Latitude variation of recurrent fluxes in the outer solar system

Recurrent low energy (greater than or = to 0.5 MeV) proton flux enhancements, reliable indicators of corotating plasma interaction regions, were observed on the Voyager 1 and 2 and Pioneer 11 spacecraft in the heliographic latitude range 2 deg S to 23 N and the heliocentric radial range 11 to 20 AU. After a period of rather high correlation between fluxes at different latitudes in early 1983, distinct differences developed in the fluxes during an overall flux decrease. The flux intensities returned to higher levels in early 1984 and differences in both the recurrence frequency and flux intensity persisted into 1985, as Voyager 1 traveled to 23 AU and 25 N latitude. Intercomparison of data from the three spacecraft indicates that the flux differences are most likely due to latitudinal rather than radial or temporal variations

Pengaturan Hukum Mengenai Pemalsuan Uang Rupiah Menurut Pasal 244 Sampai Dengan Pasal 252 Kuhp

Tujuan dilakukannya penelitian ini adalah untuk mengetahui bagaimana pengaturan hukum mengenai tindak pidana pemalsuan uang rupiah menurut Pasal 244 sampai dengan Pasal 252 KUHP dan bagaimana tindak pidana pemalsuan uang rupiah menurut Undang-Undang Republik Indonesia Nomor 7 Tahun 2011 tentang Mata Uang. Dengan menggunakan metode penelitian yuridis normatif, disimpulkan: 1. Ketentuan tindak pidana pemalsuan uang yang diatur dalam Kitab Undang-Undang Hukum Pidana belum mengatur secara komprehensif jenis perbuatan tersebut dan sanksi yang diancamkan. Oleh karena itu ketentuan-ketentuan hukum mengenai tindak pidana pemalsuan uang disempurnakan dalam Undang-Undang Republik Indonesia Nomor 7 Tahun 2011 tentang Mata Uang. 2.Tindak pidana pemalsuan uang rupiah menurut Undang-Undang Republik Indonesia Nomor 7 Tahun 2011 tentang Mata Uang telah diatur secara lebih lengkap dan terinci sebagaimana diatur dalam Pasal 33 sampai dengan Pasal 41 pengaturan mengenai ketentuan pidana terkait masalah penggunaan, peniruan, Perusakan, dan pemalsuan Rupiah

Effect of Salinity on Glycogen Content in the Brine Shrimp, Artemia salinas, of Great Salt Lake

The brine shrimp, Artemia salinas, is one of the few organisms to be found in the hostile environment of the Great Salt Lake. Salt concentrations in the lake are found to exceed those in the oceans. In such an environment, the utilization of energy, even after it has been procured, presents a problem. The life inhabiting the lake has developed extraordinary adaptations to this and similar problems. Electron micrographs produced by Dr. Nabil Youssef of Utah State University have revealed that unusual quantities of glycogen can be found in the muscle of brine shrimp taken from the Great Salt Lake. The glycogen was found to be associated in large packets rather than being dispersed in small quantities throughout the tissue. It was al so observed that the mitochondria were small, a tendency that might indicate anaerobic rather than aerobic respiration. These observations led to the initiation of this project. Samples of Artemia were collected from the Great Salt Lake and analyzed for glycogen content in an effort to determine the effect of salinity on the mode of respiration

Intricacies of development : the impact of maternal experience and isolation on the social development of juvenile male rats

Reproductive experience induces changes in females. Parity-related differences in maternal treatment of offspring can induce enduring changes in offspring. The relationships between maternal experience, early social isolation, and development were explored in rodents in this experiment. Male rats were weaned from multiparous (MP) and primiparous (PP) mothers and placed into isolation or social housing for four weeks. They were then observed in a social-interaction test. Social behavior and neural oxytocin and vasopressin were assessed post-testing, while corticosterone levels were measured across the four weeks. Weaning was extremely stressful for all offspring. PP- and MP-raised pups exhibited differences in social behavior, and trends towards different hormonal and neural profiles. The isolation paradigm was examined in a multidimensional fashion, revealing novel and provocative associations. This study further clarified some of the many ways that offspring development may be altered

Solar modulation and interplanetary gradients of the galactic electrons flux, 1977 - 1984

The flux of electrons with energy from approx. 10 to 180 MeV measured with the electron telescope on the Voyager 1 and 2 spacecraft in the heliocentric radial range 1 - 22 AU between 1977 and 1984 is reported. Jovian electrons were clearly observable between 1978 and 1983 (radial range 2 - 12 AU) at energies below approx. 50 MeV. Above approx. 50 MeV the electron intensity exhibited temporal variations generally related to the 11 year modulation of protons 75 MeV. The overall magnitude of the electron intensity changes between the maximum intensity observed in 1977 and the minimum intensity in 1981 was a factor approx. 2, also comparable to that observed for 75 MeV protons. By early 1985 the electron intensity had apparently recovered to the level observed in 1977 whereas the proton intensity was still about 20% lower. A detailed interpretation of these electron variations in all energy channels depends on an accurate subtraction of background induced by energetic protons of a few 100 MeV. This subtraction is facilitated by calibration results at several energies

The Energy Spectrum of Jovian Electrons in Interplanetary Space

The energy spectrum of electrons with energies approx 10 to approx 180 MeV measured with the electron telescope on the Voyager 1 and 2 spacecraft in interplanetary space from 1978 to 1983 is studied. The kinetic energy of electrons is determined by double dE/dx measurements from the first two detectors (D sub 1, D sub 2) of a stack of eight solid state detectors and by the range of particle penetration into the remaining six detectors (D sub 3 to D sub 8) which are interleaved with tungsten absorbers. From 1978 to 1983 (radial range approximately 2 to a pproximately 12 AU) electrons of Jovian origin were clearly observable for electrons stopping in D(sub 3(E approximately greater than 4 MeV)) and in D(sub 4 (E approximately greater than 8 MeV)). For electrons stopping in D(sub 5(E approximately greather than 12 MeV)), the jovian flux dominated the galactic electron flux for a period of approximately one year near the encounter with Jupiter. Jovian electrons were also observed in D(sub 6(E approximately greater than 21 MeV)) but not in D(sub 7(E approximately greater than 28 MeV)). A detailed interpretation of the electron variations in all energy channels depends on an accurate subtraction of background induced by energetic protons of a few 100 MeV. This substraction is facilitated by laboratory calibration results at several energies. Further results on the differential energy spectrum of Jovian electrons and limits on the maximum detected energies will be reported