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Rachel S. Somerville Gerard Lemson Tsafrir S. Kolatt Avishai Dekel 《Monthly notices of the Royal Astronomical Society》2000,316(3):479-490
We study the merging history of dark matter haloes in N -body simulations and semi-analytical 'merger trees' based on the extended Press–Schechter (EPS) formalism. The main focus of our study is the joint distribution of progenitor number and mass as a function of redshift and parent halo mass. We begin by investigating the mean quantities predicted directly by the Press–Schechter (PS) and EPS formalism, such as the halo mass and conditional mass functions, and compare these predictions with the results of the simulations. The higher moments of this distribution are not predicted by the EPS formalism alone and must be obtained from the merger trees. We find that the Press–Schechter model deviates from the simulations at the level of 30–50 per cent on certain mass scales, and that the sense of the discrepancy changes as a function of redshift. We show that this discrepancy is reflected in the higher moments of the distribution of progenitor mass and number. We investigate some related statistics such as the accretion rate and the mass ratio of the largest two progenitors. For galaxy sized haloes ( M ∼1012 M⊙ ), we find that the merging history of haloes, as represented by these statistics, is well reproduced in the merger trees compared with the simulations. The agreement deteriorates for larger mass haloes. We conclude that merger trees based on the extended Press–Schechter formalism provide a reasonably reliable framework for semi-analytical models of galaxy formation. 相似文献
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Several fundamental issues of fracture mechanics during the post-dynamic stage are yet not fully understood, including fracture arrest mechanisms, effects of the three-dimensional fracture propagation on fracture aperture and height relations, and the role played by fracture tips on fracture termination. We studied these issues in the seismically active Dead Sea basin, where clastic dikes (>10 m) and numerous smaller dikelets (<1 m) dynamically intruded the late-Pleistocene soft rock of the Lisan Formation. A three-dimensional study of the dikelets shows that they form arrest zones at the tips of the larger clastic dikes. Geometrically, the dikelets are divided into two parts: (1) the main dikelet, in which the aperture profile along the dikelet height is approximately elliptic; and (2) the elongated tip, in which the aperture profile along the tip height is approximately constant. The dikelet aspect ratio is defined as A/H, where A is dikelet aperture and H is dikelet height. A plot of A/H versus H describes power relations with two different zones: (1) Zone A, with a small variation of A/H, between 0.02 and 0.06, for dikelets in height range of 100–700 mm; and (2) Zone B, where the aspect ratio sharply increases to 0.23 in dikelets with heights less than 100 mm. We interpret that during deceleration, when the height of the elongated tip became greater than 1/10 of the dikelet height, inelastic conditions are dominant. Under these conditions, the fracture velocity decreases significantly and the dikelet aspect ratio increases. The present observations and analyses indicate that formation of elongated tips and dike (fracture) segmentation are essential for the decay of the dynamic fracturing. 相似文献
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A combined sample of 79 high- and low-redshift Type Ia supernovae (SNe) is used to set constraints on the degree of anisotropy in the Universe out to z ≃1. First, we derive the global most probable values of matter density ΩM , the cosmological constant ΩΛ and the Hubble constant H 0 , and find them to be consistent with the published results from the two data sets of Riess et al. and Perlmutter et al. We then examine the Hubble diagram (HD, i.e., the luminosity–redshift relation) in different directions on the sky by utilizing spherical harmonic expansion. In particular, via the analysis of the dipole anisotropy, we divide the sky into the two hemispheres that yield the most discrepant of the three cosmological parameters, and the scatter χ HD 2 in each case. The most discrepant values roughly move along the locus −4ΩM +3ΩΛ =1 (cf. Perlmutter et al.), but by no more than Δ≈2.5 along this line. For a perfect Friedmann–Robertson–Walker universe, Monte Carlo realizations that mimic the current set of SNe yield values higher than the measured Δ in ∼1/5 of the cases (for ΩM ). We discuss implications for the validity of the Cosmological Principle, and possible calibration problems in the SNe data sets. 相似文献
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Stav Shapira Tsafrir Levi Yaron Bar-Dayan Limor Aharonson-Daniel 《Natural Hazards》2018,91(3):1059-1074
The use of casualty modeling in the field of disaster management is well established. Nevertheless, it is currently based almost exclusively on damage to the built environment and fails to consider additional factors that may influence the number of casualties in a given event, such as behavioral features of the exposed population. The present study has taken an innovative approach and integrated behavioral traits of residents in a high-risk area in northern Israel, near the Dead Sea Transform, into a well-known casualty estimation simulation. The expected behavioral characteristics of residents during an earthquake, in city sectors with different socioeconomic rankings, were assessed using a designated survey and were applied into the casualty estimation process. In order to test the sensitivity of the behavioral factor, twelve synthetic earthquake scenarios were designed. The results shed light on the relationship between specific behavioral strategies and casualty projections and suggest that loss estimation models that do not take behavioral factors into account may overestimate the projected number of casualties. Households with low socioeconomic status were found to be more vulnerable in terms of risk of injury and death compared with those ranked higher. The present study shows the importance of raising public awareness regarding proper behavior prior to and during the event which can help increase resilience of communities, mitigate risks and losses and ultimately save lives. Further implications of these results and possible ways of improving casualty modeling and community resilience are also discussed. 相似文献
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Natural Hazards - Building damage probabilities are invaluable for assessing short-term losses from natural hazards. In many countries however, the individual building level data required for... 相似文献
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Tsafrir S. Kolatt & Matthias Bartelmann 《Monthly notices of the Royal Astronomical Society》1998,296(3):763-772
We propose a method to remove the mass-sheet degeneracy that arises when the mass of galaxy clusters is inferred from gravitational shear. The method utilizes high-redshift standard candles that undergo weak lensing. Natural candidates for such standard candles are type Ia supernovae (SNe Ia).
When corrected with the light-curve shape (LCS), the peak magnitude of SNe Ia provides a standard candle with an uncertainty in apparent magnitude of Δ m ≃0.1–0.2. Gravitational magnification of a background SN Ia by an intervening cluster would cause a mismatch between the observed SN Ia peak magnitude compared with that expected from its LCS and redshift. The average detection rate for SNe Ia with a significant mismatch of ≥2Δ m behind a cluster at z ≃0.05–0.15 is about 1–2 supernovae per cluster per year at J , I , R ≲25–26.
Since SNe are point-like sources for a limited period, they can experience significant microlensing by massive compact halo objects (MACHOs) in the intracluster medium. Microlensing events caused by MACHOs of ∼10−4 M⊙ are expected to have time-scales similar to that of the SN light curve. Both the magnification curve by a MACHO and the light curve of a SN Ia have characteristic shapes that allow us to separate them. Microlensing events caused by MACHOs of smaller mass can unambiguously be identified in the SN light curve if the latter is continuously monitored. The average number of identifiable microlensing events per nearby cluster ( z ≲0.05) per year is ∼0.02 ( f /0.01), where f is the fraction of the cluster mass in MACHOs of masses 10−7 < M macho /M⊙<10−4 . 相似文献
When corrected with the light-curve shape (LCS), the peak magnitude of SNe Ia provides a standard candle with an uncertainty in apparent magnitude of Δ m ≃0.1–0.2. Gravitational magnification of a background SN Ia by an intervening cluster would cause a mismatch between the observed SN Ia peak magnitude compared with that expected from its LCS and redshift. The average detection rate for SNe Ia with a significant mismatch of ≥2Δ m behind a cluster at z ≃0.05–0.15 is about 1–2 supernovae per cluster per year at J , I , R ≲25–26.
Since SNe are point-like sources for a limited period, they can experience significant microlensing by massive compact halo objects (MACHOs) in the intracluster medium. Microlensing events caused by MACHOs of ∼10
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