PERLINDUNGAN KONSUMEN TERHADAP PRODUK POMADE TANPA IZIN EDAR (SUATU PENELITIAN DI KOTA BANDA ACEH)

ABSTRAKHaiter Noventri,2017PERLINDUNGAN KONSUMEN TERHADAP PRODUK POMADE TANPA IZIN EDAR (suatu penelitian di Kota Banda Aceh)Fakultas Hukum Universitas Syiah Kuala(v,56),pp.,bibl.RISMAWATI, S. H., M. HumPasal 10 Keputusan Kepala Badan Pengawas Obat dan Makanan Republik Indonesia Nomor HK.00.05.4.1745 Tahun 2003 tentang Kosmetik menyatakan bahwa setiap produk kosmetik sebelum diedarkan diwajibkan kepada produsen kosmetik tersebut untuk mendaftarkan produknya guna mendapatkan hak izin edar. Namun di Banda Aceh peredaran merek-merek Pomade yang tidak memiliki hak izin edar saat ini semakin banyak, terlebih maraknya toko-toko online, tempat pangkas, dan oulet-oulet resmi merek Pomade tertentu yang menjual Pomade tanpa izin edar.Tujuan penulisan skripsi ini untuk menjelaskan bagaimana tanggung jawab yang dibebankan kepada produsen, menjelaskan upaya hukum yang dilakukan oleh konsumen yang telah dirugikan karena mengunakan Pomade tanpa izin edar dan menjelaskan bagaimana tanggung jawab dari BPOM Kota Banda Aceh terhadap beredarnya produk Pomade tanpa izin edar yang telah merugikan pihak konsumen.Data dalam penelitian skripsi ini diperoleh dengan penelitian kepustakaan dan penelitian lapangan. Penelitian kepustakaan dilakukan untuk memperoleh data sekunder dengan cara mempelajari literatur dan perundang-undangan yang berlaku, sedangkan penelitian lapangan digunakan untuk memperoleh data primer melalui wawancara dengan responden dan informan.Hasil penelitian menjelaskan bahwa tanggung jawab produsen Pomade tanpa izin edar terhadap konsumen yang mengalami kerugian ialah; Menganti produk dengan yang baru dan mengembalikan uang pembelian produk pomade. Upaya hukum yang dapat dilakukan oleh konsumen Pomade atas pelanggaran haknya, yaitu konsumen dapat memilih menggunakan beberapa upaya hukum, seperti lansung mengadu kepada produsen Pomade, melalui BPSK dan melalui jalur pengadilan umum. Tanggung jawab BPOM Banda Aceh terhadap beredarnya produk Pomade tanpa izin edar, ialah dengan menyita produk Pomade tanpa izin edar yang beredar, melakukan pembinaan terhadap produsen, melakukan Penyidakan dan pengawasan berkala, membentuk program Unit Layanan Konsumen (ULK), Komunikasi, Informasi dan Edukasi (KIE), dan kampanye KLIK. Disarankan kepada pemerintah agar lebih merata dalam melakukan sosialisasi mengenai tangung jawab produsen Pomade dan hak-hak konsumen. Juga disarankan pihak pemerintah untuk dapat membentuk adanya BPSK di Banda Aceh. kepada pihak BPOM agar dapat lebih merata dalam melakukan penyidakan terhadap semua jenis kosmetik

On the metallicity of open clusters. III. Homogenised sample

Open clusters are known as excellent tools for various topics in Galactic research. For example, they allow accurately tracing the chemical structure of the Galactic disc. However, the metallicity is known only for a rather low percentage of the open cluster population, and these values are based on a variety of methods and data. Therefore, a large and homogeneous sample is highly desirable. In the third part of our series we compile a large sample of homogenised open cluster metallicities using a wide variety of different sources. These data and a sample of Cepheids are used to investigate the radial metallicity gradient, age effects, and to test current models. We used photometric and spectroscopic data to derive cluster metallicities. The different sources were checked and tested for possible offsets and correlations. In total, metallicities for 172 open cluster were derived. We used the spectroscopic data of 100 objects for a study of the radial metallicity distribution and the age-metallicity relation. We found a possible increase of metallicity with age, which, if confirmed, would provide observational evidence for radial migration. Although a statistical significance is given, more studies are certainly needed to exclude selection effects, for example. The comparison of open clusters and Cepheids with recent Galactic models agrees well in general. However, the models do not reproduce the flat gradient of the open clusters in the outer disc. Thus, the effect of radial migration is either underestimated in the models, or an additional mechanism is at work. [abridged]Comment: Accepted for publication in Astronomy and Astrophysics: 18 pages, 10 figures, 4 table

Metallicity determination of M dwarfs - Expanded parameter range in metallicity and effective temperature

Context. Reliable metallicity values for M dwarfs are important for studies of the chemical evolution and advancement of planet formation theory in low-mass environments. Historically the determination of stellar parameters of low-mass stars has been challenging due to the low surface temperature, causing several molecules to form in the photospheric layers. In our work we use the fact that infrared high-resolution spectrographs have opened up a new window for investigating M dwarfs. Aims. Metallicity determination using high-resolution spectra is more accurate than the use of low-resolution spectra, but rather time-consuming. In this paper we expand our sample analyzed with this precise method both in metallicity and effective temperature in order to build up a calibration sample for a future revised empirical calibration. Methods. Because of the relatively few molecular lines in the J-band, continuum rectification is possible for high-resolution spectra, allowing the stellar parameters to be determined with greater accuracy than using optical spectra. The metallicity was determined using synthetic spectral fitting of several atomic species. Results. We have analyzed sixteen targets, with a range of effective temperature from 3350-4550 K. The resulting metallicities lie between -0.5 < [M/H] < +0.4. A few targets have previously been analyzed using low-resolution spectra, and we find a rather good agreement with our values. A comparison with available photometric calibrations shows varying agreement, and the spread within all empirical calibrations is large. Conclusions. Including the targets from our previous paper, we have analyzed 28 M dwarfs using high-resolution infrared spectra. The targets spread approximately one dex in metallicity and 1400 K in effective temperature. For individual M dwarfs we achieve uncertainties of 0.05 dex and 100 K on average.Comment: 13 page

Gaia FGK Benchmark Stars and their reference parameters

In this article we summarise on-going work on the so-called Gaia FGK Benchmark Stars. This work consists of the determination of their atmospheric parameters and of the construction of a high-resolution spectral library. The definition of such a set of reference stars has become crucial in the current era of large spectroscopic surveys. Only with homogeneous and well documented stellar parameters can one exploit these surveys consistently and understand the structure and history of the Milky Way and therefore other of galaxies in the Universe.Comment: to appear in ASI Conference Series, 2014, Vol. 10 for the Workshop of Spectral Libraries held in Lyon, Oct. 201

Metallicity determination of M dwarfs - High-resolution IR spectroscopy

Context. Several new techniques to determine the metallicity of M dwarfs with better precision have been developed over the last decades. However, most of these studies were based on empirical methods. In order to enable detailed abundance analysis, standard methods established for warmer solar-like stars, i.e. model-dependent methods using fitting of synthetic spectra, still need to be used. Aims. In this work we continue the reliability confirmation and development of metallicity determinations of M dwarfs using high- resolution infrared spectra. The reliability was confirmed though analysis of M dwarfs in four binary systems with FGK dwarf companions and by comparison with previous optical studies of the FGK dwarfs. Methods. The metallicity determination was based on spectra taken in the J band (1.1-1.4 {\mu}m) with the CRIRES spectrograph. In this part of the infrared, the density of stellar molecular lines is limited, reducing the amount of blends with atomic lines enabling an accurate continuum placement. Lines of several atomic species were used to determine the stellar metallicity. Results. All binaries show excellent agreement between the derived metallicity of the M dwarf and its binary companion. Our results are also in good agreement with values found in the literature. Furthermore, we propose an alternative way to determine the effective temperature of M dwarfs of spectral types later than M2 through synthetic spectral fitting of the FeH lines in our observed spectra. Conclusions. We have confirmed that a reliable metallicity determination of M dwarfs can be achieved using high-resolution infrared spectroscopy. We also note that metallicites obtained with photometric metallicity calibrations available for M dwarfs only partly agree with the results we obtain from high-resolution spectroscopy.Comment: 18 page

Gaia FGK Benchmark Stars: Effective temperatures and surface gravities

Large Galactic stellar surveys and new generations of stellar atmosphere models and spectral line formation computations need to be subjected to careful calibration and validation and to benchmark tests. We focus on cool stars and aim at establishing a sample of 34 Gaia FGK Benchmark Stars with a range of different metallicities. The goal was to determine the effective temperature and the surface gravity independently from spectroscopy and atmospheric models as far as possible. Fundamental determinations of Teff and logg were obtained in a systematic way from a compilation of angular diameter measurements and bolometric fluxes, and from a homogeneous mass determination based on stellar evolution models. The derived parameters were compared to recent spectroscopic and photometric determinations and to gravity estimates based on seismic data. Most of the adopted diameter measurements have formal uncertainties around 1%, which translate into uncertainties in effective temperature of 0.5%. The measurements of bolometric flux seem to be accurate to 5% or better, which contributes about 1% or less to the uncertainties in effective temperature. The comparisons of parameter determinations with the literature show in general good agreements with a few exceptions, most notably for the coolest stars and for metal-poor stars. The sample consists of 29 FGK-type stars and 5 M giants. Among the FGK stars, 21 have reliable parameters suitable for testing, validation, or calibration purposes. For four stars, future adjustments of the fundamental Teff are required, and for five stars the logg determination needs to be improved. Future extensions of the sample of Gaia FGK Benchmark Stars are required to fill gaps in parameter space, and we include a list of suggested candidates.Comment: Accepted by A&A; 34 pages (printer format), 14 tables, 13 figures; language correcte

Stellar Fluxes as Probes of Convection in Stellar Atmospheres

Convection and turbulence in stellar atmospheres have a significant effect on the emergent flux from late-type stars. The theoretical advancements in convection modelling over recent years have proved challenging for the observers to obtain measurements with sufficient precision and accuracy to allow discrimination between the various predictions. An overview of the current observational techniques used to evaluate various convection theories is presented, including photometry, spectrophotometry, and spectroscopy. The results from these techniques are discussed, along with their successes and limitations. The prospects for improved observations of stellar fluxes are also given.Comment: 3 pages, 1 figure; to appear in Convection in Astrophysics, Proc. IAUS 239, F.Kupka, I.W. Roxburgh, K.L. Chan ed