Pengaruh Model Mind Mapping Berbantuan Media Couple Cards Terhadap Hasil Belajar IPA Siswa Kelas V MIS Bidayatul Hidayah Rafa Tahun Ajaran 2019/2020

Penelitian ini bertujuan untuk mengetahui; (1) seberapa besar peningkatan hasil belajar IPA setelah diterapkan model mind mapping berbantuan media couple cards pada siswa kelas V MIS Bidayatul Hidayah Rafa tahun ajaran 2019/2020, (2) seberapa besar perbedaan hasil belajar IPA menggunakan model mind mapping berbantuan media couple cards dengan pembelajaran konvensional pada siswa kelas V MIS Bidayatul Hidayah Rafa Tahun Ajaran 2019/2020, dan (3) seberapa besar pengaruh model mind mapping berbantuan media couple cards terhadap hasil belajar IPA siswa kelas V MIS Bidayatul Hidayah Rafa Tahun Ajaran 2019/2020. Penelitian ini merupakan penelitian kuantitatif eksperimen jenis Quasi Eksperimental Design dengan tipe pretest-posttest group design. Populasi penelitian ini adalah seluruh siswa/i kelas V yang berjumlah 72 orang, sedangkan sampel penelitian adalah siswa/i kelas V Yordania yang berjumlah 23 orang sebagai kelas eksperimen dan siswa/i kelas V Irak yang berjumlah 22 orang sebagai kelas kontrol. Instrumen penelitian ini menggunakan pretest dan posttest. Teknik pengumpulan data dengan wawancara, studi dokumentasi, dan tes. Sedangkan teknik analisis data dengan uji t. Hasil penelitian menunjukkan rata-rata nilai pretest kelas eksperimen sebesar 51,9565 sedangkan nilai posttest nya sebesar 77,8261 dengan nilai dari 65 ke 90. Sedangkan rata-rata nilai pretest kelas kontrol sebesar 44,545 sedangkan nilai posttest nya sebesar 66,364 dengan nilai dari 60 ke 80. Berdasarkan hasil perhitungan uji t, didapatkan thitung = 4,941 dengan ttabel = 2,021 pada taraf signifikan 5 % dan dk 43. Dengan demikian, thitung > ttabel maka Ha diterima dan H0 ditolak

Pengaruh Non Perfoming Loan (NPL), Dewan Komisaris Independen, Return on Assets (ROA) dan Capital Adequacy Ratio (CAR) terhadap Return Saham ( Studi Empiris pada Bank Umum BUMN Periode 2012-2016)

Bank Umum Badan Usaha Milik Negara (BUMN) merupakan market leader dari pangsa pasar sebesar 34,95 %. Fenomena terjadinya krisis ekonomi global pada tahun 2008 menyebabkan dampak perlambatan pertumbuhan ekonomi di Indonesia hingga tahun 2016. Terjadinya perlambatan pertumbuhan ekonomi ini mengakibatkan terjadinya penurunan kinerja Bank Umum Badan Usaha Milik Negara (BUMN). Melemahnya kinerja perbankan ini mengakibatkan laju pertumbuhan kredit serta laba Bank BUMN ini mengalami penurunan. Apabila kondisi ini terus berlanjut maka Bank Umum BUMN akan terancam, dengan demikian kemungkinan Bank Umum BUMN mengalami penurunan return saham. Penelitian ini menggunakan dua jenis variabel, yaitu variabel bebas terdiri dari rasio NPL, Komisaris Independen, ROA, dan CAR. Variabel terikat yaitu return saham. Tujuan dari penelitian ini adalah untuk mengetahui pengaruh NPL, Komisaris Independen, ROA, dan CAR terhadap return saham Bank Umum Badan Usaha Milik Negara (BUMN) baik secara simultan maupun parsial. Data yang digunakan dalam penelitian ini diperoleh dari data laporan keuangan. Populasi dalam penelitian ini adalah Bank Umum BUMN tahun 2012-2016. Teknik purposive sampling digunakan untuk pengambilan sampel dan diperoleh sampel sebanyak 4 perusahaan dengan kurun waktu lima tahun secara triwulan, sehingga didapat 80 data yang diobservasi. Metode analisis data dalam penelitian ini adalah analisis regresi data panel. Hasil penelitian menunjukkan bahwa variabel NPL, Komisaris Independen, ROA, dan CAR secara simultan berpengaruh terhadap return saham. Secara parsial, variabel NPL, Komisaris Independen, ROA, dan CAR tidak berpengaruh terhadap return saham. Berdasarkan hasil penelitian ini, apabila investor ingin melakukan investasi pada Bank BUMN maka investor tidak melihat dari aspek NPL, Komisaris Independen, ROA, dan CAR terhadap return saham. Kata Kunci : Return Saham, NPL, Komisaris Independen, ROA, CA

Photometry of the trans-neptunian object 1993 SC.

We obtained broadband photometry of the Trans-Neptunian Object 1993 SC with the Steward Observatory 1.5-m telescope near Mt. Bigelow, Arizona and the Lunar and Planetary Laboratory CCD on 8 October 1996. 1993 SC exhibited a constant brightness (V = 22.67) with a 1 sigma scatter about the average of 0.06 magnitudes during a five hour interval. In addition, we obtained observations of 1993 SC with the Steward Observatory 2.3-m telescope on Kitt Peak, Arizona during 24 - 27 November 1995. Once again 1993 SC exhibited a constant brightness (V = 22.73) with a 1 sigma scatter about the average of 0.04 magnitudes. If 1993 SC has a lightcurve, the amplitude must be at the level of 0.12 magnitudes or less. If the obliquity of 1993 SC is near zero degrees, then 1993 SC is spherical with a semi-major to semi-minor axis ratio less than or equal to 1.12. A spherical nature for 1993 SC may be the result of self gravity exceeding the tensile strength of the material in the interior of 1993 SC. If the obliquity of 1993 SC is large, then 1993 SC could have an irregular shape. The steady intrinsic brightness for 1993 SC suggests that the object has a relatively uniform surface albedo. Our photometry and the assumption of a comet-like albedo (0.04) indicates that the diameter of 1993 SC is ~ 240 km

Suppressive effects of co-stimulatory molecule expressions on mouse splenocytes by anti-allergic agents in vitro.

The influence of anti-allergic drugs, epinastine hydrochloride (EP) and disodium cromoglycate (DSCG), on the co-stimulatory molecule expression was examined using in vitro cell culture technique. Spleen cells obtained from BALB/c mice 10 days after immunization with haemocyanin absorbed to aluminium hydroxide were cultured in the presence of 100.0 microg/ml haemocyanin and various concentrations of the agents. Low concentrations (<1.5 x 10(-4)M) of EP and DSCG did not influence spleen cell blastic activity induced by antigenic stimulation, whereas these agents caused significant inhibition of spleen cell activation when 2 x 10(-4) M of the agents were added to cell cultures. EP and DSCG also did not affect blastic activity of sensitized splenic T cells by anti-CD3 monoclonal antibody stimulation even when these cells were cultured in the presence of 2 x 10(-4) M of the agents. We next examined the influence of EP and DSCG on the expression of co-stimulatory molecules on spleen cells in response to antigenic stimulation. Sensitized spleen cells were cultured in the presence of 2 x 10(-4)M of the agents and the expression of molecules were examined by flow cytometer 24h later. EP and DSCG suppressed the expression of costimulatory molecules, CD40 and CD80, but not CD86, on splenic B cells which were enhanced by antigenic stimulation in vitro

The temperature of nitrogen on Pluto

With Hapke scattering theory and absorption coefficients derived from our laboratory measurements of solid N2 we have modeled the spectrum of Triton. By comparing a Hapke scattering model to the measured spectrum from Triton, we determined the temperature of the N2 on the satellite's surface to be 38 (+2, -1) K which is in accord with the measurements of Voyager 2. Applying this technique to Pluto we find that the temperature of N2 on that body is 40 +/- 2 K. Other aspects of this investigation are discussed

Pluto's lower atmosphere structure and methane abundance from high-resolution spectroscopy and stellar occultations

Context: Pluto possesses a thin atmosphere, primarily composed of nitrogen, in which the detection of methane has been reported. Aims: The goal is to constrain essential but so far unknown parameters of Pluto's atmosphere such as the surface pressure, lower atmosphere thermal stucture, and methane mixing ratio. Methods: We use high-resolution spectroscopic observations of gaseous methane, and a novel analysis of occultation light-curves. Results: We show that (i) Pluto's surface pressure is currently in the 6.5-24 microbar range (ii) the methane mixing ratio is 0.5+/-0.1 %, adequate to explain Pluto's inverted thermal structure and ~100 K upper atmosphere temperature (iii) a troposphere is not required by our data, but if present, it has a depth of at most 17 km, i.e. less than one pressure scale height; in this case methane is supersaturated in most of it. The atmospheric and bulk surface abundance of methane are strikingly similar, a possible consequence of the presence of a CH4-rich top surface layer.Comment: AA vers. 6.1, LaTeX class for Astronomy & Astrophysics, 9 pages with 5 figures Astronomy and Astrophysics Letters, in pres

Discovery of carbon monoxide in the upper atmosphere of Pluto

Pluto's icy surface has changed colour and its atmosphere has swelled since its last closest approach to the Sun in 1989. The thin atmosphere is produced by evaporating ices, and so can also change rapidly, and in particular carbon monoxide should be present as an active thermostat. Here we report the discovery of gaseous CO via the 1.3mm wavelength J=2-1 rotational transition, and find that the line-centre signal is more than twice as bright as a tentative result obtained by Bockelee-Morvan et al. in 2000. Greater surface-ice evaporation over the last decade could explain this, or increased pressure could have caused the atmosphere to expand. The gas must be cold, with a narrow line-width consistent with temperatures around 50 K, as predicted for the very high atmosphere, and the line brightness implies that CO molecules extend up to approximately 3 Pluto radii above the surface. The upper atmosphere must have changed markedly over only a decade since the prior search, and more alterations could occur by the arrival of the New Horizons mission in 2015.Comment: 5 pages; accepted for publication in MNRAS Letter

Anisotropic inverse Compton scattering of photons from the circumstellar disc in PSR B1259-63

The gamma-ray binary system PSR B1259-63 consists of a 48 ms pulsar orbiting a Be star. The system is particularly interesting because it is the only gamma-ray binary system where the nature of the compact object is known. The non-thermal radiation from the system is powered by the spin-down luminosity of the pulsar and the unpulsed radiation originates from the stand-off shock front which forms between the pulsar and stellar wind. The Be star/optical companion in the system produces an excess infrared flux from the associated circumstellar disc. This infrared excess provides an additional photon source for inverse Compton scattering. We discuss the effects of the IR excess near periastron, for anisotropic inverse Compton scattering and associated gamma-ray production. We determine the infrared excess from the circumstellar disc using a modified version of a curve of growth method, which takes into account the changing optical depth through the circumstellar disc during the orbit. The model is constrained using archive data and additional mid-IR observations obtained with the VLT during January 2011. The inverse Compton scattering rate was calculated for three orientations of the circumstellar disc. The predicted gamma-ray light curves show that the disc contribution is a maximum around periastron and not around the disc crossing epoch. This is a result of the disc being brightest near the stellar surface. Additional spectroscopic and near-infrared observations were obtained of the system and these are discussed in relation to the possibility of shock heating during the disc crossing epoch.Comment: 15 pages, 14 figures and 4 tables. MNRAS in press. Updated references, correction of typos in a few of the equations in sec. 5.2 and appendix, and other minor typo correction

The Surfaces of Pluto and Charon

Much of the surface of Pluto consists of high-albedo regions covered to an unknown depth by Beta-N2, contaminated with CH4, CO, and other molecules. A portion of the exposed surface appears to consist of solid H2O. The remainder is covered by lower albedo material of unknown composition. The N2 ice may occur as polar caps of large extent, leaving ices and other solids of lower volatility in the equatorial regions. The low-albedo material found primarily in the equatorial regions may consist in part of solid hydrocarbons and nitriles produced from N2 and CH4 in the atmosphere or in the surface ices. Alternatively, it may arise from deposition from impacting bodies and/or the chemistry of the impact process itself. Charon's surface is probably more compositionally uniform than that of Pluto, and is covered by H2O ice with possible contaminants or exposures of other materials that are as yet unidentified. The molecular ices discovered on Pluto and Charon have been identified from near-infrared spectra obtained with Earth-based telescopes. The quantitative interpretation of those data has been achieved through the computation of synthetic spectra using the Hapke scattering theory and the optical constants of various ices observed in the laboratory. Despite limitations imposed by the availability of laboratory data on ices in various mixtures, certain specific results have been obtained. It appears that CH4 and CO are trace constituents, and that some fraction of the CH4 (and probably the CO) on Pluto is dissolved in the matrix of solid N2. Pure CH4 probably also occurs on Pluto's surface, allowing direct access to the atmosphere. Study of the nitrogen absorption band at 2.148 micrometers shows that the temperature of the N2 in the present epoch is 40 +/-2 K. The global temperature regime of Pluto can be modeled from observations of the thermal flux at far-infrared and millimeter wavelengths. The low-albedo equatorial regions must be significantly warmer than the polar regions covered by N2 (at T = 40 K) to account for the total thermal flux measured. At the present season, the diurnal skin depth of the insolation-driven thermal wave is small, and the observed mm-wave fluxes may arise from a greater depth. Alternatively, the mm-wave flux may arise from the cool, sublimation source region. The surface microstructure in the regions covered by N2 ice is likely governed by the sintering properties of this highly volatile material. The observed nitrogen infrared band strength requires that expanses of the surface be covered with cm-sized crystals of N2. Grains of H2O ice on Charon, in contrast, are probably of order 50 micrometers in size, and do not metamorphose into larger grains at a significant rate. Because of the similarities in size, density, atmosphere and surface composition between Pluto and Neptune's satellite Triton, the surface structures observed by Voyager on Triton serve as a plausible paradigm for what might be expected on Pluto. Such crater forms, tectonic structures, aeolian features, cryovolcanic structures, and sublimation-degraded topography as are eventually observed on Pluto and Charon by spacecraft will give information on their interior compositions and structures, as well as on the temperature and wind regimes over the planet's extreme seasonal cycle