Tanggung Jawab Direksi PT. Dewata Abdi Nusa Yang Pailit Kepada Konsumen (Studi Kasus Perumahan Graha Dewata Kota Malang)

Developer company PT. Dewata Abdi Nusa (DAN) bankrupted through decision 16/PAILIT/2013/PN.NIAGA.SBY. Verdict lead singer consumer losing their rights Sale and Purchase Agreement due to PT. not done, and the taxable income PT. bankrupted, consumer only serves as concurrent creditors or third party. Based provision in Law No. 8 of 1999 on Consumer Protection, and the responsibility of directors of AT Act No. 40 of 2007 Concerning Limited Liability Losses Being experienced with consumers should be settled fairly and customer is entitled to replace the loss. Should the responsibilities carried out by the board of directors is shown to the locker loss consumer losses despite differences all taxable income directors authorized their bankrupt decision switch shown to the receiver. This paper using empirical legal research with sociological juridical approach. Case used pursuant to Decision 16/PAILIT/2013/PN.NIAGA.SBY. Writers wanted to assess the responsibility of directors of the taxable income decision bankrupt shown to consumers. Research shows that the civil liability of directors addressed to the customer switch shown to the curator DAN consumer taxable income decision bankruptcy, as creditors domiciled third party concurrent or taxable income occurred bankruptcy, if directors proven do errors and neglect then the directors can be held accountable until shown to her possessions. The certificate should have been shown to be submitted earlier consumers nowadays most hearts still be under the control of Bank BRI and Bank partially again is on lie and orangutan individuals as collateral debt director of PT. DAN. The legal remedy can be done by obtaining back consumer to review their rights is only the remedy of cassation and reconsideration

Ultrasonic Method for Nonintrusive Low-Liquid-Level Sensing

The physics and fundamental principles of ultrasonic pulse echo technology are well understood, and pulse echo techniques have been used widely for measurement of materials properties such as modulus, stress, and thickness, and for defect detection and flaw characterization [1,2]

The relation between stellar magnetic field geometry and chromospheric activity cycles - I. The highly variable field of ɛ Eridani at activity minimum

The young and magnetically active K dwarf Epsilon Eridani exhibits a chromospheric activity cycle of about 3 years. Previous reconstructions of its large-scale magnetic field show strong variations at yearly epochs. To understand how Epsilon Eridani's large-scale magnetic field geometry evolves over its activity cycle we focus on high cadence observations spanning 5 months at its activity minimum. Over this timespan we reconstruct 3 maps of Epsilon Eridani's large-scale magnetic field using the tomographic technique of Zeeman Doppler Imaging. The results show that at the minimum of its cycle, Epsilon Eridani's large-scale field is more complex than the simple dipolar structure of the Sun and 61 Cyg A at minimum. Additionally we observe a surprisingly rapid regeneration of a strong axisymmetric toroidal field as Epsilon Eridani emerges from its S-index activity minimum. Our results show that all stars do not exhibit the same field geometry as the Sun and this will be an important constraint for the dynamo models of active solar-type stars

The Mixmaster Spacetime, Geroch's Transformation and Constants of Motion

We show that for $U(1)$-symmetric spacetimes on $S^3 \times R$ a constant of motion associated with the well known Geroch transformation, a functional $K[h_{ij},\pi^{ij}]$, quadratic in gravitational momenta, is strictly positive in an open subset of the set of all $U(1)$-symmetric initial data, and therefore not weakly zero. The Mixmaster initial data appear to be on the boundary of that set. We calculate the constant of motion perturbatively for the Mixmaster spacetime and find it to be proportional to the minisuperspace Hamiltonian to the first order in the Misner anisotropy variables, i.e. weakly zero. Assuming that $K$ is exactly zero for the Mixmaster spacetime, we show that Geroch's transformation, when applied to the Mixmaster spacetime, gives a new \mbox{$U(1)$-symmetric} solution of the vacuum Einstein equations, globally defined on \mbox{$S^2 \times S^1 \times R$},which is non-homogeneous and presumably exhibits Mixmaster-like complicated dynamical behavior.Comment: 25 pages, preprint YCTP-20-93, Revte

Optimization of Ultrasound-Assisted Extraction of Total Extractive Substances from Galium verum L

Ultrasound-assisted extraction (US-AE) of total extractive substances from the herb Lady's Bedstraw (Galium verum L.) is useful extraction method for its application in food manufacturing. The effect of different temperatures (T) and solventto-solid ratios (S) on the US-AE extraction yield was studied in this paper. The influence and optimum of the operating parameters (T and S) was investigated using response surface methodology (RSM). The T and S had impact on extraction yield. RSM showed that the optimal extraction parameters, which gave a maximum extraction yield of 18.7%, were T of 40 oC and S of 30 kg kg(-1). Using modeled optimized conditions, detected relative difference between predicted and experimental yield was 3.3 %. RSM successfully predicted optimal parameters and proved as useful tool for standardization of extraction conditions for bioactive components from plants important for food industry

The relation between stellar magnetic field geometry and chromospheric activity cycles – II The rapid 120-day magnetic cycle of <i>τ</i> Bootis

One of the aims of the BCool programme is to search for cycles in other stars and to understand how similar they are to the Sun. In this paper, we aim to monitor the evolution of τ Boo’s large-scale magnetic field using high-cadence observations covering its chromospheric activity maximum. For the first time, we detect a polarity switch that is in phase with τ Boo’s 120-day chromospheric activity maximum and its inferred X-ray activity cycle maximum. This means that τ Boo has a very fast magnetic cycle of only 240 days. At activity maximum τ Boo’s large-scale field geometry is very similar to the Sun at activity maximum: it is complex and there is a weak dipolar component. In contrast, we also see the emergence of a strong toroidal component which has not been observed on the Sun, and a potentially overlapping butterfly pattern where the next cycle begins before the previous one has finished

The solar wind from a stellar perspective: how do low-resolution data impact the determination of wind properties?

Alfv\'en-wave-driven 3D magnetohydrodynamic (MHD) models, which are increasingly used to predict stellar wind properties, contain unconstrained parameters and rely on low-resolution stellar magnetograms. We explore the effects of the input Alfv\'en wave energy flux and the surface magnetogram on the wind properties predicted by the Alfv\'en Wave Solar Model (AWSoM). We lowered the resolution of two solar magnetograms during solar cycle maximum and minimum using spherical harmonic decomposition. The Alfv\'en wave energy was altered based on non-thermal velocities determined from a far ultraviolet (FUV) spectrum of the solar twin 18 Sco. Additionally, low-resolution magnetograms of three solar analogues were obtained using Zeeman Doppler imaging (ZDI). Finally, the simulated wind properties were compared to Advanced Composition Explorer (ACE) observations. AWSoM simulations using well constrained input parameters taken from solar observations can reproduce the observed solar wind mass and angular momentum loss rates. The resolution of the magnetogram has a small impact on the wind properties and only during cycle maximum. However, variation in Alfv\'en wave energy influences the wind properties irrespective of the solar cycle activity level. Furthermore, solar wind simulations carried out using the low-resolution magnetogram of the three stars instead of the solar magnetogram could lead to an order of a magnitude difference in the simulated wind properties. The choice in Alfv\'en energy has a stronger influence on the wind output compared to the magnetogram resolution. The influence could be even stronger for stars whose input boundary conditions are not as well constrained as those of the Sun. Unsurprisingly, replacing the solar magnetogram with a stellar magnetogram could lead to completely inaccurate solar wind properties, and should be avoided in solar and stellar wind simulations.Comment: accepted for publication in A&