Tindak Pidana terhadap Konflik Antar Kampung dalam Perspektif Hukum Pidana

Tujuan dilakukannya penelitian ini adalah untuk mengetahui bagaimana perspektif sosiologis hukum terhadap konflik antar kampung di Indonesia dan bagaimana implementasi KUHP terhadap konflik antar kampung yang terjadi di Indonesia. Dengan menggunakan metode penelitian yuridis normatif, maka dapat disimpulkan: 1. Konflik antar kampung di Indonesia bisa terjadi karena tingginya faktor sosiologis dari masyarakat setempat yang melakukan peristiwa pidana tersebut, dari faktor disorganisasi sosial, individualisme dalam praktek politik dan ekonomi, mobilitas sosial dan konflik budaya. konflik antar kampung biasanya terjadi karena ketersinggungan anggota kelompok, kesalahpahaman, dendam, minuman keras, rasa solidaritas, kesenjangan sosial, penguasaan lahan dan hal-hal lain yang dapat membuat perpecahan. 2. Rumusan Pasal 170 dan Pasal 358 Kitab Undang-Undang Hukum Pidana telah jelas dan mengatur tentang konflik antar kampung, bukan saja karena telah terjadinya kekerasan terhadap orang dan barang yang dilakukan secara bersama-sama, namun juga dapa merugikan orang lain. Dalam Kitab Undang-Undang Hukum Pidana juga telah diatur dan dibagi tentang peranan dan pertanggungjawaban pelaku konflik antar kampung sesuai dengan Pasal 55 dan Pasal 56 KUHP. Namun implementasinya cukup sulit dalam memberikan sanksi yang adil dan efektif terhadap kerumunan massa yang melakukan konflik antar kampungtersebut. Hal ini karena dalam hukum pidana kita tidak mengenal pertanggungjawaban kolektif dan sanksi pidana lebih lanjut ditunjukkan kepada diri individu pelanggar. Menjatuhkan sanksi terhadap pelaku secara merata tidak mungkin dilakukan

The seismic properties of low-mass He-core white dwarf stars

We present here a detailed pulsational study applied to low-mass He-core white dwarfs, based on full evolutionary models representative of these objects. The background stellar models on which our pulsational analysis was carried out were derived by taking into account the complete evolutionary history of the progenitor stars, with special emphasis on the diffusion processes acting during the white dwarf cooling phase. We computed nonradial $g$-modes to assess the dependence of the pulsational properties of these objects with stellar parameters such as the stellar mass and the effective temperature, and also with element diffusion processes. We also performed a g- and p-mode pulsational stability analysis on our models and found well-defined blue edges of the instability domain, where these stars should start to exhibit pulsations. We found substantial differences in the seismic properties of white dwarfs with $M_* \gtrsim 0.20 M_{\odot}$ and the extremely low-mass (ELM) white dwarfs ($M_* \lesssim 0.20 M_{\odot}$). Specifically, $g$-mode pulsation modes in ELM white dwarfs mainly probe the core regions and are not dramatically affected by mode-trapping effects by the He/H interface, whereas the opposite is true for more massive He-core white dwarfs. We found that element diffusion processes substantially affects the shape of the He/H chemical transition region, leading to non-negligible changes in the period spectrum of low-mass white dwarfs. Our stability analysis successfully predicts the pulsations of the only known variable low-mass white dwarf (SDSS J184037.78+642312.3), and also predicts both $g$- and $p$-mode pulsational instabilities in a significant number of known low-mass and ELM white dwarfs.Comment: 14 pages, 15 figures, 2 tables. To be published in Astronomy & Astrophysic

Einstein y la religión

"A pesar de sus muchas declaraciones, no sabemos del todo qué quiso significar Einstein con la palabra Dios. En su obra científica Dios fue el concepto gobernante-un concepto mal definido, porque, ¿quién puede definir a Dios?- pero un símbolo no sólo de la pasión de Einstein por lo asombroso y lo bello, sino también de aquel intuitivo sentido de comunión con el Universo, que fue el distintivo de su genio." Banesh Hoffmann, Albert Einstein.  

Hydrocarbon Source Rock Potential of the Sinamar Formation, Muara Bungo, Jambi

DOI: 10.17014/ijog.v1i1.175The Oligocene Sinamar Formation consists of shale, claystone, mudstone, sandstone, conglomeratic sandstone, and intercalation of coal seams. The objective of study was to identify the hydrocarbon source rock potential of the Sinamar Formation based on geochemichal characteristics. The analyses were focused on fine sediments of the Sinamar Formation comprising shale, claystone, and mudstone. Primary data collected from the Sinamar Formation well and outcrops were analyzed according to TOC, pyrolisis analysis, and gas chromatography - mass spectometry of normal alkanes that include isoprenoids and sterane. The TOC value indicates a very well category. Based on TOC versus Pyrolysis Yields (PY) diagram, the shales of Sinamar Formation are included into oil prone source rock potential with good to excellent categories. Fine sediments of the Sinamar Formation tend to produce oil and gas originated from kerogen types I and III. The shales tend to generate oil than claystone and mudstone and therefore they are included into a potential source rock

A New Timescale for Period Change in the Pulsating DA White Dwarf WD 0111+0018

We report the most rapid rate of period change measured to date for a pulsating DA (hydrogen atmosphere) white dwarf (WD), observed in the 292.9 s mode of WD 0111+0018. The observed period change, faster than 10^{-12} s/s, exceeds by more than two orders of magnitude the expected rate from cooling alone for this class of slow and simply evolving pulsating WDs. This result indicates the presence of an additional timescale for period evolution in these pulsating objects. We also measure the rates of period change of nonlinear combination frequencies and show that they share the evolutionary characteristics of their parent modes, confirming that these combination frequencies are not independent modes but rather artifacts of some nonlinear distortion in the outer layers of the star.Comment: 10 pages, 6 figures, accepted for publication in The Astrophysical Journa