PENGARUH LIKUIDITAS, SOLVABILITAS, DAN PROFITABILITAS TERHADAP HARGA SAHAM (Studi Kasus Pada Perusahaan Perbankan Yang Terdaftar Di Bursa Efek Indonesia Periode 2011-2015)

ABSTRAK Harga saham merupakan panutan untuk melihat nilai sebuah perusahaan, apabila harga saham suatu perusahaan tergolong ke dalam kriteria yang tinggi maka dapat dikatakan nilai perusahaan tersebut dalam keadaan sangat baik, sebaliknya apabila harga saham perusahaan tersebut sedang turun maka dapat dikatakan bahwa perusahaan yang bersangkutan sedang mengalami permasalahan atau sedang dalam keadaan kurang baik. Tinggi rendahnya harga saham suatu perusahaan dapat dipengaruhi oleh berbagai faktor diantaranya faktor likuiditas, solvabilitas, dan profitabilitas. Penelitian ini bertujuan untuk mengetahui pengaruh mengenai rasio likuiditas, solvabilitas, dan profitabilitas perusahaan perbankan yang terdaftar di Bursa Efek Indonesia terhadap harga saham. Rasio-rasio keuangan yang diteliti yaitu Current Ratio, Return on Investment dan Debt to Asset Ratio. Penelitian ini menggunakan metode penelitian deskriptif-asosiatif. Jumlah sample yang digunakan dalam penelitian ini adalah sebanyak 10 perusahaan perbankan yang terdaftar di Bursa Efek Indonesia pada periode 2011 sampai dengan 2015. Data yang digunakan dalam penelitian ini adalah data sekunder yang sudah terpublikasi di Bursa Efek Indonesia. Metode pengambilan sample yang digunakan adalah purposive sampling dimana pengambilan sample dilakukan berdasarkan kriteria tertentu. Metode statistik yang digunakan dalam penelitian ini adalah metode regresi linier berganda. Hasil penelitian ini menunjukkan bahwa variabel likuiditas secara parsial berpengaruh terhadap harga saham, variabel solvabilitas secara parsial tidak berpengaruh terhadap harga saham, dan variabel profitabilitas secara parsial berpengaruh terhadap harga saham. Secara simultan variabel likuiditas, solvabilitas, dan profitabilitas berpengaruh terhadap harga saham perusahaan perbankan yang terdaftar di Bursa Efek Indonesia. Kata Kunci: Likuiditas, Solvabilitas, dan Profitabilitas, serta Harga Saha

A search for L dwarf binary systems

We present analysis of HST Planetary Camera images of twenty L dwarfs identified in the course of the Two Micron All-Sky Survey. Four of the targets have faint, red companions at separations between 0.07 and 0.29 arcseconds (1.6 to 7.6 AU). In three cases, the bolometric magnitudes of the components differ by less than 0.3 magnitudes. Since the cooling rate for brown dwarfs is a strong function of mass, similarity in luminosities implies comparable masses. The faint component in the 2M0850 system, however, is over 1.3 magnitudes fainter than the primary in the I-band, and ~0.8 magnitudes fainter in M(bol). Indeed, 2M0850B is ~0.8 magnitudes fainter in I than the lowest luminosity L dwarf currently known, while the absolute magnitude we deduce at J is almost identical with M_J for Gl 229B. Theoretical models indicate a mass ratio of \~0.75. The mean separation of the L dwarf binaries in the current sample is smaller by a factor of two than amongst M dwarfs. We discuss the implications of these results for the temperature scale in the L/T transition region and for the binary frequency amongst L dwarfs.Comment: 38 pages, 11 figures; accepted for A

A Hubble Space Telescope ACS Search for Brown Dwarf Binaries in the Pleiades Open Cluster

We present the results of a high-resolution imaging survey for brown dwarf binaries in the Pleiades open cluster. The observations were carried out with the Advance Camera for Surveys onboard the Hubble Space Telescope. Our sample consists of 15 bona-fide brown dwarfs. We confirm 2 binaries and detect their orbital motion, but we did not resolve any new binary candidates in the separation range between 5.4AU and 1700AU and masses in the range 0.035--0.065~Msun. Together with the results of our previous study (Martin et al., 2003), we can derive a visual binary frequency of 13.3$^{+13.7}_{-4.3}$\% for separations greater than 7~AU masses between 0.055--0.065~M_{\sun} and mass ratios between 0.45--0.9$<q<$1.0. The other observed properties of Pleiades brown dwarf binaries (distributions of separation and mass ratio) appear to be similar to their older counterparts in the field.Comment: 29 pages, 7 figures, 6 tables, accepted for publication in Ap

PENGARUH PROMOSI DAN LOKASI TERHADAP PROSES KEPUTUSAN PEMBELIAN. (Studi Pada Konsumen Dealer Honda PT. Netral Jaya Motor Bandung)

ABSTRAK Penelitian ini bertujuan untuk mengetahui pengaruh Promosi dan Lokasi terhadap Keputusan Pembelian ( Studi pada Konsumen Dealer Honda PT.Netral Jaya Motor Bandung ). Metode yang digunakan adalah deskriptif verifikatif. Objek penelitian adalah konsumen yang berbelanja di Konsumen Dealer Honda PT.Netral Jaya Motor Bandung dengan jumlah sampel sebanyak 96 responden. Analisis data yang digunakan yaitu menggunakan analisis regresi linear berganda, korelasi berganda dan koefisien determinasi. Berdasarkan hasil analisis pengaruh promosi dan lokasi terhadap proses keputusan pembelian secara simultan adalah sebesar 284,194. Sedangkan secara parsial promosi memiliki pengaruh terhadap proses keputusan pembelian dengan koefisien korelasi sebesar 0,502 dan koefisien determinasi sebesar 50,2 %. lokasi memiliki pengaruh terhadap Proses keputusan pembelian dengan koefisien korelasi sebesar 0,158 dan koefisien determinasi sebesar 15,8% Kata Kunci : Promosi, Lokasi, Proses Keputusan Pembelia

Can Planets survive Stellar Evolution?

We study the survival of gas planets around stars with masses in the range 1-5 Msun, as these stars evolve off the Main Sequence. We show that planets with masses smaller than one Jupiter mass do not survive the Planetary Nebula phase if located initially at orbital distances smaller than (3-5) AU. Planets more massive than two Jupiter masses around low mass (1 Msun on the Main Sequence) stars survive the Planetary Nebula stage down to orbital distances of 3 AU. As the star evolves through the Planetary Nebula phase, an evaporation outflow will be established at the planet's surface. Evaporating planets may be detected using spectroscopic observations. Planets around white dwarfs with masses M_WD > 0.7 Msun are generally expected to be found at orbital radii r > 15 AU. If planets are found at smaller orbital radii around massive white dwarfs, they had to form as the result of the merger of two white dwarfs.Comment: 30 pages, 7 figures, 2 tables, accepted for publication in Ap

A Pan-STARRS 1 study of the relationship between wide binarity and planet occurrence in the Kepler field

The NASA Kepler mission has revolutionized time-domain astronomy and has massively expanded the number of known extrasolar planets. However, the effect of wide multiplicity on exoplanet occurrence has not been tested with this data set. We present a sample of 401 wide multiple systems containing at least one Kepler target star. Our method uses Pan- STARRS 1 and archival data to produce an accurate proper motion catalogue of the Kepler field. Combined with Pan-STARRS 1 SED fits and archival proper motions for bright stars, we use a newly developed probabilistic algorithm to identify likely wide binary pairs which are not chance associations. As byproducts of this we present stellar SED templates in the Pan-STARRS 1 photometric system and conversions from this system to Kepler magnitudes. We find that Kepler target stars in our binary sample with separations above 6 arcsec are no more or less likely to be identified as confirmed or candidate planet hosts than a weighted comparison sample of Kepler targets of similar brightness and spectral type. Therefore we find no evidence that binaries with projected separations greater than 3000 au affect the occurrence rate of planets with P <300 d around FGK stars.Peer reviewe

The Virgo cluster distance from 21 cm-line widths

The distance of the Virgo cluster is derived in the B band from the 21 cm-line width-absolute magnitude relation. The latter is calibrated using 18 spirals with Cepheid distances mainly from HST. The calibration is applied to a complete sample of non-peculiar spirals with i>45 deg and lying within the optical (n=49) or X-ray (n=35) contour of the cluster, resulting in a mean cluster distance of (m-M)_0=31.58+/-0.24 mag (external error) or 20.7+/-2.4 Mpc. The mean distance of subcluster A is 0.46+/-0.18 mag smaller than that of subcluster B, but the individual distances of the members of the two substructures show considerable overlap. The distance modulus is corrected by -0.07 mag for the fact that cluster members have lower H I-surface fluxes and are redder in (B-I) at a given line width than the (field) calibrators. Different sources of the B magnitudes and line widths have little effect on the resulting distance. Different precepts for the internal-absorption correction change the result by no more than +/-0.17 mag. The individual distances of the cluster members do not show any dependence on recession velocity, inclination, Hubble type or line width. The dependence on apparent magnitude reflects the considerable depth effect of the cluster. The adopted distance is in good agreement with independent distance determinations of the cluster. Combining the cluster distance with the corrected cluster velocity of 1142+/-61 km/s gives H_0=55+/-7 km/s/Mpc (external error). If the Virgo cluster distance is inserted into the tight Hubble diagram of clusters out to 11000 km/s using relative distances to the Virgo cluster one obtains a global value of H_0=57+/-7 km/s/Mpc.Comment: 37 pages, LaTeX using AAS aaspp4 style, 14 eps figures, 7 Tables; to be published in the Astrophysical Journal (Main Journal

Radio emission from Supernova Remnants

The explosion of a supernova releases almost instantaneously about 10^51 ergs of mechanic energy, changing irreversibly the physical and chemical properties of large regions in the galaxies. The stellar ejecta, the nebula resulting from the powerful shock waves, and sometimes a compact stellar remnant, constitute a supernova remnant (SNR). They can radiate their energy across the whole electromagnetic spectrum, but the great majority are radio sources. Almost 70 years after the first detection of radio emission coming from a SNR, great progress has been achieved in the comprehension of their physical characteristics and evolution. We review the present knowledge of different aspects of radio remnants, focusing on sources of the Milky Way and the Magellanic Clouds, where the SNRs can be spatially resolved. We present a brief overview of theoretical background, analyze morphology and polarization properties, and review and critical discuss different methods applied to determine the radio spectrum and distances. The consequences of the interaction between the SNR shocks and the surrounding medium are examined, including the question of whether SNRs can trigger the formation of new stars. Cases of multispectral comparison are presented. A section is devoted to reviewing recent results of radio SNRs in the Magellanic Clouds, with particular emphasis on the radio properties of SN 1987A, an ideal laboratory to investigate dynamical evolution of an SNR in near real time. The review concludes with a summary of issues on radio SNRs that deserve further study, and analyzing the prospects for future research with the latest generation radio telescopes.Comment: Revised version. 48 pages, 15 figure

Semiempirical calculation of van der Waals coefficients for alkali-metal and alkaline-earth-metal atoms

The van der Waals coefficients, C-6, C-8, and C-10 for the alkali-metal (Li, Na, K, and Rb) and alkaline-earth-metal (Be, Mg, Ca, and Sr) atoms are estimated by a combination of ab initio and semiempirical methods. Polarizabilities and atom-wall coefficients are given as a diagnostic check, and the lowest order nonadiabatic dispersion coefficient, D-8 and the three-body coefficient, C-9 are also presented. The dispersion coefficients are in agreement with the available relativistic many-body perturbation theory calculations. The contribution from the core was included by using constrained sum rules involving the core polarizability and Hartree-Fock expectation values to estimate the f-value distribution

A population genomics approach shows widespread geographical distribution of cryptic genomic forms of the symbiotic fungus Rhizophagus irregularis.

Arbuscular mycorrhizal fungi (AMF; phylum Gomeromycota) associate with plants forming one of the most successful microbe-plant associations. The fungi promote plant diversity and have a potentially important role in global agriculture. Plant growth depends on both inter- and intra-specific variation in AMF. It was recently reported that an unusually large number of AMF taxa have an intercontinental distribution, suggesting long-distance gene flow for many AMF species, facilitated by either long-distance natural dispersal mechanisms or human-assisted dispersal. However, the intercontinental distribution of AMF species has been questioned because the use of very low-resolution markers may be unsuitable to detect genetic differences among geographically separated AMF, as seen with some other fungi. This has been untestable because of the lack of population genomic data, with high resolution, for any AMF taxa. Here we use phylogenetics and population genomics to test for intra-specific variation in Rhizophagus irregularis, an AMF species for which genome sequence information already exists. We used ddRAD sequencing to obtain thousands of markers distributed across the genomes of 81 R. irregularis isolates and related species. Based on 6 888 variable positions, we observed significant genetic divergence into four main genetic groups within R. irregularis, highlighting that previous studies have not captured underlying genetic variation. Despite considerable genetic divergence, surprisingly, the variation could not be explained by geographical origin, thus also supporting the hypothesis for at least one AMF species of widely dispersed AMF genotypes at an intercontinental scale. Such information is crucial for understanding AMF ecology, and how these fungi can be used in an environmentally safe way in distant locations