Papers by Valery Shuvalov
Mining
Here, we present a numerical model for simulating the formation and evolution of the gas and dust... more Here, we present a numerical model for simulating the formation and evolution of the gas and dust cloud that forms after the detonation of high explosive charges in boreholes. This model provides a possible method for converting a substance ejected from an explosion funnel into discrete particles (smaller particles and stones) and calculating the movement of these condensed particles and their interaction with the air–gas flow; this method uses the framework of equations for multiphase media motion. For modeling of borehole explosion, we focused on the parameters of commercial blasting that are carried out at the Lebedinsky open pit. The results of simulating the initial stage of a borehole explosion with a mass of 1000 kg are presented in this paper. These results demonstrate the evolution of a gas and dust cloud, the change in the mass of particles of different sizes in the air over time, and their spatial distribution.
Numerical Simulation of Asteroid Deceleration in the Venus Atmosphere
Dynamic Processes in Geospheres
Ejecta Formation and Deposition After the Mjølnir Impact
Lunar and Planetary Science Conference, Mar 1, 2003
Ejecta Distribution from Small Impacts
A field study of the Chelyabinsk airburst impact
AGU Fall Meeting Abstracts, Dec 1, 2013
Chelyabinsk meteoroid entry: analysis of acoustic signals in the area of direct sound propagation
40th COSPAR Scientific Assembly, 2014
Numerical Modeling of the Mjølnir Marine Impact Event
Lunar and Planetary Science Conference, Mar 1, 2002
Numerical estimates of seismic effects after collisions of small bodies with the Earth atmosphere
40th COSPAR Scientific Assembly, 2014
The Chelyabinsk airburst shockwave
Asteroids, Comets, Meteors 2014, Jul 1, 2014
Estimates of abundance of vapor condensate from the impacts of asteroids and comets on the Moon
40th COSPAR Scientific Assembly, 2014
Icarus, 1997
INTRODUCTION Radiation energies of bright flashes caused by disintegration A relatively small num... more INTRODUCTION Radiation energies of bright flashes caused by disintegration A relatively small number of satellites in high-altitude of large meteoroids in the atmosphere have been measured orbits (20,000 km and higher) provide coverage of most using optical sensors on board geostationary satellites. Light curves versus time are available for some of the events. We of the Earth's surface. It is possible to have essentially have worked out several numerical techniques to derive the continuous, 24-h, all weather coverage over the entire surkinetic energy of the meteoroids that produced the flashes. face of the Earth. Space-based infrared sensors detect Spectral opacities of vapor of various types of meteoroids bright flashes (the average number of flashes is about 30 were calculated for a wide range of possible temperatures per year). In addition, optical sensors detect light curves and densities. Coefficients of conversion of kinetic energy in the visible portion of the spectrum. The bright flashes to radiation energy were computed for chondritic and are caused by explosive disintegration of large meteoroids iron meteoroids 10 cm to 10 m in size using radiationin the atmosphere (Reynolds 1992, Tagliaferri 1993, 1996, hydrodynamics numerical simulations. Luminous efficiency increases with body size and initial velocity. Some analytical Tagliaferri et al. 1994, McCord et al. 1995). approximations are presented for average conversion coeffi-Information that can be derived from observations by cients for irons and H-chondrites. A mean value of this the Satellite Network (SN) is of great interest to planetary coefficient for large meteoroids (1-10 m in size) is about science. Energy-frequency distribution of SN bolides may 5-10%. The theory was tested by analyzing the light curves provide the opportunity to predict probability of impacts, of several events in detail. give a more accurate account of the population of the near-Kinetic energies of impactors and energy-frequency distribu-Earth objects, and anticipate the hazard from large imtion of 51 bolides, detected during 22 months of systematic pacts. observations in 1994-1996, are determined using theoretical Retrieval of meteoroid attributes (energy, velocity, values of luminous efficiencies and heat-transfer coefficients. The number of impacts in the energy range from 0.25 to 4 kt mass, density) from the light power curves is a challenging TNT is 25 per year and per total surface of the Earth. task. The simplest method to assess the meteoroid kinetic The energy-frequency distribution is in a rather good energy is to divide the released radiation energy by a lumiagreement with that derived from acoustic observations and nous efficiency (efficiency for conversion of kinetic energy the lunar crater record. Acoustic systems have registered one to radiation energy). The use of empirical values of lumi-1 Mt event in 12 years of observation. Optical systems have nous efficiency for small meteoroids (Bronsten 1983) and not detected such an event as yet due to a shorter time of artificial meteors (Ayers et al. 1970, Givens and Page 1971) observation. The probability of a 1 Mt impact was estimated is inappropriate for assessment of large SN meteoroids.
Meteoritics & Planetary Science, 2018
The results of numerical modeling of meteoroids' interaction with Earth's atmosphere are presente... more The results of numerical modeling of meteoroids' interaction with Earth's atmosphere are presented. We model the entry in two dimensions and then interpolate the results into a 3-D model to calculate interaction of shock waves with the surface. Maximum shock pressures, wind speeds, and areas subjected to substantial overpressure are calculated for oblique impacts of asteroids and comets. We show that vertical impacts produce a smaller damage zone on the surface than oblique ones. Damage caused by shock waves covers an order of magnitude larger area than any other hazardous effects. The function of energy release in the atmosphere, which is traditionally used in meteoritics, has a limited application if cosmic bodies are larger than tens of meters in diameter: at each time moment energy is smoothed along a substantial length of the trajectory; both emitted radiation (routinely used for calibration of semi-analytical models) and shock wave amplitude are complex functions of temperature-density distributions in atmosphere.
Numerical modeling of Tunguska-like impacts
Planetary and Space Science, 2002
A two-dimensional numerical model with radiation and ablation is developed for the study of the i... more A two-dimensional numerical model with radiation and ablation is developed for the study of the impact of rather large (several meters or several tens of meters) meteoroids. This model is applied to consider the vertical impact of a 30m in radius cometary projectile. Numerical simulations clearly demonstrate the two main stages in the meteoroid's evolution. During the first stage the
Numerical Simulations of Explosive Type Generator
APS, Jun 1, 1999
Explosive-type generator (ETG) was elaborated by Yu. Kiselev (IDG RAS) for generation of high vel... more Explosive-type generator (ETG) was elaborated by Yu. Kiselev (IDG RAS) for generation of high velocity gaseous jets. It differs from previous versions of similar devices (being developed by Voytenko) by very high efficiency (about 5-10% at maximum jet velocity of around 40 km/s). The operation of the instrument is based on porous matter compression under action of cylindrical detonation wave.
Chelyabinsk airburst shockwave characteristics from Korkino coal mine seismic records
Impact Hazard of Large Meteoroids and Small Asteroids
Meteoroids, 2019
Dust Ejection Induced by Small Meteoroids Impacting Martian Surface
The objective of this study is numerical modeling of meteoroid impact on the martian surface and ... more The objective of this study is numerical modeling of meteoroid impact on the martian surface and determination of the resulting dust cloud parameters. Additional information is contained in the original extended abstract.
Most cosmic bodies impacting the Earth fall into seas and oceans, which cover more than two-third... more Most cosmic bodies impacting the Earth fall into seas and oceans, which cover more than two-thirds of the Earth’s surface. However, among more than 150 craters discovered on the Earth, only 15–20 found recently were formed as a result of marine target impacts (Ormö and Lindström 2000). The deficit of underwater craters is explained by the relative youth of a typical ocean floor (<150–180 Ma), insufficient exploration of the sea/ocean floor, and specific features of the underwater cratering process. Most of the known underwater craters were formed in shallow seas, where the water depth is comparable with an impactor size. Eltanin (Gersonde et al. 1997) is the only presently known impact structure formed due to impact into a deep (∼4 km) ocean. The process of cratering of marine target impacts has been poorly investigated; however, relations obtained for continental craters are commonly used to estimate the parameters of underwater craters. A small number of numerical simulations w...
Scaling Relations for Radiation Effects Due to Impacts of Large Cosmic Objects
Asteroids risk models require understanding how an asteroid (or a comet) entering into the atmosp... more Asteroids risk models require understanding how an asteroid (or a comet) entering into the atmosphere can harm people and infrastructure. Radiation produced due to the flight of a cosmic object in the atmosphere and due to an emission of a plume is one of the main dangerous consequences of a crater-forming impact. This thermal radiation can be strong enough to be dangerous to people, to ignite fires and even to melt rocks. The effects of the radiation may be estimated based on the data on nuclear explosions or based on the especially elaborated model. Numerical simulation of the impacts of large cosmic objects provides a basis for construction of scaling relations, which allow estimating easily the thermal exposure distribution on the surface and some other important parameters. These scaling relations are useful tool for rapid assessments of hazardous effects of thermal radiation. All scaling relations described in this article are implemented in the developed web-based Calculator ...
Trigger Effect of an Asteroidal or Cometary Impact at the Permian–Triassic Boundary
The Araguainha impact crater in Brazil with a diameter of 40 km could be formed by the impact of ... more The Araguainha impact crater in Brazil with a diameter of 40 km could be formed by the impact of an asteroid or a comet with a diameter of about 3 km. We conducted numerical simulations of the impacts of such objects with velocities 20 km/s (asteroid) and 50 km/s (comet) and calculated thermal fluxes on the surface of the Earth produced by direct thermal radiation from impact plumes. Estimates of the conditions of ignition of dry materials show that highly inflammable materials, such as dry grass and leaves, can catch fire in an area of 4000–4500 km in size. The impact also causes an earthquake of magnitude 9–10, which, according to some suggestions, could lead to release of methane from organic-rich sediments, including oil shale. The age of the Araguainha crater, within the limits of errors of its determination, is close to the time of the great mass extinction at the Permian–Triassic boundary, when the land was united into one supercontinent Pangea. Climatic conditions and the le...
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Papers by Valery Shuvalov