Peramalan Pasang Surut Di Perairan Ujungnegoro Kabupaten Batang Jawa Tengah

Pantai Ujungnegoro memiliki luas kawasan 6.800 Ha.Sebagian besar penduduk di pesisir pantai ujungnegoro yang sebagian besar bermata pencaharian sebagai nelayan. Sebagai wilayah yang terpencil yang dikelilingi oleh laut, dan memiliki potensi wisata bahari yang sangat besar, wilayah ini tidak lepas dari pengaruh parameter oseanografi yaitu pasang surut. Pasang surut merupakan suatu fenomena pergerakan naik turunnya permukaan air laut secara berkala yang diakibatkan oleh kombinasi gaya gravitasi dan gaya tarik benda-benda astronomi terutama oleh bumi, bulan dan matahari. Tujuan dilakukannya penelitian ini adalah untuk meramalkan pasang surut di perairan pantai ujungnegoro karena pasang surut pada tiap perairan berbeda- beda.Analisis harmonik pasang surut menggunakan metode Admiralty. Tujuan perhitungan metode admiralty adalah untuk mendapatkan konstanta harmonik pasang surut yang meliputi Amplitudo, M2, S2, K1, O1, N2, K2, P1, M4, MS4. Hasil dari metode Admiralty diperoleh nilai Formzahl sebesar 1,57 cm maka pasang surut perairan Pantai Ujungnegoro adalah bertipe pasang surut harian tunggal dengan MSL = 64,3 cm, LLWL = 49 cm, dan HHWL = 80 cm.Peramalan Pasang Surut menggunakan software MIKE 21 yang memiliki nilai MRE sebesar 10,761

Jupiter is alive! HST observations of Jupiter's aurora during Juno orbits 18, 19 and 20. (Invited)

The terawatts of ever-changing ultraviolet auroral emissions that are always observed with HST at both poles of Jupiter demonstrate that Jupiter's planetary system is “alive.” The characteristics of the different components of Jupiter's UV aurora provide information on the evolution of the overall state of the portion of the Jovian magnetosphere to which they connect. During the present medium-size HST campaign (HST GO-15638, cycle 26), precession of the line of apsides of Juno's orbit makes it possible to probe different regions of the magnetosphere, compared to Juno orbits during previous HST cycles. Solar wind dynamics and internal processes are known to have strong influence on Jupiter's aurora, but their relative contributions and the way they couple with each other are still under debate. Cycle 26 falls during the expected minimum of the 11-year solar activity cycle. Current measurements suggest that the solar activity is already exceptionally low, with very few solar events, like CMEs, reaching Jupiter. This provides an unprecedented opportunity to observe Jupiter's aurora during a period when its magnetosphere is mainly controlled by internal processes, therefore revealing Jupiter's natural "breathing." The present HST campaign is meant to observe Jupiter's bright FUV auroral emissions in time-tag imaging mode during Juno orbits 18 to 22 (Feb-Sep 2019). We focus on the 5-day periods prior to and during Junos perijove, when Juno is sampling the current sheet region within 60 RJ, which is expected to contain the plasma source responsible for most bright auroral components, but is in a location where these aurorae cannot be observed with Juno-UVS. We sample Jupiter's emissions at a frequency of ~1 HST visit per Jovian rotation, with typically 10 HST visits for each of the 5 Juno orbits. Here we present preliminary results inferred from HST observations and concurrent Juno in situ data, obtained during Juno orbits 18, 19 and 20

Jupiter is alive! HST observations of Jupiter's aurora during Juno orbits 18, 19 and 20.

The terawatts of ever-changing ultraviolet auroral emissions that are always observed with HST at both poles of Jupiter demonstrate that Jupiter's planetary system is “alive.” The characteristics of the different components of Jupiter's UV aurora provide information on the evolution of the overall state of the portion of the Jovian magnetosphere to which they connect. During the present medium-size HST campaign (HST GO-15638, cycle 26), precession of the line of apsides of Juno's orbit makes it possible to probe different regions of the magnetosphere, compared to Juno orbits during previous HST cycles. Solar wind dynamics and internal processes are known to have strong influence on Jupiter's aurora, but their relative contributions and the way they couple with each other are still under debate. Cycle 26 falls during the expected minimum of the 11-year solar activity cycle. Current measurements suggest that the solar activity is already exceptionally low, with very few solar events, like CMEs, reaching Jupiter. This provides an unprecedented opportunity to observe Jupiter's aurora during a period when its magnetosphere is mainly controlled by internal processes, therefore revealing Jupiter's natural "breathing." The present HST campaign is meant to observe Jupiter's bright FUV auroral emissions in time-tag imaging mode during Juno orbits 18 to 22 (Feb-Sep 2019). We focus on the 5-day periods prior to and during Junos perijove, when Juno is sampling the current sheet region within 60 RJ, which is expected to contain the plasma source responsible for most bright auroral components, but is in a location where these aurorae cannot be observed with Juno-UVS. We sample Jupiter's emissions at a frequency of ~1 HST visit per Jovian rotation, with typically 10 HST visits for each of the 5 Juno orbits. Here we present preliminary results inferred from HST observations and concurrent Juno in situ data, obtained during Juno orbits 18, 19 and 20

Juno, Hubble and James Webb observing Jupiter’s aurora

Hubble Space Telescope (HST) observations of Jupiter’s aurora, supporting the Juno mission, started on 30 Nov 2016. So far, they successfully covered orbits PJ03 to PJ06. After PJ07 in July 2017, the HST campaign will be interrupted by a solar avoidance period, preventing any observations from late August to the end of December 2017 (PJ08 to PJ10). The campaign will resume with PJ11 and continue until the end of HST cycle 25 (PJ15). Here, we present a brief summary of the HST data that has been acquired so far. It shows a broad range of auroral morphologies, suggesting that the Juno mission is sampling di ff erent facets of Jupiter’s magnetospheric activity. One should keep in mind that HST will not last forever. We should be ready to switch to the James Webb Telescope and take advantage of the overlap between the HST and JWST missions to prepare a smooth transition. The numerous infrared observations of Jupiter’s aurora obtained from ground based telescopes during Juno and obviously with Juno-JIRAM demonstrate that we can expect much from the tremendous performances of the JWST NIRCam and NIRSpec instruments

HST observations of Jupiter's UV aurora during Juno's orbits PJ03, PJ04 and PJ05

The intense ultraviolet auroral emissions of Jupiter are currently being monitored in the frame of a large Hubble Space Telescope (HST) program meant to support the NASA Juno prime mission. The present study addresses the three first Juno orbits (PJ03, 04 and 05) during which HST obtained parallel observations. These three campaigns basically consist of a 2-week period bracketing the time of Juno’s closest approach of Jupiter (CA). At least one HST visit is scheduled every day during the week before and the week following CA. During the ∼12-hour period centered on CA and depending on observing constraints, several HST visits are programmed in order to obtain as many simultaneous observations with Juno-UVS as possible. In addition, at least one HST visit is obtained near Juno’s apojove, when UVS is continuously monitoring Jupiter’s global auroral power, without spatial resolution, for about 12 hours. We are using the Space Telescope Imaging Spectrograph (STIS) in time-tag mode in order to provide spatially resolved movies of Jupiter’s highly dynamic aurora with timescales ranging from seconds to several days. We discuss the preliminary exploitation of the HST data and present these results in such a way as to provide a global magnetospheric context for the different Juno instruments studying Jupiter’s magnetosphere, as well as for the numerous ground based and space based observatories participating to the Juno mission

The auroral footprint of Enceladus on Saturn

Although there are substantial differences between the magnetospheres of Jupiter and Saturn, it has been suggested that cryovolcanic activity at Enceladus(1-9) could lead to electrodynamic coupling between Enceladus and Saturn like that which links Jupiter with Io, Europa and Ganymede. Powerful field-aligned electron beams associated with the Io-Jupiter coupling, for example, create an auroral footprint in Jupiter's ionosphere(10,11). Auroral ultraviolet emission associated with Enceladus-Saturn coupling is anticipated to be just a few tenths of a kilorayleigh (ref. 12), about an order of magnitude dimmer than Io's footprint and below the observable threshold, consistent with its non-detection(13). Here we report the detection of magnetic-field-aligned ion and electron beams (offset several moon radii downstream from Enceladus) with sufficient power to stimulate detectable aurora, and the subsequent discovery of Enceladus-associated aurora in a few per cent of the scans of the moon's footprint. The footprint varies in emission magnitude more than can plausibly be explained by changes in magnetospheric parameters-and as such is probably indicative of variable plume activity

Progranulin-associated primary progressive aphasia: A distinct phenotype?

The neuropsychological features of the primary progressive aphasia (PPA) syndromes continue to be defined. Here we describe a detailed neuropsychological case study of a patient with a mutation in the progranulin (GRN) gene who presented with progressive word-finding difficulty. Key neuropsychological features in this case included gravely impoverished propositional speech with anomia and prolonged word-finding pauses, impaired speech repetition most marked for sentences, and severely impaired verbal (with preserved spatial) short-term memory. There was a dissociated profile of performance on semantic processing tasks: visual semantic processing was intact, while within the verbal domain, verb comprehension was impaired and processing of nouns was intact on tasks requiring direct semantic processing but impaired on tasks requiring associative or inferential processing. Brain MRI showed asymmetric left cerebral atrophy particularly affecting the temporo-parietal junction, supero-lateral temporal and inferior frontal lobes. This case most closely resembles the PPA syndrome known as the logopenic/phonological aphasia variant (LPA) however there were also deficits of grammar and speech repetition suggesting an overlap with the progressive non-fluent aphasia (agrammatic) variant (PNFA). Certain prominent features of this case (in particular, the profile of semantic impairment) have not been emphasised in previous descriptions of LPA or PNFA, suggesting that GRN may cause an overlapping PPA syndrome but with a distinctive cognitive profile. This neuropsychological evidence suggests that GRN-PPA may result from damage involving the temporo-parietal junction and its functional connections in both the dorsal and ventral language networks, with implications for our understanding of language network pathophysiology