京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第22248号 / 理博第4562号 / 新制||理||1655(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 野上 大作, 教授 嶺重 慎, 教授 長田 哲也 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第18797号 / 理博第4055号 / 新制||理||1583(附属図書館) / 31748 / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 上田 佳宏, 教授 太田 耕司, 教授 嶺重 慎 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

Accretion disks around black holes with gas radiating out parts of its gravitational potential energy have long served as objects of both theoretical and observational studies. By solving the structure equations of the disk it is possible to predict the outgoing radia- tive flux and the observed spectrum of the disk and test the validity of the theory against direct observations. The standard thin disk model (Shakura-Sunyaev, Novikov-Thorne) shows, however, a still unexplained non-negligible deviance in the observed spectrum at higher mass accretion rates. To amend to the set of proposed explanations, in this thesis we examine the effect of the magnetic pressure on the trapping of some of the internal energy generated by viscous dissipation processes in the disk and advecting this energy to the black hole. A phenomenological description of heat advection mediated by a highly heterogenous magnetic field will be given, as well as its effect on the spectrum and observed effective temperature. 1

Graph theoretic modeling has served as an invaluable tool for solving a variety of problems since its introduction in Euler's paper on the Bridges of Königsberg in 1736 . Two amongst them of contemporary interest are the modeling of Redundant Arrays of Inexpensive Disks (RAID), and the identification of network attacks. While the former is vital to the protection and uninterrupted availability of data, the latter is crucial to the integrity of systems comprising networks. Both are of practical importance due to the continuing growth of data and its demand at increasing numbers of geographically distributed locations through the use of networks such as the Internet. The popularity of RAID has soared because of the enhanced I/O bandwidths and large capacities they offer at low cost. However, the demand for bigger capacities has led to the use of larger arrays with increased probability of random disk failures. This has motivated the need for RAID systems to tolerate two or more disk failures, without sacrificing performance or storage space. To this end, we shall first perform a comparative study of the existing techniques that achieve this objective. Next, we shall devise novel graph-theoretic algorithms for placing data and parity in arrays of n disks (n ≥ 3) that can recover from two random disk failures, for n = p - 1, n = p and n = 2p - 2, where p is a prime number. Each shall be shown to utilize an optimal ratio of space for storing parity. We shall also show how to extend the algorithms to arrays with an arbitrary number of disks, albeit with non-optimal values for the aforementioned ratio. The growth of the Internet has led to the increased proliferation of malignant applications seeking to breach the security of networked systems. Hence, considerable effort has been focused on detecting and predicting the attacks they perpetrate. However, the enormity of the Internet poses a challenge to representing and analyzing them by using scalable models. Furthermore, forecasting the systems that they are likely to exploit in the future is difficult due to the unavailability of complete information on network vulnerabilities. We shall present a technique that identifies attacks on large networks using a scalable model, while filtering for false positives and negatives. Furthermore, it also forecasts the propagation of security failures proliferated by attacks over time and their likely targets in the future.

Super Earths are a class of exoplanets with masses between 1-10 M⊕. Comprising nearly 70 % of the discovered planet population, they are largest class of exoplanets known. Super Earths exhibit an interesting variety of compositions, as their densities imply that they range from dense, rocky planets to those with substantial amounts of water. This thesis aims to understand why super Earths form so frequently, and to connect the final compositions of super Earths to the regions where they form in protoplanetary disks. To do this, we combine a model that calculates the physical and chemical conditions within a protoplanetary disk with a core accretion model of planet formation. A key feature of our planet formation model is planet traps that act as barriers to rapid type-I migration. The traps we include in our model are the dead zone, which can be caused by cosmic ray or X-ray ionization, the ice line, and the heat transition. In disks with lifetimes >􏰐 4 Myr we find that planet formation in all traps results in Jovian planets. Typically, the X-ray dead zone and heat transition traps produce hot Jupiters orbiting near 0.05 AU while the cosmic ray dead zone and ice line traps produce Jupiters near 1 AU. Super Earths are found to form in disks with short lifetimes 􏰑< 2 Myr that photoevaporate prior to planets undergoing runaway gas accretion. Additionally, we find that super Earth formation takes place in low-mass disks (<􏰑 0.05 M⊙), where planet formation timescales exceed disk lifetimes inferred through observations. The location of various traps throughout the disk play a key role in allowing super Earths to achieve a range of compositions. Super Earths forming in the ice line or heat transition accrete solids from cold regions of the disk, resulting in planets with large ice contents (up to 50 % by mass). Conversely, super Earths formed in the dead zone trap accrete solids from warm regions of the disk and are therefore composed of mostly rocky materials (less than 5 % ice by mass). / Thesis / Master of Science (MSc)

No description available.

No description available.

<p> Fragmentation during encounters between protostellar disks provides a possible scenario for the formation of substellar objects such as brown dwarfs and planets. A series of simulations of protostellar disk encounters were performed to investigate the fragmentation under different encounter parameters, and to characterize the properties of any resultant fragments. It was found that the initial disk minimum Toomre Q must satisfy Qini ;S 1.1 for the fragmentation to be induced by the encounters. Fragments of substellar mass can form via disk fragmentation, shock layer fragmentation and tidal tail fragmentation, and the effectiveness of each mechanism is closely related to the initial disk configuration. The fragmentation is also constrained by the relative encounter velocity since the number of fragments decreases quickly with increasing velocity. </p> <p> In comparing to previous studies of protostellar disk encounters it was also found that resolving both the local Jeans Mass during the encounter and the disks' vertical structure are critical to prevent artificial fragmentation and give the correct picture. Heating and cooling rates were estimated in both the optically thin and thick regimes. The comparison between the two indicates that during strong impacts the heating rate increases rapidly but is still comparable to the cooling rate, so the locally isothermal equation of state used in this study is an acceptable approximation. </p> <p> 32 clumps formed in various Qini = 0.9 disk-disk encounters were taken as the sample in an analysis of fragment properties and prospects for their further evolution. The results show that the clump masses are all less than the hydrogen burning mass limit ~ 0.075M0 , so the objects are substellar. Most of the clumps are of brown dwarf mass since the formation of planetary mass clumps is suppressed due to numerical resolution. The mass distribution is broadly consistent to the observed initial mass function in Pleiades. The clumps have highly flattened disk-like shapes and possess large spin angular momentum, which implies that young brown dwarfs may develop disks, jets, or planetary mass companions. About one third of the fragments are unbound to the stars and likely to form free floating brown dwarfs. Orbital analyses of the clumps which are bound to the stars show that there is a lack of close brown dwarf companions ( R < 3 AU), which is consistent to the observed "brown dwarf desert". Many of the orbits are highly eccentric and intersect with other orbits, so ejection of some clumps due to gravitational scattering is likely. Also, dispersion of gas during the encounter and the high spin angular momentum of the clumps may provide mechanisms other than ejection to prevent the clumps from accreting more mass, making the simulated clumps representative of the long term substellar mass function. </p> / Thesis / Master of Science (MSc)

The problem of finding the stress distribution about circular, noncentral holes in a spinning disk is discussed. A theoretical approximation is first developed using the methods of elasticity and combining solutions to similar problems from Ling (reference 6) and Timoshenko and Goodier (reference 2). Results are then found in the form of a maximum stress concentration factor which occurs at the edges of the holes. The accuracy of the derived solution is checked by obtaining values photoelastically from a similar spinning disk. Stress patterns are studied in photographs obtained with a strobeflash and camera. The results are presented in a usable form for application to design. / Master of Science

Redundant Arrays of Inexpensive Disks or RAID is a popular method of improving the reliability and performance of disk storage. Of various levels of RAID, mirrored or RAID1 and rotating parity or RAID5 configurations have become moat popular. Mirrored or RAID1 provides best overall performance and is easier to configure, but has 100 percent storage overhead for the redundancy. Rotating parity or RAID5, on the other hand, is quite inexpensive for the redundancy it provides, shorn impressive performance for reads and full-stripe writes in normal mode, but the small write performance is poor due to the read-modify-write cycle involved. The performance drops drastically when one of the disks fails and the system enters degraded mode. Also RAID5 is relatively difficult to configure. Typical non-scientific system disk access patterns exhibit very high locality of reference. This thesis presents the design and implementation of an Adaptive Hierarchical RAID array to exploit this high locality. Frequently accessed data is migrated towards the top of the hierarchy and not so frequently acee88ed data is moved down the hierarchy, thus adaptively rearranging itself to the access patterns. Previous work on Adaptive Hierarchical RAID such as HP AutoRAID has explored one part of the design space, namely design of configurable storage at the SGSI level with no interaction with higher level layers like volume manager. This thesis explores a different design point: namely, one that is centered at the volume manager layer. This is important also for the reason that with fibre channel disks and SCSI-3, Storage Area Networks (SAN) no longer need a conventional controller but a modified version of a controller that is more close to a volume manager.