Search academic texts

Information × Registration Number 0216U001525, 0115U002865 , R & D reports Title Application of the GRID-technology to the astrophysical computing intensive tasks and upgrade/development of the GRID cluster of MAO NANU popup.stage_title Head Berczik P.P., Registration Date 18-02-2016 Organization Main Astronomical Observatory popup.description2 The main objective of the project - is to study the dynamical evolution of the galactic center and the central black hole accretion disk with the gas and with the highest possible resolution large. Compared to our previous work for the year 2012 in this area (Just et al, 2012, ApJ, 758, 51), this year we planned to calculate an extended series of models with a relatively small number of particles, but with a wide range of parameters (holding several dozen calculations with different parameters of the masses of black holes and accretion disk). The main focus of the simulation in this task - the study of the dynamic interaction of the central star cluster with a supermassive black hole (Super Massive Black Hole - SMBH), which is surrounded by a massive accretion disk (Accretion Disks - AD). Moving star surrounded SMBH (particularly in the AD) we have a (along with forces from SMBH and other stars) dissipative force which (in our opinion, set out in Just et al, 2012, ApJ, 758, 51) can significantly enhance accretion rate on SMBH. For the integration of the motion of individual stars in the system, the direct N-body code with precision integrator fourfold phi-GRAPE / GPU proprietary (Harfst et al, NewA, 12, 357), which has already undergone a detailed testing of dozens of articles in the past few years. The code was designed as a parallel MPI code from the possibility of using all methods of hardware (GRAPE, GPU, FPGA, CPU-SSE2, CPU-AVX, Xeon Phi) to calculate the gravitational interaction between particles. A further object also been numerically simulated changes in the chemical composition gradient (oxygen and nitrogen) in the massive disk galaxies (in red shifts in the z = 1) as a result of the interaction and fusion of data objects with dwarf galaxies local volume (50 PDA), a comparison changes in chemical composition gradient in the outer parts of the disk galaxies (from 10 - 20 kpc) with observational gradients according to the given SDSS. Panoramic spectral overview CALIFA (Calar Alto Legacy Integral Field Area) allows you to get up to 5625 spectra for one galaxy (Sanchez et al. 2012). Currently available data for 200 galaxies further increase their number to 600. In order to determine the physical characteristics of interstellar space galaxies must find in each spectrum, the intensity measured, the width and position of the emission lines of hydrogen, oxygen, nitrogen, sulfur, et al., And usually requires at least several cell lines in different stages of ionization. To solve this problem, we have developed a software package for locating, measuring the parameters of the emission lines and error estimates derived parameters. Data processing for a galaxy with a rough estimate of the error lasts, as a rule, tens of hours, and a reliable estimate of the error parameters require even much more time. Thus, this task requires the amount of computer resources, greatly exceeds the resources of a separate PC and even small clusters consisting of multiple nodes. Despite the high degree of concurrency problem (process independently of the other, you can not just data for each galaxy and thousands of spectra of each galaxy), we plan to adapt the software and to develop a grid-based interface to perform our tasks in the grid environment, which will dramatically increase the speed calculations. Product Description popup.authors Берцик Петер Петерович Велесь Олександр Анатолійович Зінченко І.А. Кравченко Д.В. popup.nrat_date 2020-04-02 Close