatures, resulting in hotter upper atmospheres and the dissipation of dayside clouds. Differences in the temperature structures are then associated with nuanced differences in the circulation patterns and clouds. Models of the cooler HD 189733 b have global cloud coverage, regardless of the radiative transfer scheme, whereas there are larger differences in the models of HD 209458 b, particularly in the extent of the partial cloud coverage on its dayside. This results in minor changes to the thermal and reflected light phase curves of HD 189733 b, but more significant differences for the picket fence and double gray versions of HD 209458 b.
Simulating Hydrogen-poor Interaction-powered Supernovae with CHIPS
Authors: Takei Yuki , Tsuna Daichi , Ko Takatoshi , Shigeyama Toshikazu 
Published: January 2024

Abstract
We present the updated open-source code Complete History of Interaction-Powered Supernovae (CHIPS) that can be applied to modeling supernovae (SNe) arising from an interaction with the massive circumstellar medium (CSM) as well as the formation process of the CSM. Our update mainly concerns extensions to hydrogen-poor SNe from stripped progenitors, targeting the modeling of interaction-powered SNe Ibc, such as Type Ibn and Icn SNe. We successfully reproduce the basic properties of the light curves of these types of SNe that occur after the partial eruption of the outermost layer with a mass of 0.01–0.1 M
⊙ at ≲1 year before explosion. We also find that the luminosity of the observed precursors can be naturally explained by the outburst that creates the dense CSM, given that the energy of the outburst is efficiently dissipated by collision with an external material, possibly generated by a previous mass eruption. We discuss possible scenarios causing eruptive mass loss based on our results.
Constraints on Solar Wind Density and Velocity Based on Coronal Tomography and Parker Solar Probe Measurements
Authors: Bunting Kaine A. , Barnard Luke , Owens Mathew J. , Morgan Huw 
Published: January 2024

Abstract
Previous work has established an empirical relationship between densities gained from coronal rotational tomography near the ecliptic plane with solar wind outflow speeds at heliocentric distance r
0 = 8R
⊙. This work aims to include solar wind acceleration, and thus velocity profiles out to 1 au. Inner boundary velocities are given as a function of normalized tomographic densities, ρ

N
, as

V

0

=

75
∗

e

−

5.2
*

ρ

N

+
108

, and typically range from 100 to 180 km s−1. The subsequent acceleration is defined as

V
(
r
)
=

V

0

1
+

α

IP

1
−

e

−

r
−

r

0

/

r

H

, with α
IP ranging between 1.75 and 2.7, and r
H between 50 and 35 R
⊙ dependent on V
0. These acceleration profiles approximate the distribution of in situ measurements by Parker Solar Probe (PSP) and other measurements at 1 au. Between 2018 November and 2021 September these constraints are applied using the HUXt model and give good agreement with in situ observations at PSP, with a ∼6% improvement compared with using a simpler constant acceleration model previously considered. Given the known tomographical densities at 8 R
⊙, we extrapolate density to 1 au using the model velocities and assuming mass flux conservation. Extrapolated densities agree well with OMNI measurements. Thus coronagraph-based estimates of densities define the ambient solar wind outflow speed, acceleration, and density from 8 R
⊙ to at least 1 au. This sets a constraint on more advanced models, and a framework for forecasting that provides a valid alternative to the use of velocities derived from magnetic field extrapolations.
Improved Orthorectification and Empirical Reduction of Topographic Effects in Monostatic Mini-RF S-band Observations of the Moon
Authors: Fassett Caleb I. , Bramson Ali M. , Cahill Joshua T. S. , Harris Cameron P. , Morgan Gareth A. , Neish Catherine D. , Nypaver Cole A. , Patterson G. Wesley , Rivera-Valentin Edgard , Taylor Patrick A. , Thomson Bradley J. ,   the Mini-RF Team
Published: January 2024

Abstract
The Miniature Radio Frequency instrument (Mini-RF) on the Lunar Reconnaissance Orbiter obtained widespread synthetic aperture radar observations of the Moon in the S band (12.6 cm), including nearly complete coverage at both lunar poles. The currently archived monostatic data have spatial offsets from the lunar reference frame, making them more difficult to compare to other data sets. To address this issue, we have developed a new algorithm for spatially controlling the Mini-RF S-band monostatic data set and orthorectifying these data onto lunar topography. Additionally, as the influence of incidence angle changes on radar observations is well known, we describe an empirical approach to account for variations in observation geometry and surface topography. Individual radar swaths and mosaics produced using this method more clearly show the variability in scattering behavior due to changes in lunar regolith properties and suppress some of the behavior arising from these topographic effects alone. Once these terrain effects are taken into account, we find that areas of permanent shadow at both poles have a higher median radar reflectivity than nonpermanently shadowed regions, but the polarization behavior of shadowed versus unshadowed areas is largely similar. The higher radar reflectivity in permanent shadow is likely the result of physical or compositional differences in these unique environments, though the precise cause remains uncertain. The results here illustrate how reducing the influence of topography and geometry effects in Mini-RF radar data may enable better characterization of lunar geologic units, regolith structure, and potential areas hosting volatile deposits at the lunar poles.
Head and neck cancer pain
Authors: Sarumpaet Venny Tiursani , Dewi Yussy Afriani , Mahdiani Sally 
Published: January 2024

Background: Pain is a condition that often occurs in patients with head and neck cancer. Pain in patients with malignancy occurs mostly due to metastatic processes.
Method: This research is a cross-sectional descriptive study to measure variables using the VAS, BPI, HADS, and LANSS questionnaires.
Result: 127 subjects met the inclusion and exclusion criteria. Most patients with were male (63.8%), with the most ages being in the 46–55 year group (33.9%). Most patients were in stage III (48%), with the most diagnosed being nasopharyngeal malignancy (42.5%). About 60.6% of patients have received pain management according to WHO Step 2 and most suffered from neuropathic pain (65.8%) with the most pain intensity being moderate pain (53.5%). Pain interfered most with activities (91.3%) and as many as 64.6% experienced depression.
Conclusion: A description of pain in head and neck patients is needed for good management of malignancy and pain management.
Durable Learning Strategies in Nursing Education: State-of-the-Evidence Review
Authors: Mechtel Marci , Kitt-Lewis Erin , Reaves Crista , Sinacori Barbara , O'Brien Tara , Logan Paul , Rimbey Patrice , Streiff Kimberly , Phillips Kathleen 
Published: January 2024

Background:
Health professions (HP) students must achieve durable learning (DL) to transfer and apply knowledge from the classroom to the clinical setting. This review examines the state of the science of classroom-based DL in HP.

Method:
The Joanna Briggs Systematic Review Methodology was used. MEDLINE, CINAHL, PsycINFO, and ERIC databases were searched for articles published from 2006 to 2022. A total of 2,000 titles were identified for review, with 51 studies being selected for inclusion.

Results:
Multiple classroom-based learning strategies generally reported as being effective were identified, including flipped classroom, educational technology, spaced learning, team-based learning, concept mapping and schema, testing, and case study and problem-based learning.

Conclusion:

Although DL has been proven to be effective in the classroom setting for HP, no one type has been shown to be more effective than others. Additional research is needed within the context of transferring knowledge to clinical settings and in nursing education.

[
J Nurs Educ
. 2024;63(1):24–31.]
Les infrastructures portuaires dans l’iconographie monétaire romaine
Authors: Grimaldi Florian 
Published: January 2024

« Comment représente-t-on un port ? » C’est cette question qui a mené à la constitution d’un corpus de monnaies portant des représentations de ports ou d’éléments d’infrastructures liées à l’activité portuaire. Cette recherche s’appuie sur l’étude iconographique d’émissions républicaines, impériales et provinciales allant de la fin du Ier s. av. J.-C. à la fin du IIIe s. apr. J.-C. Elle a pour but de mettre en évidence les types extrêmement divers de représentations utilisés, allant de l’évocation à la représentation plus ou moins réaliste de bassins portuaires, ainsi que des éléments tels que phares, amers, navalia. Elle a permis de dégager une tendance à une certaine convergence des formes dans la représentation des bassins portuaires. Une standardisation, plus ou moins conventionnelle, a pu être mise en exergue, dans la représentation des structures de signalisations. Les premières conclusions de cette étude ont soulevé de nouvelles problématiques qui n’ont pu être traitées dans cet article comme l’évolution des typologies, ou la raison d’être de ces émissions…