بينش امروزي ما پيرامون جهان هستي مبتني بر مدل استاندارد ذرات بنيادي مي‌باشد. مطابق اين جهان از يك مجموعه فرميون‌هاي بنيادي اسپين 12   به نام كوارك‌ها و لپتون‌ها تشكيل شده است و برهم كنش‌هاي ميان اين سنگ‌هاي اوليه طبيعت عبارتند از: برهم كنش الكترومغناطيسي، برهم كنش هسته‌اي قوي، و برهمكنش هسته‌اي ضعيف است كه از طريق مبادله بوزون‌هاي پيمانه‌اي به نام فوتون، گلئونW±   و‏Z0   صورت مي‌گيرد. اين مدل در نيمه دوم قرن بيستم در نتيجه ي تلاش مشاركت آميز دانشمندان در عرصه جهاني شكل گرفت. فرمول بندي كنوني آن در اواسط دهه ???? ميلادي پس از تاييد تجربي وجود كوارك‌ها نهايي شد.

  Abstract: Einstein's field equations predict the existence of four-dimensional black holes. The first uncharged and charged four-dimensional black hole solutions are known as Schwarzschild and Riesenordstrom black holes, respectively. The first three-dimensional black hole solution known as BTZ (Banados-Teitelboim-Zanelli) black holes was obtained in 1992 by solving the field equations in the presence of the negative cosmological constant. In the first part of this thesis, we obtained three-dimensional black hole solutions, with spherical symmetry, in Einstein's gravity, and after calculating thermodynamic quantities, we show that the first law of thermodynamics is true for these black holes. Then, using the canonical ensemble method, we check the thermodynamic stability of these black holes. In the second part, we extend the above idea to dilaton black holes (in Einstein-dilaton gravity). For this purpose, we obtain the black hole solutions of the field equations in the presence of a scalar field and considering the Lagrangian of the electromagnetic field as a material field and examine their geometric properties. Then we calculate the thermodynamic parameters of these black holes (mass, electric charge, temperature, entropy and electric potential) in appropriate ways. We show that the obtained quantities apply to the first law of thermodynamics of black holes and at the end we analyze the thermodynamic stability of dilatonic black holes using the canonical ensemble method. Keywords: 3D black holes, linear electrodynamics, Einstein-dilaton gravity, dilaton black holes, coupled gravity.

  Abstract:One of thequantities studied in the fission process is the mass distribution of thefission fragments. When fission occurs, fission fragments with different massesare created. In this thesis, the temperature dependence of the fission fragmentmass yield width for high excitation energies is investigated. The width of themass yield depends on the number of nucleons in the nuclei, the volume andsurface terms of the energy level density parameter, the temperature and thepotential stiffness parameter related to the degree of freedom of the massasymmetry. Calculations are done using the transition state fission model. Forfission of 201Tl, 207Bi, 210Po and 213Atnuclei, we will compare the results of theoretical calculations withexperimental data. Also, the contribution of the surface term of the energylevel density parameter in the width is investigated for differenttemperatures.Keywords: Fission fragment, Temperature dependence, Width of mass yield

ميلياردها سال پيش انفجاربزرگ اتفاق افتاد،وجهان ما اغاز شد.علت انفجاربزرگ ، بزرگترين رازي است كه بشرهنوز نميداند،اين نظريه يكي از مهمترين موفقيت هاي علمي قرن بيستم است امروزه نمي توان جهان را بدون درك انفجار بزرگ شناخت ولي اين نظريه به نواحي كه فيزيك آن قابل فهم وآزمايش است محدود مي شودوتوضيحي براي نحوه ي تحول عالم در زمان هاي   ابتدايي تر وداغ تر ندارد. براي شناخت كيهان شناسي نوين بايد به اوايل قرن بيستم برگرديم،زماني كه انيشتين نظريه نسبيت عام خود را در سال1915 ميلادي منتشر كرد طبق اين نظريه بيان ميكند كه هندسه ي عالم با توزيع ماده ي درون عالم ،مشخص مي شود.در سال 1922 فريدمن جواب   معادلات كيهان شناسي انيشتين را برپايه ي يك عالم همگن وهمسانگرد بدست آوردكه به متريك FRW معروف شد.اين متريك نشان ميداد كه برخلاف تصور معمول آن زمان ،عالم درحال انبساط است. هابل در سال 1929بطور تجربي انبساط عالم توسط مشاهدات را تاييد كردو از ان پس متريك فريدمن به ابزار اصلي نظريه هاي كيهان شناسي تبديل شد.دراواخر دهه ي 1940،جرج گاموف وشاگردانش پيش بيني كردند كه جهان امروز بايد از تابش جسم سياه پر شده باشد ولي مشاهده ي تجربي اين پديده در سال 1965 انجام گرفت. در دهه ي 1970مشخص شداين تابش كه تابش ريزموج زمينه ي كيهانيCMB نام گرفت،به لحاظ توزيع فركانسي   داراي طيف تابش جسم سياه است.سرانجام جامعه ي علمي قانع شدند كه اين تابش باقي مانده اي از انفجار بزرگ است. بدين ترتيب مدل مهبانگ بعنوان مدل استانداردانفجار بزرگ پذيرفته شد. با كشف ويژگي همگني وهمسانگردي تابش زمينه ي كيهاني ،مشكلاتي چون تختي عالم،مشكل افق،مشكل تك قطبي ونيز منشا افت وخيزهاي اين تابش مطرح شدند كه كيهان شناسي استاندارد پاسخ قانع كننده اي براي اين مشكلات نداشت. كيهان شناسي تورمي اولين باربعنوان مدلي براي حل مشكلات نظريه ي استاندارد انفجار بزرگ ارائه شد.در اين الگو فرض مي شود كه ماده ي غالب جهان در لحظات اوليه پس از انفجار ،يك ميدان اسكالر است كه ميدان اينفليتون نام دارد.وجود اين ميدان باعث شده است كه انبساط عالم داراي شتابي مثبت باشد وبدين ترتيب در بازه ي بسيار بسيار كوچكي از زمان،شعاع عالم به مقدار زيادي رشد كرده است. يكي ازمسايل اساسي در كيهان شناسي نوين ،منشآ افت وخيز هاي اوليه ي ميدان تورمي زا در طول اين دوره ،بعنوان هسته ي اوليه ي تشكيل ساختارها مي باشد كه اين الگوي تورمي داراي پيش بيني هايي براي توزيع ناهمسانگردي ها واختلالات مشاهده شده در عالم است. در واقع ساختار هاي بزرگ مقياسي كه در جهان امروز مشاهده مي شوند،از افت وخيزهاي كوانتومي يك ميدان اسكالر در طي دوران تورمي در جهان اغازين ناشي شده اند .اختلال هاي نخستين كه در طي دوره ي تورم ايجاد شده اند، اثرشان روي توزيع ماده وتابش كاملا مشهود است. يكي از مهمترين نتايج مدل هاي تورمي اين است كه وجود طيف هايي براي اختلالات اسكالر واختلالات تانسوري كه به ترتيب عامل ايجاد ناهمگني چگالي ووامواج گرانشي هستند، پيش بيني مي كنند. اختلال هاي نخستين كه در طي تورم ايجاد شده اند ،اثرشان را روي طيف توان CMBنشان مي دهند وقيود قابل مشاهده اي را روي اين طيف ايجاد مي كنند .اثرات اين اختلالات را مي توان با محاسبه ي پارامترهاي اختلالي مدل هاي تورمي روي طيف توان CMB،مشاهده كرد. دراين پايان نامه مطالب، به شرح زير ارائه مي شوند:

  olar observations have been of great importance not only to solar physicists but also to geologists, astronomers and meteorologists. The main source of energy for the earth is the sun, and changes in solar radiation and its composition have a significant effect on the weather and, consequently, human activities. Su  ots can be mentioned as one of the components that may affect meteorological parameters and the earth's climate system, which can ultimately cause fluctuations and changes in these quantities. In this study, by using different statistical methods such as correlation analysis, spectral analysis of time series and scatter plots, focusing on stations in the west of the country, which include 4 stations of Hamedan, Kermanshah, Khorram Abad and Sanandaj, in order to understand the possible effect of su  ots on the behavior of quantities Precipitation, average temperature, relative humidity and sea level pressure in the statistical period from 1979 to 2021 were calculated and the necessary investigation was done. The analysis of the correlation coefficient on the main data of meteorological quantities and su  ot data showed the absence of a significant linear relationship between them. But this does not mean the absence of other relationships between the changes of su  ots and meteorological parameters. Using other statistical methods such as drawing scatter diagrams, spectral analysis and filtering data in the band related to the 11-year cycle in determining the type of relationship between solar activities and meteorological quantities and also determining the intensity of its influence on this quantity. It was very effective. The peak related to the 11-year periodicity of su  ots and its intensity in different meteorological quantities were revealed using spectral analysis. From the data distribution charts, it was concluded that there is a weak relationship between the number of su  ots and the probability of light and heavy rain events, relative humidity and low and high temperature in the west of the country. In relation to the amount of pressure, no significant effect was observed.

in 1916 , einstein expressed his theory of gravity as a second - order symmetric tensor , which is based on the theory of gravity as the curvature of spacetime .one of the ويژگيهاي of this theory is known as the بيني of the black hole as the field equation , the most simple جوابها in the four - dimensional case is called شوارتزشيلد and رايزنر - نوردستروم solution .the search for جوابهاي سياهچالهاي in space - the three - dimensional space in 1992 ended .بانادوس and his colleagues ( Banados - Teitelboim - Zanelli ) demonstrated that the field equations in the presence of the negative cosmological constant have also a non - stationary response ( if einstein used the cosmological constant to say that the universe is static , but it is later used to show the universe that is expanding ) [ 2 , 1 ] … this is called سياهچالههاي سياهچالههاي .later , سياهچالههاي BTZ were also obtained from solving the gravitational field equations coupled with maxwell 's electrodynamics [ 3 ] .next , the three - dimensional سياهچالههاي was introduced as the جوابهاي of the field equations in the presence of maxwell 's electrodynamics and in einstein - ديلاتون theory [ 5 , 4 ] .recently , a model of maxwell 's modified electrodynamics is introduced in the name of euler - heisenberg electrodynamics , which is used to study the scalar tensor of maxwell in scalar - tensor theory [ 6 ] .in ref . [ 7 ] , einstein 's field equations are solved in the presence of euler - heisenberg and cosmological constant .­­­­­­­­ at the end of the thesis we can develop a novel method based on the einstein - ديلاتون gravitational theory .for this purpose , euler - heisenberg electrodynamics is used as a model of nonlinear electrodynamics which is called maxwell 's modified model .first , by using the three - dimensional theory of euler - heisenberg 's lagrangian theorem , the coupled equations of tensor , vector , and scalar field equations are obtained in einstein 's theory and then by introducing a three - dimensional symmetric metric , the equations are obtained which are a second - order coupled system .in order to solve this problem , we use different حدسي مدلهاي to solve this problem by calculating the number of equations obtained for حلمعادلات and finding unknown unknowns .finally , we obtain the potential field of ديلاتوني , faraday 's law tensor , and the black solution of nonlinear charged چاله .by calculating the thermodynamic and thermodynamic properties of the black holes , the first law of ترموديناميكرابررسي is ميكنيم .the transition phase transition of the black hole is determined by using the canonical ensemble method and by calculating the black thermal capacity of the holes , the transition points of the first type and transition horizon of the second type and also the radius of the black event horizon are determined which are in the thermodynamic equilibrium state .

   In order to realize low cost and high-performance energy storage, it is very important to develop a doped cathode material for high capacity and long cycle lithium ion batteries. LiMn1.977(Ce, Cu, Ti, CeCuTi)0.023O4 nanoparticles are considered a promising cathode material due to incomparable high structural stability, high capacity and safety during the charge/discharge cycles. Here we report on the LiMn2O4 cathode doped with Ce, Cu, Ti, CeCuTi and CNT contamination. Among the pure LiMn2O4 and different doped LiMn2O4 samples, the Ti-doped LiMn2O4 cathode calcined at 700 ?C shows the highest capacity of 144.701 mAh.g-1 after 20 cycles with a high current density of 0.1 C which reaches 186.413 mAh.g-1with CNT doping (capacity retention=98.924 %). This is due to the small size of the Ti atom, resulting in high porosity for reversible storage of lithium, and also the presence of titanium in the lattice increases the dielectric constant. This study provides a reliable and easy way to fabricate and analyze LiMn1.977(Ce, Cu, Ti, CeCuTi)0.023O4 nanoparticle-based cathodes with excellent performance.

  The problem of the expansion of the universe is one of the biggest puzzles in modern astronomy. Scientists have discovered that our universe started with a big bang and has been expanding ever since. Researchers have tried to measure the current rate of expansion of the universe. In the first chapter, to investigate the amount of cosmic expansion, we introduce type la supernovae and then compare their observations for the luminosity distance as a function of redshift with the results of the supernova cosmology project and the high-Z supernova search team. By examining CMB, the Hubble constant is introduced to use this quantity to estimate the age of the universe since the Big Bang, and then to study the supernova data to detect the accelerating expansion of the universe. Then, by comparing the calculated luminosity distance in the non-matter or radiation, the effect of vacuum energy on the apparent luminosity was obtained. Then, the existence of dark energy is proved and its density instability is investigated. In the second chapter, we describe the classic problems of cosmology, namely the plane and the problem of the horizon, and examine the amount of inflation required to solve each. The exponential form increases, which means that the universe is growing rapidly, and the end of inflation occurs when some of the scalar field of inflation is paired with the fields of ordinary matter and radiation. In such a way that the density of the scalar field decreases and then the period of reheating occurs, which causes the entropy of the current world. In the third chapter, he first introduces Tachyon hot inflation and studies it in the contemporary theory of ring quantum gravity, using Poisson's bracket for LQC variables, obtains the classical Hamiltonian constraint and then the modified Friedman equation. Then we obtain the Hubble parameter and the pressure and density of energy and its Tachyon field potential, and then we define the parameters of slow rolling and by entering the condition of end of inflation, we obtain the value of power e. In the next section, we study the cosmic perturbations of the Tachyon hot-inflation model, including curvature perturbation, entropy perturbation, and density perturbation, and the scalar index in the high dissipative regime, which leads to the perturbation spectrum, and describe its relationships. We obtain the Einstein turbulent field equation for the Fourier components e^ikx and then calculate the exponential potential of the Tachyon field.

   در كل كار مافرض كرده ايم كه ميدان تورم در معادله حركت در غلتش ثابت قابل قبول است. ما فرض مي كنيم كه تورم با هيچ قشر ديگري همراه نيست بنابراين تورم سرد است. در ادامه كه برسي ما شامل يك مدل تورمي ثابت جديد نيست، اما حاوي يك رويكردي جديد براي بازسازي پتانسيل تورمي كه ثبات تكامل ميدان را ثابت مي كند. به جاي استفاده از ميدان به عنوان متغير، ما از تعدادي عدد توان الكترونيكي استفاده مي كنيم كه به نظر مي رسد يك ابزار مفيد در تورم گرم است. راه حل هاي تحليلي براي پارامترهابل، ميدان اسكالر و پتانسيل به عنوان تابعي از عدد توان الكتذوني، محاسبه شده است. سرانجام، نشان داده شد كه اين روش كاملاً منطبق است بر تحليل راه حل هايي كه تاكنون در تورم   غلتش ثابت به دست آمده است.

   The three approach to relativistic generalization of coherent state are discussed in the simplest case of a spinless   article: the standard, canonical, coherent states, the Lorentzian state and the coherent state introduced by Kaiser and independently by Twareque Ali,Antoine and Gazeau. All treatment utilize the Newton-Wigner localization avd dynamics described by saltpeter equation .The behavior of expectation values of relativistic observables in coherent state is analyzed in detail and the Heisenberg uncertainty relation are investigated.

Abstract    In this work, a geophysical study is conducted on Sarableh plain which is located in Sarableh city, Chardavol district, Ilam province. The objective of this research is to investigate the geology of aquifers in order to determine optimal locations for well drilling based on electrical resistivity measurements of subsurface structures.   67 electrical sounding with electrode spacing of up to 1000 m were conducted in the area. Configuration of electrical soundings included 10 profiles with average spacing of 800 m between adjacent profiles while based on topology, the spacing ranges from 500 m to 1500 m. Measured apparent resistivities were mapped for all electrode spacing and resistivity sections in profiles 2, 3, 4, 5, and 9 based on the one-dimensional and two-dimensional inverse modeling were calculated Using ZondRes2d software. Finally by interpretation of apparent resistivity maps and resistivity sections, the optimal locations for well drilling were obtained by considering aquifer geometry and water recharges. The best location turns out to be at ditance of 3000 m from the start point of profile 9. The depth of the drilling well should be 120 m. An alternative option is drilling of a 150 m well at distance of 1700-1800 m from the start point of profile 5. Keywords: Groundwaters; Schlumberger array; Resistivity method; Sarableh field; one-dimensional and two-dimensional inverse modeling; resistivity pseudo-sections.

We study the damping of longitudinaloscillations of a prominence thread caused by the mass accretion.Wesuggested asimple modeldescribing this phenomenon. In this model we considered a thincurved magnetictube filled with the plasma. The prominence threadis in thecentral part of the tube and it consists of densecold plasma. The parts of thetube at the two sides of the thread are filledwith hot rarefied plasma. Weassume that there are flows of rarefied plasma toward the thread caused by theplasma evaporation at themagnetic tube footpoints. Our main assumption is thatthe hot plasma is instantaneously accommodated bythe thread when it arrivesatthe thread, and its temperature and density become equal to those of thethread. Then we derive the system of ordinary differentialequations describingthe thread dynamics. We solve this system of ordinary differential equations intwo particular cases. In the firstcase we assume that the magnetic tube iscomposed of an arc of a circle with two straight lines attached to its endssuch that the wholecurve is smooth. A very important property of this model isthat the equations describing the thread oscillations are linear foranyoscillation amplitude. We obtain the analytical solution of the governingequations. Then we obtain the analytical expressions for theoscillation dampingtime and periods. We find that the damping time is inversely proportional tothe accretion rate. The oscillationperiods increase with time.We conclude thatthe oscillations can damp in a few periods if the inclination angle is sufficientlysmall, notlarger that 10° , and the flow speed is sufficiently large, notless that 30 kms-1 . In the second model we consider the tube withthe shapeof an arc of a circle. The thread oscillates with the pendulumfrequency dependent exclusively on the radius of curvature of the arc.Thedamping depends on the mass accretion rate and the initial mass of the threathatis the mass of the thread at the moment whenit is perturbed. First we considersmall amplitude oscillations and use the linear description.

 abstract

  In this study, we investigate the Nonaxi symmetric oscillations of thin twisted magnetic flux tubes in two states. First, when the magnetic field inside and outside the magnetic flux tube is twisted and the twist is weak. Then, while the magnetic field outside the tube is straight and homogenous, however it is twisted inside the tube. And secondly we add the equilibrium current of the plasma along the magnetic field. And by adding the flow effect, we study the frequency of the oscillations in the presence of current, we obtain the magnetic pressure relationship inside and outside the magnetic flux tubes, and by applying boundary conditions we obtain the dispersion relation. Using the dispersion realtion we plot the graph ?? in terms of ????. And we see that the frequency of kink oscillations increases in the presence of the equilibrium current of the plasma.

در اين پايان نامه، تابش هاي باردار به دو دسته تقسيم مي شود.گروه اول الكترون و پوزيترون و گروه دوم ذرات سنگين مانند ذرات آلفا،پروتون، ميون و ساير هسته هاي سنگين را دربرمي گيرد.براي محاسبه توان توقف پروتون و آلفا از رابطه بته بلاخ استفاده مي شود.ميزان اتلاف انرژي پروتون وآلفارا در ماهيچه،استخوان وبافت نرم با استفاده از نرم افزار ميپل محاسبه كرده ونتايج آن را با استفاده از نرم افزار اوريجين در نمودارها نشان داده شده است.توان توقف پروتون و آلفا را در آب و طلا بدون تصحيح وبا درنظر گرفتن تصحيح اثر چگالي محاسبه شده است.اثر چگالي در انرژي هاي بالا، باعث كاهش ميزان توان توقف مي شود.توان توقف پروتون و آلفا را در آلومينيوم بدون تصحيح و بادر نظر گرفتن تصحيحات اثر چگالي، باركاس و بلاخ نيز انجام داده شده است.بررسي ها نشان مي دهد كه توان توقف با تصحيح اثر باركاس و بلاخ در انرژي هاي پايين كاهش مي يابد. 

In this study, we investigate the entangled coherent states and their decoherence. We briefly introduce the coherent states which have been identified in physics and then the introduction and creation of   loch coherent states are dealt with.‎‎‎‎ We examine these states from different points of view, namely, group theory, irreducible representations and also from Fock Bargmann's viewpoint. Moreover, we investigate the entangled coherent states which are among the most important states in quantum information processing. ‎‎‎‎‎There are some criteria for the study of these states, including ‎B‎ell inequality, entropy, fidelity and entanglement of formation, which will be explained here in brief. ‎ ‎‎We will examine the qubit of orthogonal coherent states. We present these states on ‎B‎loch sphere.‎ ‎‎‎‎‎In quantum optics, a possible method of producing the entangled states of two mode of light field, is transmission of single mode state and its interference with another state (vacuum state) on a beam splitter. ‎‎‎We will calculate the amount of entanglement in these states which can be produced in beam splitter. The entangled states which are produced by using this method, are the entangled coherent states.‎ ‎‎‎‎‎‎We will describe the decoherence of ‎these‎ coherent state ‎qubits‎‎ and finally, using the adaptive Bloch sphere, we will provide an interpretation of these states.‎‎‎‎‎

  This thesis studies vanishing of Ext modules over Cohen–Macaulay local rings. The main result of this thesis implies that the Auslander–Reiten conjecture holds for maximal Cohen–Macaulay modules of rank one over Cohen–Macaulay normal local rings. It also recovers a theorem of Avramov– Buchweitz–S¸ega and Hanes–Huneke, which shows that the Tachikawa conjecture holds for Cohen–Macaulay generically Gorenstein local rings. This conjecture is widely open in general, even for modules overcommutativeNoetherianlocalrings. Oversuchrings,weprovethatalargeclass of ideals satisfy the extension condition proposed in the aforementioned conjecture of Auslander and Reiten. Keywords: Auslander-Reitenconjecture,Cohen-Macaulyring,Normalring,Gornestein ring, Free module, Weakly m-full and Ext module.

 quarkonium production

 0

Ternary fragmentation by calculating the potential energy surfaces (PES)with the inclusion of deformation and orientation degrees of freedom forthe 4He- and 10Be-accompanied fission of the 252Cf nucleus is studied. most favored ternary fragmentation channels in the light charged particles(4He and/or 10Be)-accompanied fission of the 252Cf nucleus are predictedusing the PES calculations. The sensitivity of PES due to the groundstate quadrupole deformation (?2) and the orientation effects (90?–90? and0?–0?) of the fragments are analyzed.

  Internal solitons generated at the Columbia River plume front during ebb tides are revealed in Synthetic Aperture Radar (SAR) images. Scale analyses indicated that these internal waves belong to the finite-depth category. Based on the study by Zheng et al. [2002], a theoretical model for the finite-depth category was developed that relates radar backscatter cross-section to dynamic parameters of internal solitons. Using the theoretical model and in-situ density data collected by the River Influences on Shelf Ecosystem (RISE) project cruise in July 2004, we obtained the half width, amplitude, phase speed, and wave energy per crest length of the internal solitons at four.

A fully quantum mechanical model of two-component Manakov solitons is developed in both the Heisenberg and Schr?dinger representations, followed by an analytical, linearized quantum theory of Manakov solitons in the Heisenberg picture. This theory is used to analyze the vacuum-induced fluctuations of Manakov soliton propagation and collision. The vacuum fluctuations induce phase diffusion and dispersion in Manakov soliton propagation. Calculations of the position, polarization angle, and polarization state fluctuations show an increase in collision-induced noise with a decrease in the relative velocity between the two solitons, as expected because of an increase in the interaction length. Fluctuations in both the polarization angle and state are shown to be independent of propagation distance, opening up possibilities for communications, switching, and logic, exploiting these properties of Manakov solitons.

  We have investigated the effect of thermal conduction and compressive viscosity on the damping of longitudinal magnetohydrodynamic waves generated in a cooling background in a uniformly magnetised plasma. Compressive viscosity and thermal conduction are assumed to be the dominant mechanisms for the damping of the oscillations in hot coronal loops. We have assumed the low-beta plasma to use the rigid flux tube approximation, which enables us to disregard the magnetic field perturbation therefore the magnetic field was assumed to be constant and aligned along the z-direction. The background temperature is allowed to change as a function of time and to decay exponentially with characteristic cooling times typical for coronal loops which is much longer than the characteristic oscillation period P, i.e., that we consider a temporally slowly varying plasma. The latter assumption has allowed us to use the WKB method to model the damped oscillations. In the leading order approximation of the WKB method, called the approximation of geometrical optics, we have derived the dispersion equation determining the instantaneous complex frequency of the loop oscillation. In the next order approximation, called the approximation of physical optics, we have obtained the equation determining the variation of oscillation amplitude with time.   We have used the analytical results to estimate the dependence of the oscillation amplitude on time numerically. We have obtained in cold loops the damping due to compressive viscosity is very weak and in hott loops the damping of oscillation becomes stronger also, cooling reduces the damping rate due to compressive viscosity. But in loops with higher temperature, taking into account the effects of compressive viscosity and thermal conduction can overcome the effect of cooling and the oscillation amplitude secreases with time in cooling coronal loops.

  حالت هاي همدوس عموما يك ارتباط تنگاتنگ بين روابط كلاسيك و كوانتومي يك سيستم داده شده را فراهم مي آورد. اين حالت ها در حقيقت ويژه بردارهايي خاص در فضاي هيلبرت مي باشند كه حداقل داراي سه ويژگي مهم پيوستگي، نرماليزه پذيري و رابطه هماني را دارا مي باشند. كوانتش يك نگاشت انتگرالي مي باشد كه ما را از فضاي كلاسيك به فضاي كوانتومي مي برد. در اين پايان نامه حالتي را در نظر مي گيريم كه در مكانيك كوانتومي استاندارد وجود ندارد و مكانيك كوانتوم استاندارد قادر به توجيه آن نيست، براي حل اين مشكل از حالت هاي همدوس كمك مي گيريم. با استفاده از كوانتش انتگرالي برزين، مقدار كلاسيكي تابع( مشاهده پذير ) را در نگاشت انتگرالي قرار داده و معادل كوانتومي آن ( عملگر ) را بدست خواهيم آورد. فضاهاي ناجابجايي دو بعدي مي توانند سطح تخت ناجابه جايي و يا سطح كره ناجابجايي و يا هر سطح خميده ديگر باشند. در اينجا حالت هاي همدوس را در سطح تخت ناجابجايي (صفحه ناجابجا) بررسي مي كنيم. منظور از ناجابجايي مختصات، ناجابجايي مكاني است و ناجابه جايي را بين مختصه هاي زماني در نظر نمي گيريم زيرا از لحاظ مفاهيم يكتايي و عليت دچار مشكل مي شويم. همچنين سه شرط پيوستگي، نرماليزه پذيري و رابطه هماني را برا ي حالت هاي همدوس در فضاي ناجابجا بررسي مي كنيم

  Black holes are objects in the cosmos have amazing compact and heavy objects that even light does not pass through the discovery of quasars, black holes were discovered fact. Super red shift quasars Vtabshy a thousand light years are less than the diameter of a typical galaxy

   فصل اول اين پايان نامه بررسي مختصري از ساختار خورشيد و پديده هاي آن مي باشد.در فصل دوم بررسي امواج مغناطوهيدرديناميكي و معادلات توصيف كننده ي اين امواج را خواهيم داشت. در فصل سوم امواج سوسيسي در لوله هاي تاج خورشيد رامورد بررسي قرار خواهيم داد. در فصل چهارم  به بررسي اثر جريان بر طول موج هاي قطع و فركانس امواج سوسيسي سريع در لوله هاي تاج خورشيد با ميدان مغناطيسي پيچشي خواهيم پرداخت.

 In this thesis, zohdys method which was firstly applied, as a quick method, to interpret geoelectrical Schlumberger and Wenner data, is used to invert frequency domain airborne electromagnetic (AEM) data. This method is based on a layered earth and without having an initial guess, the number thickness and conductivity of the ground can be calculated. Basically, this method is a kind of forward modelling in which the starting model is created from data itself. Then this model changes in thickness and conductivity of layers so that the difference between observed data and calculated data from changing model reaches to a minimum. Now, the model of the earth is founded. This method is applied on airborne electromagnetic (AEM) data from one and two dimensional synthetic multi-layer models and the result show that zohdys method has acceptable performance to retrieve conductivity and thickness values of earth layers.