115 research outputs found
Poligami dalam Hukum Islam dan Hukum Positif Indonesia Serta Urgensi Pemberian Izin Poligam di Pengadilan Agama
Penulisan artikel ini bertujuan untuk mengetahui dasar hukum berpoligami dalam hukum islam maupun hukum positif di Indonesia serta mengetahui bagaimana urgensi pemberian izin berpoligami di Pengadilan Agama. Dalam tulisan ini menggunakan pendekatan yuridis normatif dengan berbagai teori interpretasi. Pengadilan Agama merupakan lembaga peradilan dibawah Mahkamah Agung yang sangat penting dalam menangani permasalahan mengenai sengketa yang berhubungan dengan agama Islam. Mulai dari perkawinan, kewarisan, wasiat, hibah, wakaf, zakat, infak, sedekah, sampai ekonomi syariah menjadi tugas dan wewenang dari Pengadilan Agama yang sesuai dengan Pasal 49 dan 50 UU No.7 Tahun 1989 tentang Pengadilan Agama yang telah diamandemen dengan UU No.3 Tahun 2006. Dalam Pasal 4 ayat (1) UU No. 1 Tahun 1974 tentang Perkawinan, apabila seorang suami ingin beristri lebih dari seorang maka wajib mengajukan permohonan kepada Pengadilan di daerah tempat tinggalnya (yaitu Pengadilan Agama). Diatur pula dalam pasal-pasal berikutnya dalam pengajuan poligami harus memenuhi syarat-syarat yang sudah ditentukan menurut UU Perkawinan. Pengaturan tentang poligami di hukum positif seakan mempersulit suami untuk poligami, sedangkan hukum islam sendiri tidak terlalu mempersulit seorang suami untuk poligami. Oleh karena itu kedua hukum ini harus saling sinkron agar tidak menimbulkan suatu permasalahan dalam perkawinan khususnya poligami
Characterizing the gamma-ray long-term variability of PKS 2155-304 with H.E.S.S. and Fermi-LAT
Studying the temporal variability of BL Lac objects at the highest energies
provides unique insights into the extreme physical processes occurring in
relativistic jets and in the vicinity of super-massive black holes. To this
end, the long-term variability of the BL Lac object PKS 2155-304 is analyzed in
the high (HE, 100 MeV 200 GeV)
gamma-ray domain. Over the course of ~9 yr of H.E.S.S observations the VHE
light curve in the quiescent state is consistent with a log-normal behavior.
The VHE variability in this state is well described by flicker noise
(power-spectral-density index {\ss}_VHE = 1.10 +0.10 -0.13) on time scales
larger than one day. An analysis of 5.5 yr of HE Fermi LAT data gives
consistent results ({\ss}_HE = 1.20 +0.21 -0.23, on time scales larger than 10
days) compatible with the VHE findings. The HE and VHE power spectral densities
show a scale invariance across the probed time ranges. A direct linear
correlation between the VHE and HE fluxes could neither be excluded nor firmly
established. These long-term-variability properties are discussed and compared
to the red noise behavior ({\ss} ~ 2) seen on shorter time scales during
VHE-flaring states. The difference in power spectral noise behavior at VHE
energies during quiescent and flaring states provides evidence that these
states are influenced by different physical processes, while the compatibility
of the HE and VHE long-term results is suggestive of a common physical link as
it might be introduced by an underlying jet-disk connection.Comment: 11 pages, 16 figure
Detection of variable VHE gamma-ray emission from the extra-galactic gamma-ray binary LMC P3
Context. Recently, the high-energy (HE, 0.1-100 GeV) -ray emission
from the object LMC P3 in the Large Magellanic Cloud (LMC) has been discovered
to be modulated with a 10.3-day period, making it the first extra-galactic
-ray binary.
Aims. This work aims at the detection of very-high-energy (VHE, >100 GeV)
-ray emission and the search for modulation of the VHE signal with the
orbital period of the binary system.
Methods. LMC P3 has been observed with the High Energy Stereoscopic System
(H.E.S.S.); the acceptance-corrected exposure time is 100 h. The data set has
been folded with the known orbital period of the system in order to test for
variability of the emission. Energy spectra are obtained for the orbit-averaged
data set, and for the orbital phase bin around the VHE maximum.
Results. VHE -ray emission is detected with a statistical
significance of 6.4 . The data clearly show variability which is
phase-locked to the orbital period of the system. Periodicity cannot be deduced
from the H.E.S.S. data set alone. The orbit-averaged luminosity in the
TeV energy range is erg/s. A luminosity of erg/s is reached during 20% of the orbit. HE and VHE
-ray emissions are anti-correlated. LMC P3 is the most luminous
-ray binary known so far.Comment: 5 pages, 3 figures, 1 table, accepted for publication in A&
Multi-messenger observations of a binary neutron star merger
On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta
VizieR Online Data Catalog: RX J1713.7-3946 HESS spectrum (HESS+, 2018)
FITS files with the very high-energy gamma-ray images, Fig.1, and the spectrum, Fig.3, as ascii text file. (3 data files)
VizieR Online Data Catalog: W49B with H.E.S.S. and Fermi-LAT (HESS+, 2018)
File hessmap.fit contains the gamma-ray excess map obtained with H.E.S.S. in the direction of the supernova remnant W49B
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