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Sediqi Mohammad Naser Hendrawan Vempi Satriya Adi Komori Daisuke 《Theoretical and Applied Climatology》2022,149(1-2):511-524
Theoretical and Applied Climatology - The global climate models (GCMs) of Coupled Model Intercomparison Project phase 6 (CMIP6) were used for spatiotemporal projections of precipitation and... 相似文献
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Adi Nusser 《Monthly notices of the Royal Astronomical Society》2001,325(4):1397-1401
We derive the asymptotic mass profile near the collapse centre of an initial spherical density perturbation, δ ∝ M − ε , of collisionless particles with non-radial motions. We show that angular momenta introduced at the initial time do not affect the mass profile. Alternatively, we consider a scheme in which a particle moves on a radial orbit until it reaches its turnaround radius, r ∗. At turnaround the particle acquires an angular momentum L =ℒ√ GM * r * per unit mass, where M ∗ is the mass interior to r ∗. In this scheme, the mass profile is M ∝ r 3/(1+3 ε ) for all ε >0 , in the region r / r t ≪ℒ , where r t is the current turnaround radius. If ℒ≪1 then the profile in the region ℒ≪ r / r t ≪1 is M ∝ r for ε <2/3 , and remains M ∝ r 3/(1+3 ε ) for ε ≥2/3 . The derivation relies on a general property of non-radial orbits which is that the ratio of the pericentre to apocentre is constant in a force field k ( t ) r n with k ( t ) varying adiabatically. 相似文献
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Adi Nusser 《New Astronomy》2009,14(4):365-368
The time scale for cooling of the gravitationally bound gaseous intracluster medium (ICM) is not determined by radiative processes alone. If the ICM is in quasi-hydrostatic equilibrium in the fixed gravitational field of the dark matter halo then energy losses incurred by the gravitational potential energy of the gas should also be taken into account. This “gravitational heating” has been known for a while using explicit solutions to the equations of motion. Here, we re-visit this effect by applying the virial theorem to gas in quasi-hydrostatic equilibrium in an external gravitational field, neglecting the gravity of the gas. For a standard NFW form of halo profiles and for a finite gas density, the response of the gas temperature to changes in the total energy is significantly delayed. The effective cooling time could be prolonged by more than an order of magnitude inside the scale radius of the halo. Gas lying at a distance twice the scale radius, has negative heat capacity so that the temperature increases as a result of energy losses. Although external heating (e.g. by AGN activity) is still required to explain the lack of cool ICM near the center, the analysis here may circumvent the need for heating in farther out regions where the effective cooling time could be prolonged to become larger than the cluster age and also explains the increase of temperature with radius in these regions. 相似文献
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Enzo Branchini Amiram Eldar Adi Nusser 《Monthly notices of the Royal Astronomical Society》2002,335(1):53-72
We present extensive tests of the fast action method (FAM) for recovering the past orbits of mass tracers in an expanding universe from their redshift-space coordinates at the present epoch. The tests focus on the reconstruction of present-day peculiar velocities using mock catalogues extracted from high-resolution N -body simulations. The method allows for a self-consistent treatment of redshift-space distortions by direct minimization of a modified action for a cosmological gravitating system. When applied to ideal, volume-limited catalogues, FAM recovers unbiased peculiar velocities with a one-dimensional, 1σ error of ∼220 km s−1 , if velocities are smoothed on a scale of 5 h −1 Mpc. Alternatively, when no smoothing is applied, FAM predicts nearly unbiased velocities for objects residing outside the highest density regions. In this second case the 1σ error decreases to a level of ∼150 km s−1 . The correlation properties of the peculiar velocity fields are also correctly recovered on scales larger than 5 h −1 Mpc. Similar results are obtained when FAM is applied to flux-limited catalogues mimicking the IRAS PSC z survey. In this case FAM reconstructs peculiar velocities with similar intrinsic random errors, while velocity–velocity correlation properties are well reproduced beyond scales of ∼8 h −1 Mpc. We also show that FAM provides better velocity predictions than other, competing methods based on linear theory or the Zel'dovich approximation. These results indicate that FAM can be successfully applied to presently available galaxy redshift surveys such as IRAS PSC z . 相似文献
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Atmospheric Ne, Ar, Kr and Xe are observed in fluids occurring in deep basins. Modifications of their abundance patterns reveal modes of recharge and brine formation, phase separations during boiling, and association of natural gas with water or oil. Radiogenic 4He and 40Ar serve as age indicators of entrapped fluids, effective over a significant portion of the geological time scale. Simultaneous application of δ13C, atmospheric noble gases and radiogenic 4He and 40Ar, is recommended to identify: (a) recent bacterial natural gas formation, not accompanied by oil, and (b) natural gas formed along with oil in a mature source rock. 相似文献
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Guruh Samodra Danang Sri Hadmoko Ghalih Nur Wicaksono Indriya Parahita Adi Maulana Yudinugroho Sandy Budi Wibowo Hatma Suryatmojo Taufik Hery Purwanto Barandi Sapta Widartono Franck Lavigne 《Landslides》2018,15(5):985-993
The Clapar landslide induced debris flow consisted of the Clapar landslide occurred on 24 March 2017 and the Clapar debris flow occurred on 29 March 2017. The first investigation of the Clapar landslide induced debris flow was carried out two months after the disaster. It was followed by UAV mapping, extensive interviews, newspaper compilation, visual observation and field measurements, and video analysis in order to understand chronology and triggering mechanism of the landslide induced debris flow in Clapar. The 24 March 2016 landslide occurred after 5 hours of consecutive rainfall (11,2 mm) and was affected by combination of fishponds leak and infiltration of antecedent rain. After five days of the Clapar landslide, landslide partially mobilized to form debris flow where the head scarp of debris flow was located at the foot of the 24 March 2016 landslide. The Clapar debris flow occurred when there was no rainfall. It was not generated by rainstorm or the surface erosion of the river bed, but rather by water infiltration through the crack formed on the toe of the 24 March 2016 landslide. Supply of water to the marine clay deposit might have increased pore water pressure and mobilized the soil layer above. The amount of water accumulated in the temporary pond at the main body of the 24 March 2016 landslide might have also triggered the Clapar debris flow. The area of Clapar landslide still shows the possibility of further retrogression of the landslide body which may induce another debris flow. Understanding precursory factors triggering landslides and debris flows in Banjarnegara based on data from monitoring systems and laboratory experiments is essential to minimize the risk of future landslide. 相似文献
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The real-space optical-depth distribution along the line of sight to the QSO Q1422+231 is recovered from two HIRES spectra using a modified version of the inversion method proposed by Nusser & Haehnelt. The first two moments of the truncated optical-depth distribution are used to constrain the density-fluctuation amplitude of the intergalactic medium (IGM) assuming that the IGM is photoionized by a metagalactic UV background and obeys a temperaturedensity relation. The fluctuation amplitude and the power-law index of the relation between gas and neutral hydrogen (H i ) density are degenerate. The rms of the IGM density at z 3.25 estimated from the first spectrum is with 1.56< <2 for plausible reionization histories. This corresponds to 0.9 2.1 with ( =1.7)=1.44±0.3. The values obtained from the second spectrum are higher by 20 per cent. If the IGM density traces the dark matter (DM) as suggested by numerical simulations we have measured the fluctuation amplitude of the DM density at an effective Jeans scale of a few 100 kpc. For cold dark matter (CDM)-like power spectra the amplitude of dark matter fluctuations on these small scales depends on the cosmological density parameter . For power spectra normalized to reproduce the space density of present-day clusters and with a slope parameter of =0.21 consistent with the observed galaxy power spectrum, the inferred can be expressed as: =0.61( /1.7)1.3 ( x J /0.62)0.6 for a flat universe, and =0.91( /1.7)1.3 ( x J /0.62)0.7 for a =0 universe. x J is the effective Jeans scale in (comoving) h 1 Mpc. Based on a suite of detailed mock spectra the 1 error is 25 per cent. The estimates increase with increasing . For the second spectrum we obtain 15 per cent lower values. 相似文献
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太平洋-印度洋贯穿流南海分支在卡里马塔海峡的十年观测回顾 总被引：5，自引：2，他引：3
Wei Zexun Li Shujiang Susanto R. Dwi Wang Yonggang Fan Bin Xu Tengfei Sulistiyo Budi Adi T. Rameyo Setiawan Agus Kuswardani A. Fang Guohong 《海洋学报(英文版)》2019,38(4):1-11
除印度尼西亚贯穿流之外，南海贯穿流也是太平洋向印度洋输送海水的重要分支。尽管基于数值模拟等方法的研究早已指出，南海分支在太平洋-印度洋洋际交换中有重要作用，但是直到2007年之前，南海分支在卡里马塔海峡处的观测几乎是空白。本文回顾了自2007年起，通过中印尼合作项目"南海-印度尼西亚海水交换及对鱼类季节性洄游的影响（SITE）"在卡里马塔海峡开展的近十年观测，以及在此基础上进一步开展的"印度尼西亚贯穿流海域水交换、内波和混合观测及其生态效应（TIMIT）"观测项目，并对SITE和TIMIT观测取得的成果进行了总结。 相似文献