1,721,247 research outputs found
Going Beyond Counting First Authors in Author Co-citation Analysis
Full text linkThe present study examines one of the fundamental aspects of author co-citation analysis (ACA) - the way co-citation
counts are defined. Co-citation counting provides the data on which all subsequent statistical analyses and mappings
are based, and we compare ACA results based on two different types of co-citation counting - the traditional type that
only counts the first one among a cited work's authors on the one hand and a non-traditional type that takes into
account the first 5 authors of a cited work on the other hand. Results indicate that the picture produced through this non-traditional author co-citation counting contains more coherent author groups and is therefore considerably clearer. However, this picture represents fewer specialties in the research field being studied than that produced through the traditional first-author co-citation counting when the same number of top-ranked authors is selected and analyzed. Reasons for these effects are discussed
Variations on the Author
Full text link“Variations on the Author” discusses two of Eduardo Coutinho’s recent films (Um Dia na Vida, from 2010, and Últimas Conversas, posthumously released in 2015) and their contribution to the general question of documentary authorship. The director’s filmography is characterized by a consistent yet self-effacing form of authorial self-inscription: Coutinho often features as an interviewer that rather than express opinions propels discourses; an interviewer that is good at listening. This mode of self-inscription characterizes him as an author who is not expressive but who is nonetheless markedly present on the screen. In Um Dia na Vida, however, Coutinho is completely absent form the image, while Últimas Conversas, on the contrary, includes a confessional prologue that moves the director from the margins to the center of his films. This article examines the ways in which these works stand out in the filmography of a director who offers new insights into the notion of cinematic authorship
Appropriate Similarity Measures for Author Cocitation Analysis
Full text linkWe provide a number of new insights into the methodological discussion about author cocitation analysis. We first argue that the use of the Pearson correlation for measuring the similarity between authors’ cocitation profiles is not very satisfactory. We then discuss what kind of similarity measures may be used as an alternative to the Pearson correlation. We consider three similarity measures in particular. One is the well-known cosine. The other two similarity measures have not been used before in the bibliometric literature. Finally, we show by means of an example that our findings have a high practical relevance.information science;Pearson correlation;cosine;similarity measure;author cocitation analysis
Dispelling the Myths Behind First-author Citation Counts
Full text linkWe conducted a full-scale evaluative citation analysis study of scholars in the XML research field to explore just how different from each other author rankings resulting from different citation counting methods actually are, and to demonstrate the capability of emerging data and tools on the Web in supporting more realistic citation counting methods. Our results contest some common arguments for the continued
use of first-author citation counts in the evaluation of scholars, such as high correlations between author rankings by first-author citation counts and other citation
counting methods, and high costs of using more realistic citation counting methods that are not well-supported by the ISI databases. It is argued that increasingly available digital full text research papers make it possible for citation analysis studies to go beyond what the ISI databases have directly supported and to employ more
sophisticated methods
Evolution of Magnetic Fields in High Mass Star Formation
No full text在此博士論文中，我分析磁場在高質量恆星形成區域所扮演的角色。般認為，磁場在恆星形成過程中扮演很重要的角色。它提供支持的力量，使得分子雲可以緩慢地塌縮，因此可以解決僅有極少比例的分子雲形成恆星的問題。另外，它可以重新分布磁通量以及轉動慣量，使得物質可以掉入中心的原恆星。然而，一直到近十年才開始有高解析度(約數角秒)的磁力線型態、而且極為有限的歸測資料。其中，次毫米波陣列是目前唯一可以偵測毫米與次毫米波段的偏極化光的陣列。這波段對恆星形成區域的塵埃輻射特別敏感。藉由觀測塵埃的熱輻射中的偏極化光，我們可以推得磁場投影的天球上的磁力線型態。利用次毫米波陣列，我研究四個在不同演化階段的高恆星形成區域：超緻密氫離子區 G5.89-0.39，塌縮原恆星核 W51 e2/e8 以及 W51 North，以及離我們最近的高質量恆星形成區域 Orion BN/KL。此外，獵戶座分子雲3 (OMC-3)中最亮的高密度核 MMS 6也是本論文的研究天體。據所分析的分子雲的運動狀態與所觀測到的複雜磁力線型態，超緻密氫離子區天體G5.89-0.39的磁場明顯的受到擾動。比較此天體中所存在的輻射壓力、氣體的力學能密度與磁壓力，我們估計輻射壓在靠近中心的高質量恆星位置的地方，有足夠的能量密度可以擾動磁場與推動附近的分子雲。在演化更早期的天體W51 e2/e8區域，我們看到被吸積盤面拉扯的磁力線型態。而在此塌縮核以外的分子雲氣中，磁場呈現非常規則的狀態。此結果傾向支持磁場主導的分裂過程。比較這兩個處於不同演化狀態的天體G5.89-0.39及W51 e2/e8，觀測所看到的磁力線分布型態，取決於恆星形成區域的演化狀態。若是中心的恆星已經釋放出足夠的能量，並且週遭的分子雲已經明顯的受到擾動，則所觀測到的磁力線可能極為複雜。而在演化比較早期的階段，磁力顯然扮演極為重要的角色—它主導分子雲氣演化到塌縮核的過程。而在演化最早期的天體MMS 6，磁通量明顯的比其他天體還低。此外，沒有更小尺度的磁力線型態存在，顯示獵戶座分子雲3的磁力線型態是非常均勻、規則的。因為磁場的投影影像容易受到投影作用的影響，我們需要更多的塌縮核的磁力線觀測數據。塌縮核W51 North磁力線已經受到分化過程的影響，其中大部分的高密度核中的磁力線方向約略一致，然而在密度最高的區域，磁力線明顯地受到規則地拉扯。我們需要一些數值模擬來解釋在這個區域所看到的磁力線型態。最後，觀測較近的高質量恆星形成區域的磁力線可以提供磁場在較小尺度的資訊。根據我們所觀測到Orion BN/KL天體內的磁力線型態，我們發現在以往所看到的較大尺度(約0.3 pc)均勻的磁場中，磁力線在比較小尺度內呈現明顯的規則、且較複雜的磁力線型態。在Orion BN/KL中，根據先前的的氨氣觀測數據顯示，此區域的分子雲處於非重力束縛態。此外，磁場方向有規則地變化方向。因此，我們推測所觀測到的磁場型態極可能是殘留的偽吸積盤面。總結，在本論文中，我發現磁場所扮演的角色隨著恆星形成區域的演化階段而改變。高解析度的磁場型態資料、分析分子雲內的氣體運動狀態、以及比較小尺度與大尺度的磁場型態對研究恆星形成區域中的磁場極為重要。In this thesis, I study the role of Magnetic (B) fields in the massive star forming process. It has been suggested that B field plays a key role in the star formation process - it sustains the molecular cloud from collapsing rapidly and helps to redistributes the flux density and angular momentum via ambipolar diffusion. However, there are limited measurements of B field strengths and also field morphologies, due to the weak signal and the limitation of instruments. The measurements of B-field morphologies associated with star-forming cores with high angular resolution, ~ a few arcseconds, are only available since recent decades. With the Submillimeter Array, the B field morphologies projected in the plane of sky (B_bot) are traced by mapping the thermal continuum emission of the dust grains at wavelengths of 870 micron. I study four massive star star forming regions in variousvolutionary stages: the collapsing core W51 e2/e8 and W51orth:dust, the Ultracompact H II (UC H II) region G5.89-0.39, andhe closest massive star forming site Orion BN/KL. The source inhe earliest evolutionary stage, the dense core MMS 6 in OMC-3, islso observed.s inferred from the gas kinematics and the complicated B fieldorphology, the B field in G5.89 is most likely been overwhelmedy the stellar feedbacks, such as expansion of the UC H II regionnd the molecular outflows. While in the collapsing core W512/e8, the hourglass-like B field associated with e2 seems to beocated in a subcritical envelope at a scale of 0.5 pc, suggestinghat the B field plays a dominant role in the formation process ofhe star-forming cores. The field geometry in W51 North:dust isomplex but organized, correlated with the fragmentation and theotation of the flattened structure. B field in Orion BN/KL shows part of the larger scale (0.5 pc) hourglass morphology. In MMS, no smaller B field structure is detected, suggesting that theield is relatively uniform across the OMC-3 filament. In thishesis, I conclude that the role of the B field varies with thevolutionary stages of the central stars. The high angularesolution B field map is crucial when study the role of the Bield in the star forming region. To understand the role of the Bield, kinematics of the molecular cloud and linking the fieldeometry with larger scale field are necessities.Contentsitle Page . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ibstract . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . iiiable of Contents . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . vist of Figures . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . viiiist of Tables . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . xitations to Previously Published Work . . . . . . . . . . . . . . . . . . . xicknowledgments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . xiii Introduction 1.1 Star formation in molecular clouds . . . . . . . . . . . . . . . . . . . 2.1.1 Magnetic Field or Turbulence Dominates Star Formation? . . 2.1.2 Previous approach to the problem . . . . . . . . . . . . . . . . 3.2 Massive Star Formation through Accretion? . . . . . . . . . . . . . . 4.3 Approach to the Problems: B field morphologies in the plane of sky . 5.3.1 Alignment Mechanism . . . . . . . . . . . . . . . . . . . . . . 5.3.2 Polarized Dust Emission . . . . . . . . . . . . . . . . . . . . . 5.3.3 The Chandrasekhar-Fermi Method . . . . . . . . . . . . . . . 6.4 Previous B? measurements: far-IR to mm . . . . . . . . . . . . . . . 6.4.1 single dish polarization: SHARC, HERTZ and SCUBA . . . . 6.4.2 interferometer: BIMA and SMA . . . . . . . . . . . . . . . . . 7.5 Structure of the thesis . . . . . . . . . . . . . . . . . . . . . . . . . . 7 Linking field geometry and collapse for the W51 e2/e8 cores 9.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10.2 Observation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12.3 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14.3.1 Continuum Emission . . . . . . . . . . . . . . . . . . . . . . . 14.3.2 Dust Polarization . . . . . . . . . . . . . . . . . . . . . . . . . 16.4 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 18.4.1 Hourglass B field Morphology inside the e2 dust ridge? . . . . 18.4.2 Hourglass B field Morphology in the e8 dust ridge? . . . . . . 19.4.3 Estimate of the Strength of the B field . . . . . . . . . . . . . 20.4.4 Characteristic Length Scales . . . . . . . . . . . . . . . . . . . 21.4.5 Role of B? from Envelope (0.5 pc) to Collapsing Cores (0.02 pc) 24.4.6 Comparison with other star formation sites . . . . . . . . . . . 25.5 Conclusion and Summary . . . . . . . . . . . . . . . . . . . . . . . . 26 field geometry in infall disk/ring system W51 North 43.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44.2 Observation and Data Reduction . . . . . . . . . . . . . . . . . . . . 46.3 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 47.3.1 Continuum emission . . . . . . . . . . . . . . . . . . . . . . . 47.3.2 Dust Polarization and the B Field . . . . . . . . . . . . . . . . 48.4 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 49.4.1 Dust continuum in collapsing cores . . . . . . . . . . . . . . . 49.4.2 Fragmentation? . . . . . . . . . . . . . . . . . . . . . . . . . . 50.4.3 B field dragged by the molecular ring? . . . . . . . . . . . . . 50.4.4 Correlation of outflow axes with B field direction and dust ridge 51.4.5 B field in massive collapsing cores . . . . . . . . . . . . . . . . 51.5 Summary . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 52 Remnant Disk in Massive Star Forming Region Orion BN/KL? 59.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 60.2 Observation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62.3 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62.3.1 Continuum Emission . . . . . . . . . . . . . . . . . . . . . . . 62.3.2 Polarization . . . . . . . . . . . . . . . . . . . . . . . . . . . . 64.3.3 Comparison of polarization at 3 mm, 1 mm and 0.87 mm . . . 65.4 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65.4.1 Dust grains being mechanically aligned? . . . . . . . . . . . . 66.4.2 Remnant dusty disk? . . . . . . . . . . . . . . . . . . . . . . . 66.4.3 Polarization from entrained flows? . . . . . . . . . . . . . . . . 68.5 Conclusion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68 Submillimeter Array Dust Polarization Image of the Ultracompact II Region G5.89-0.39 85.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 86.2 Source Description . . . . . . . . . . . . . . . . . . . . . . . . . . . . 88.3 Observation and Data Analysis . . . . . . . . . . . . . . . . . . . . . 89.4 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 91.4.1 Continuum Emission . . . . . . . . . . . . . . . . . . . . . . . 91.4.2 Dust polarization . . . . . . . . . . . . . . . . . . . . . . . . . 93.4.3 C17O 3-2 emission line . . . . . . . . . . . . . . . . . . . . . . 95.5 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 97.5.1 CO 3-2 polarization . . . . . . . . . . . . . . . . . . . . . . . . 97.5.2 The kinematics traced by C17O 3-2 emission line . . . . . . . . 98.5.3 Estimate of the B field strength . . . . . . . . . . . . . . . . . 100.5.4 Collapsing cloud or not? . . . . . . . . . . . . . . . . . . . . . 102.5.5 Compressed field? . . . . . . . . . . . . . . . . . . . . . . . . . 103.5.6 Comparison with Other Star Formation Sites . . . . . . . . . . 105.6 Conclusions and Summary . . . . . . . . . . . . . . . . . . . . . . . . 106 B field geometry in relatively quiescent core MMS 6 in OMC 2/3 123.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 123.2 Observations and Data Reduction . . . . . . . . . . . . . . . . . . . . 124.3 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 125.3.1 Polarization . . . . . . . . . . . . . . . . . . . . . . . . . . . . 125.4 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 125 Conclusion and Future Direction 129.1 Summary of Individual Source . . . . . . . . . . . . . . . . . . . . . . 130.1.1 On-going projects . . . . . . . . . . . . . . . . . . . . . . . . . 131.2 Future Direction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 132.2.1 More polarization measurements toward earlier sources . . . . 132.2.2 Linking to larger scale B field . . . . . . . . . . . . . . . . . . 133.2.3 Kinematics of the cores . . . . . . . . . . . . . . . . . . . . . . 133.2.4 Simulate B? of disks/flattened structures . . . . . . . . . . . . 133.2.5 Higher sensitivity observations . . . . . . . . . . . . . . . . . . 133ibliography 135URRICULUM VITAE 145ist of Figures.1 Schematic of structures in W51 e2/e8. . . . . . . . . . . . . . . . . . 34.2 870 ¹m and 1.3 mm continuum and polarization maps obtained withhe BIMA and SMA. . . . . . . . . . . . . . . . . . . . . . . . . . . . 35.2 –continued.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 36.3 Polarization map of the SMA restored with the BIMA synthesized beam. 37.4 Plot of polarization percentage versis normalized intensity. . . . . . . 38.5 B field maps in W51 e2 and e8. . . . . . . . . . . . . . . . . . . . . . 39.6 B field maps of the envelope and the collapsing cores in W51 e2/e8. . 40.7 Histogram of the differences between measured P.A. and a hypotheticaladial field, and the cumulative distribution. . . . . . . . . . . . . . . 41.8 Plot of position angle versus differences. . . . . . . . . . . . . . . . . 42.1 Polarization map of W51 North:dust. . . . . . . . . . . . . . . . . . . 56.1 –continue.. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 57.2 B field map of W51 North:dust . . . . . . . . . . . . . . . . . . . . . 58.1 SMA 870 ¹m continuum and its linear polarization maps. . . . . . . . 71.1 –continue . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72.1 –continue . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73.2 Map of dust continuum emission measured with BIMA and SMA . . 74.2 Polarization map of extended structures inferred 0.87 mm. . . . . . . 75.3 B field map inferred from 3 mm, 1 mm and 0.87 mm. . . . . . . . . . 76.3 B field map of extended structures inferred 0.87 mm. . . . . . . . . . 77.4 Continuum emission of the extended array data with uniform weighting. 78.4 B field map with extended array data with uniform weighting. . . . . 79.4 Retrieved NH3 map by Wilson et al. (2000). . . . . . . . . . . . . . . 80.5 B field map in Orion BN/KL with uniform weighting . . . . . . . . . 81.5 B field map in Orion BN/KL with uniform weighting. . . . . . . . . . 82.6 Dust continuum and large scale CO outflow. . . . . . . . . . . . . . . 83.1 SMA 870 ¹m continuum and polarization maps. . . . . . . . . . . . . 109.1 –continue . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 110ist of Figures.2 Maps of polarized intensity and polarization vectors. . . . . . . . . . 111.2 –continue . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 112.3 Distribution plots of polarization. . . . . . . . . . . . . . . . . . . . . 113.4 Channel maps of C17O 3-2. . . . . . . . . . . . . . . . . . . . . . . . . 114.5 Moment maps of C17O 3-2. . . . . . . . . . . . . . . . . . . . . . . . . 115.5 –continue . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 116.6 Position-Velocity diagrams of C17O 3-2. . . . . . . . . . . . . . . . . . 117.7 Spectra of C17O. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 118.8 Maps of derived mass to flux ratio and pressures. . . . . . . . . . . . 119.8 –continue . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120.1 Map of dust continuum emission measured with the SMA in MMS6 . 126.2 Map of dust continuum emission at 1.3 mm. . . . . . . . . . . . . . . 127ist of Tables.1 SMA dust polarization at 870¹m in e2 . . . . . . . . . . . . . . . . . 30.1 SMA dust polarization at 870¹m in e2 . . . . . . . . . . . . . . . . . 31.2 SMA dust polarization at 870¹m in e8 . . . . . . . . . . . . . . . . . 32.3 Derived parameters in e2 and e8 . . . . . . . . . . . . . . . . . . . . . 33.1 SMA dust polarization at 870 ¹m in W51 North:dust . . . . . . . . . 53.1 SMA dust polarization at 870 ¹m in W51 North:dust . . . . . . . . . 54.1 SMA dust polarization at 870 ¹m in W51 North:dust . . . . . . . . . 55.1 Observational parameters . . . . . . . . . . . . . . . . . . . . . . . . 70.1 SMA dust polarization at 870 ¹m in G5.89-0.39 . . . . . . . . . . . . 121.1 SMA dust polarization at 870 ¹m in G5.89-0.39 . . . . . . . . . . . . 12
Performance Evaluation of Distributed Floor Control for Push-to-Talk Service over MANET
No full text隨按即說(Push-to-talk或簡稱為PTT)服務可提供群組通訊，讓使用者之間透過一對一或是一對多的方式互相溝通。PTT類似於傳統的無線對講機，屬於半雙功通訊，也就是在同一個時間點，群組內只允許一名使用者說話，而其他使用者只能聆聽。PTT最主要的特色在於，使用者之間的通訊可以藉由簡單的按下通話按鈕而快速被建立，並不需要其他複雜的設定。目前，針對行動通訊網路，OMA(Open Mobile Alliance)組織的PoC(Push-to-talk over Cellular)計畫已訂定出PTT服務相關的通訊協定規格。OMA所訂的PoC規格是採取集中式的架構，其缺點為需要額外的成本來維護伺服器運作以及受限於伺服器能力的系統擴充度與系統可靠性。因此，有別於OMA作法，另一套採取點對點技術的服務模式被提出，在此分散式架構中，每個裝置之間是透過網際網路互相通訊。在PTT服務中， 發話權控制(Floor control)是一個相當重要的功能。當群組中同時有多名使用者按下通話按鈕時，系統會決定出唯一一個能獲得發話權的使用者。目前的無線網路中，移動式隨意網路因其不需任何基礎建設容易建構的特性而成為許多應用的最佳選擇。在這篇論文中，我們訂定了一些評估分散式floor control效能的指標，並且利用知名的網路模擬軟體NCTUns，設計不同的模擬實驗並觀察分散式floor control在移動式隨意網路上運作的優缺點。提供未來設計及實作分散式floor control方法的系統業者其參考之依據。Push-to-talk (PTT) is a service that provides one-to-one or one-to-many group communications. PTT is similar to the traditional walkie-talkie system which is a half duplex communication — while one person speaks, the other(s) just listen. The main characteristic of PTT is that the session can be established easily by pushing a button without complicated configurations. At present, PTT service is provided on cellular network. However, the interoperability is bad due to the lack of common protocol. The PoC (Push-to-talk over Cellular) project of OMA (Open Mobile Alliance) defines the protocol of PTT in cellular network. The PoC adopts centralized system architecture so that extra cost of maintaining PoC servers is required and scalability and reliability are limited by PoC servers. Different from PoC centralized approach, a distributed peer-to-peer (P2P) mode has been proposed. In P2P PTT, floor control is a critical function to service quality. When more than one user wants to speak and pushes the button, the floor owner should be quickly and properly decided by floor control. The ease of deployment makes Mobile Ad hoc NETwork (MANET) become very popular for many kinds of applications. In this thesis, we propose some performance evaluation indexes for distributed floor control over MANET, and investigate the performance of distributed floor control over MAN through a well-known network simulation tool. The simulation results indicate some guidelines for future design of distributed floor control over MANET.第一章 序論 1二章 分散式隨按即說系統 5.1分散式隨按即說系統 5.2研究動機 6.3分散式發話權控制方法 8三章 移動式隨意網路(MANET) 11.1移動式隨意網路 11.2移動式隨意網路繞送協定 12.2.1 DSDV繞送協定 14.2.2 AODV繞送協定 14四章 模擬結果與討論 16.1 效能評估指標及模擬環境介紹 16.1.1 效能評估指標 16.1.2 模擬環境介紹 18.2 模擬結果討論 19五章 結論與未來研究方向 28.1結論 28.2未來研究方向 29考文獻 3
koamabayili/VECTRON-author-checklist: VECTRON author checklist
No full textWe have done our best to complete the author checklist relating to the use of animals in the hut study. Note that the objective for the hut study was to evaluate the IRS treatment applications for residual efficacy against Anopheles mosquitoes, including the local An. coluzzii mosquito population. Cows were only used to attract mosquitoes into the huts and no tests were carried out directly on the cows. The author checklist is intended for use with studies where experiments are carried out on animals, which is why we have had such difficulty in completing this for the hut study, as many of the questions do not relate to how the cows were used
Author-wise bibliometric analysis based on entropy.
No full textAuthor-wise bibliometric analysis based on entropy.</p
- …
