Peer To Peer File Sharing
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This document discusses peer-to-peer (P2P) file sharing. It describes three common P2P architectures: centralized directory, query flooding, and exploiting heterogeneity. The centralized directory model uses a central server to store peer information and facilitate file transfers. Query flooding passes search requests between connected peers until the requested file is located. Exploiting heterogeneity designates some peers as super nodes to improve search efficiency. Advantages of P2P networks over client-server models include scalability, redundancy, and lower costs. However, P2P networks can be less stable and secure as peer numbers increase.
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Context. The early-type galaxy SDSS J133519.91+072807.4 (hereafter SDSS1335+0728), which had exhibited no prior optical variations during the preceding two decades, began showing significant nuclear variability in the Zwicky Transient Facility (ZTF) alert stream from December 2019 (as ZTF19acnskyy). This variability behaviour, coupled with the host-galaxy properties, suggests that SDSS1335+0728 hosts a ∼ 106M⊙ black hole (BH) that is currently in the process of ‘turning on’. Aims. We present a multi-wavelength photometric analysis and spectroscopic follow-up performed with the aim of better understanding the origin of the nuclear variations detected in SDSS1335+0728. Methods. We used archival photometry (from WISE, 2MASS, SDSS, GALEX, eROSITA) and spectroscopic data (from SDSS and LAMOST) to study the state of SDSS1335+0728 prior to December 2019, and new observations from Swift, SOAR/Goodman, VLT/X-shooter, and Keck/LRIS taken after its turn-on to characterise its current state. We analysed the variability of SDSS1335+0728 in the X-ray/UV/optical/mid-infrared range, modelled its spectral energy distribution prior to and after December 2019, and studied the evolution of its UV/optical spectra. Results. From our multi-wavelength photometric analysis, we find that: (a) since 2021, the UV flux (from Swift/UVOT observations) is four times brighter than the flux reported by GALEX in 2004; (b) since June 2022, the mid-infrared flux has risen more than two times, and the W1−W2 WISE colour has become redder; and (c) since February 2024, the source has begun showing X-ray emission. From our spectroscopic follow-up, we see that (i) the narrow emission line ratios are now consistent with a more energetic ionising continuum; (ii) broad emission lines are not detected; and (iii) the [OIII] line increased its flux ∼ 3.6 years after the first ZTF alert, which implies a relatively compact narrow-line-emitting region. Conclusions. We conclude that the variations observed in SDSS1335+0728 could be either explained by a ∼ 106M⊙ AGN that is just turning on or by an exotic tidal disruption event (TDE). If the former is true, SDSS1335+0728 is one of the strongest cases of an AGNobserved in the process of activating. If the latter were found to be the case, it would correspond to the longest and faintest TDE ever observed (or another class of still unknown nuclear transient). Future observations of SDSS1335+0728 are crucial to further understand its behaviour. Key words. galaxies: active– accretion, accretion discs– galaxies: individual: SDSS J133519.91+072807.4
Synopsis presentation VDR gene polymorphism and anemia (2).pptx
I am the PhD scholar of FND department, Assam down town University
Mechanisms and Applications of Antiviral Neutralizing Antibodies - Creative B...
Neutralizing antibodies, pivotal in immune defense, specifically bind and inhibit viral pathogens, thereby playing a crucial role in protecting against and mitigating infectious diseases. In this slide, we will introduce what antibodies and neutralizing antibodies are, the production and regulation of neutralizing antibodies, their mechanisms of action, classification and applications, as well as the challenges they face.
Analysis of Polygenic Traits (GPB-602)
Quantitative genetics – study of inheritance of quantitative characters or polygenic characters in experimental populations.
Embracing Deep Variability For Reproducibility and Replicability
Embracing Deep Variability For Reproducibility and ReplicabilityUniversity of Rennes, INSA Rennes, Inria/IRISA, CNRS
Embracing Deep Variability For Reproducibility and Replicability
Abstract: Reproducibility (aka determinism in some cases) constitutes a fundamental aspect in various fields of computer science, such as floating-point computations in numerical analysis and simulation, concurrency models in parallelism, reproducible builds for third parties integration and packaging, and containerization for execution environments. These concepts, while pervasive across diverse concerns, often exhibit intricate inter-dependencies, making it challenging to achieve a comprehensive understanding. In this short and vision paper we delve into the application of software engineering techniques, specifically variability management, to systematically identify and explicit points of variability that may give rise to reproducibility issues (eg language, libraries, compiler, virtual machine, OS, environment variables, etc). The primary objectives are: i) gaining insights into the variability layers and their possible interactions, ii) capturing and documenting configurations for the sake of reproducibility, and iii) exploring diverse configurations to replicate, and hence validate and ensure the robustness of results. By adopting these methodologies, we aim to address the complexities associated with reproducibility and replicability in modern software systems and environments, facilitating a more comprehensive and nuanced perspective on these critical aspects.
https://hal.science/hal-04582287
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDS
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
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Sexuality - Issues, Attitude and Behaviour - Applied Social Psychology - Psyc...
A proprietary approach developed by bringing together the best of learning theories from Psychology, design principles from the world of visualization, and pedagogical methods from over a decade of training experience, that enables you to: Learn better, faster!
Mites,Slug,Snail_Infesting agricultural crops.pdf
Order : Trombidiformes (Acarina) Class : Arachnida
Mites normally feed on the undersurface of the leaves but the symptoms are more easily seen on the uppersurface.
Tetranychids produce blotching (Spots) on the leaf-surface.
Tarsonemids and Eriophyids produce distortion (twist), puckering (Folds) or stunting (Short) of leaves.
Eriophyids produce distinct galls or blisters (fluid-filled sac in the outer layer)
Farming systems analysis: what have we learnt?.pptx
Presentation given at the official farewell of Prof Ken Gillet at Wageningen on 13 June 2024
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SDSS1335+0728: The awakening of a ∼ 106M⊙ black hole⋆
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Mechanisms and Applications of Antiviral Neutralizing Antibodies - Creative B...
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Juaristi, Jon. - El canon espanol. El legado de la cultura española a la civi...
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Sexuality - Issues, Attitude and Behaviour - Applied Social Psychology - Psyc...
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Peer To Peer File Sharing
- 1. INTERNAL PEER TO PEER FILE SHARING SYIFA NURJANAH 00120190407015
- 2. INTERNALP2P POSITIONS 1. Still running even without server 2. A peer is directly communicate with other peer 3. All those peer can get the IP address depending on the underlying architecture supported the p2p system
- 3. INTERNALHOW DOES IT WORK 1. Still running even without server 2. A peer is directly communicate with other peer 3. All those peer can get the IP address depending on the underlying architecture supported the p2p system
- 4. INTERNAL P2P ARCHITECTURE 1. Centrilized Directory • Now whenever a requesting peer comes in, it sends its query to the server. • Since the server has all the information of its peers, so it returns the IP addresses of all the peers having the requested file to the peer. • Now the file transfer takes place between these two peers. E.G Napster
- 5. INTERNAL P2P ARCHITECTURE 2. Query Flooding • Now when one peer requests for some file, this request is sent to all its neighboring nodes i.e. to all nodes which are connected to this node. If those nodes don’t have the required file, they pass on the query to their neighbors and so on. This is called as query flooding. • When the peer with requested file is found (referred to as query hit), the query flooding stops and it sends back the file name and file size to the client, thus following the reverse path. • If there are multiple query hits, the client selects from one of these peers. E.G Gnutella
- 6. INTERNAL P2P ARCHITECTURE 3. Exploiting heterogeneity • This structure can process the queries in two ways. • The first one is that the super nodes could contact other super nodes and merge their databases with its own database. Thus, this super node now has information of a large number of peers. • Another approach is that when a query comes in, it is forwarded to the neighboring super nodes until a match is found, just like in Gnutella. Thus query flooding exists but with limited scope as each super node has many child peers. Hence, such a system exploits the heterogeneity of the peers by designating some of them as group leaders/super nodes and others as their child peers. • . E.G KaZaA
- 7. INTERNAL VERSUS OF CS AND P2P CS P2P Client dan server dibedakan, berdasarkan spesifik server dan client Client dan server tidak berbeda Client server berfokus pada pembagian informasi Berfokus pada konektivitas Server yang tersentral di gunakan untuk menyimpan data Setiap peer memiliki masing masing data Server merespon service yang di request client Setiap node bisa melakukan request dan respond Lebih mahal secara biaya Tidak semahal biaya client server Lebih stabil Jika jumlah peer meningkat tingkat kestabilan rendah
- 8. INTERNAL P2P USEFUL EXTREAMLY SCALABLE DIFFICULT TO TAKE DOWN THE MORE P2P LARGER IT BECOMES FASTER WHY P2P IS USEFULL
- 9. INTERNAL ADVANTAGES OS IS NO NEEDED EXPENSIVE SERVER IS NO NEED EXPENSIVE SERVER IS NO NEED EASIER TO SET UP ONE COMPUTER FAILS IT WON’T DISTRUPTING THE NEWTORK DISADVANTAGED EASY TO SLOW DOWN WHILE COMPUTERS BEING ACCESS BY OTHER FILE AND FOLDER CAN NOT BE CENTRALLY BACK UP FILE AND RESOURCE NOT CENTRELIZED IN SPECIFIC AREA REGARDING THE SECURITY IT’S A LITLE OR EVEN NO SECURITY WHY P2P IS USEFULL
- 10. INTERNAL References • P2P(Peer To Peer) File Sharing. Accessed on October 16th 2019. • https://www.geeksforgeeks.org/p2ppeer-to-peer-file-sharing/ • A Brief History of P2P Content Distribution, in 10 Major Steps. Accessed on October 16th 2019. https://medium.com/paratii/a-brief-history-of-p2p-content-distribution-in-10-major-steps-6d6733d25122 • Peer-to-peer file sharing. Accessed on October 16th 2019. • https://en.wikipedia.org/wiki/Peer-to-peer_file_sharing • Pure P2P architecture P2P: centralized directory no. Accessed on 16th 2019 . https://studylib.net/doc/13347485/pure-p2p- architecture-p2p--centralized-directory-no • Difference between Client-Server and Peer-to-Peer Network. Accessed on October 16th. 2019 https://www.geeksforgeeks.org/difference-between-client-server-and-peer-to-peer-network/ • Slides from Werner Nutt Slides (lecturer of University Bozen Balzano. Accessed on October 15th 2019 • http://www.inf.unibz.it/~nutt/Teaching/DSs1011/dss-slides.html