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What is the purpose of a document management system (DMS)?
Document management system is a single solution which helps you create documents, collaboratively edit them, share documents with colleagues and business partners to be signed and completed and, finally, securely store them.An advanced document management system allows you to easily manage the entire document lifecycle online within a single browser tab, without mountains of paperwork and time consuming steps.That’s why it so important to choose the right DMS.These are the main benefits of using DMS for your small business or large enterprise:> Save time editing PDF document with a powerful online PDF editorMost contracts, agreements and proposals are saved and distributed as PDFs. With an online PDF Editor you can do everything you need from fixing a typo, adding information to completely reformatting a PDF document. Annotation tools make it fast and convenient to work collaboratively using PDFs.> Close deals faster with with e-signatures and fillable formsTurn a PDF into a fillable form such as a job application or patient intake form that retains your company branding and can be hosted on your website, shared via a link or QR code. Send agreements to be signed by other parties on a desktop or mobile device. You can even collect payments for services once your clients submit fillable forms with their information.> Cut Costs with Powerful Data Processing & Document GenerationAutomatically generate hundreds of forms pre-filled with data from a spreadsheet, information that you gathered using online fillable forms or customer data from a CRM. It’s also possible to automate data extraction from hundreds of forms, saving hours of tedious office work. None of this requires any coding.> Work More Efficiently Using IntegrationsIntegrate a document management system with your favorite CRM, cloud storage or other productivity platforms to cut processing costs and increase the productivity of your team.If you want to make your business more efficient, don’t wait for Monday: start looking for the right document system right now.
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Is Evolution founded on scientific proof, or is it a godless worldview founded on supposition?
Science does not operate on a 'proof' model, it is a falsification model where the hypothesis that is best supported by mountains of evidence and not falsified are promoted to Scientific Theory status.Here are just a tiny few of the many tens of thousands of studies that support Evolutionary theory - each such paper contains a record of the scientific methodology applied and the scientific evidence produced so it can be challenged or reproduced by other researchers.Theobald, D. L. 2010. A formal test of the theory of universal common ancestry. Nature 465:219-223Adl, S., Leander, B.S., Simpson, A.G.B., Archibald, J.M., Anderson, O.R., Bass, D., Bowser, S.S., Brugerolle, G., Farmer, M.A., Karpov, S., Kolisko, M., Lane, C.E., Lodge, D.J., Mann, D.G., Meisterfeld, R., Mendoza, L., Moestrup, Ø., Mozley-Standridge, S.E., Smirnov, A.V., and Spiegel, F. (2007) Diversity, nomenclature, and taxonomy of protists. Syst. Biol., 56, 684-689.Adl, S.M., Simpson, A.G., Farmer, M.A., Andersen, R.A., Anderson, O.R., Barta, J.R., Bowser, S.S., Brugerolle, G., Fensome, R.A., Fredericq, S., James, T.Y., Karpov, S., Kugrens, P., Krug, J., Lane, C.E., Lewis, L.A., Lodge, J., Lynn, D.H., Mann, D.G., McCourt, R.M., Mendoza, L., Moestrup, O., Mozley-Standridge, S.E., Nerad, T.A., Shearer, C.A., Smirnov, A.V., Spiegel, F.W. and Taylor, M.F. (2005) The new higher level classification of eukaryotes with emphasis on the taxonomy of protists. J. Eukaryot. Microbiol., 52, 399-451.Adoutte, A., G. Balavoine, N. Lartillot, O. Lespinet, B. Prud'homme, and R. de Rosa. 2000. The new animal phylogeny: Reliability and implications. Proceedings of the National Academy of Sciences (USA) 97:4453-4456.Ahmad, S., A. Selvapandiyan, and R. K. Bhatnagar. 1999. A protein-based phylogenetic tree for Gram-positive bacteria derived from hrcA, a unique heat-shock regulatory gene. International Journal of Systematic Bacteriology 49:1387-1394.Anderson, C. L. 1998. Phylogenetic relationships of the Myxozoa. Pages 341-350 in Evolutionary Relationships among Protozoa (G.H. Coombs, K. Vickerman, M.A. Sleigh, and A. Warren, eds.) Chapman & Hall, London.Anderson, C. L., E. U. Canning, and B. Okamura. 1998. A triploblast origin for Myxozoa? Nature 392:346-347.Andersson, S. G. E., A. Zomorodipour, J. O. Andersson, T. Sicheritz-Ponten, U. C. M. Alsmark, R. M. Podowski, A. K. Naslund, A. S. Eriksson, H. H. Winkler, and C. G. Kurland. 1998. The genome sequence of Rickettsia prowazekii and the origin of mitochondria. Nature 396:133-140.Andersson, S.G. and Kurland, C.G. (1999) Origins of mitochondria and hydrogenosomes. Curr. Opin. Microbiol., 2, 535-541.Aravind, L., R. L. Tatusov, Y. I. Wolf, D. R. Walker, and E. V. Koonin. 1998. Evidence for massive gene exchange between archaeal and bacterial hyperthermophiles. Trends in Genetics 14:442-444.Archibald, J.M. (2005) Jumping genes and shrinking genomes.probing the evolution of eukaryotic photosynthesis with genomics. IUBMB Life, 57, 539-547.Archibald, J.M., Longet, D., Pawlowski, J. and Keeling, P.J. (2002) A novel polyubiquitin structure in Cercozoa and Foraminifera: evidence for a new eukaryotic supergroup. Mol. Biol. Evol., 20, 62-66.Arisue, N., Hasegawa, M., and Hashimoto, T. (2005) Root of the Eukaryota tree as inferred from combined maximum likelihood analyses of multiple molecular sequence data. Molecular Biology and Evolution, 22(3), 409-420.Ayala, F. J., A. Rzhetsky, and F. J. Ayala. 1998. Origin of the metazoan phyla: Molecular clocks confirm paleontological estimates. PProceedings of the National Academy of Sciences (USA) 95:606-611.Baguñà, J., P. Martinez, J. Paps, and M. Riutort. 2008. Back in time: a new systematic proposal for the Bilateria. Philosophical Transactions of the Royal Society Series B 363(1496):1481-1491Baldauf, S. L. (1999) A search for the origins of animals and fungi: Comparing and combining molecular data. American Naturalist, 154(suppl.), S178-S188.Baldauf, S. L., J. D. Palmer, and W. F. Doolittle. 1996. The root of the universal tree and the origin of eukaryotes based on elongation factor phylogeny. Proceedings of the National Academy of Sciences of the United States of America 93:7749-7754.Baldauf, S.L. and Doolittle, W.F. (1997) Origin and evolution of the slime molds (Mycetozoa). Proceedings of the National Academy of Sciences (USA), 94, 12007-12012.Baldauf, S.L. and Palmer, J.D. (1993) Animals and fungi are each other's closest relatives: congruent evidence from multiple proteins. Proc. Natl. Acad. Sci. USA, 90, 11558-11562.Baldauf, S.L., Roger, A.J., Wenk-Siefert, I. and Doolittle, W.F. (2000) A kingdom-level phylogeny of eukaryotes based on combined protein data. Science, 290, 972-977.Balows, A., H.G. Träper, M. Dworkin, W. Harder, and K.-H. Schleifer (eds.). 1992. The Prokaryotes. A Handbook on the Biology of Bacteria: Ecophysiology, Isolation, Identification, Applications. Second edition, Volumes I-IV. Springer Verlag, New York.Bapteste, E., Brinkmann, H., Lee, J., Moore, D., Sensen, C., Gordon, P., Durufle, L., Gaasterland, T., Lopez, P., Muller, M. and Philippe, H. (2002) The analysis of 100 genes supports the grouping of three highly divergent amoebae: Dictyostellium, Entamoeba, and Mastigamoeba. Proc. Natl. Acad. Sci. U S A, 99, 1414-1419.Barns, S. M., C. F. Delwiche, J. D. Palmer, and N. R. Pace. 1996. Perspectives on archaeal diversity, thermophily and monophyly from environmental rRNA sequences. Proceedings of The National Academy of Sciences (U.S.A.) 93:9188-9193.Barns, S. M., R. E. Fundyga, M. W. Jeffries and N. R. Pace. 1994. Remarkable archaeal diversity detected in a Yellowstone National Park hot spring environment. Proceedings of the National Academy of Sciences of the United States of America 91(5): 1609-1613.Bass, D., Moreira, D., Lopez-Garcia, P., Polet, S., Chao, E.E., von der Heyden, S., Pawlowski, J. and Cavalier-Smith, T. (2005) Polyubiquitin insertions and the phylogeny of Cercozoa and Rhizaria. Protist, 156, 149-161.Battistuzzi, F. U. and A. B. Hedges. 2009. A major clade of prokaryotes with ancient adaptations to life on land. Molecular Biology and Evolution 26(2):335-343; doi:10.1093/molbev/msn247Battistuzzi, F. U., A. Feijao, and A. B. Hedges. 2004. A genomic timescale of prokaryote evolution: insights into the origin of methanogenesis, phototrophy, and the colonization of land. BMC Evolutionary Biology 4:44-.Becerra, A., L. Delaye, S. Islas, and A. Lazcano. 2007. The very early stages of biological evolution and the nature of the last common ancestor of the three major cell domains. Annual Review of Ecology, Evolution, and Systematics 38:361-379.Benachenhou, L. N., P. Forterre and B. Labedan. 1993. Evolution of glutamate dehydrogenase genes: Evidence for two paralogous protein families and unusual branching patterns of the archaebacteria in the universal tree of life. Journal Of Molecular Evolution 36(4): 335-346.Benachenhou, L. N., P. Forterre and B. Labedan. 1993. Evolution of glutamate dehydrogenase genes: Evidence for two paralogous protein families and unusual branching patterns of the archaebacteria in the universal tree of life. Journal Of Molecular Evolution 36:335-346.Bern, M. and D. Goldberg. 2005. Automatic selection of representative proteins for bacterial phylogeny. BMC Evolutionary Biology 5:34-.Berney, C. and Pawlowski, J. (2006) A molecular time-scale for eukaryote evolution recalibrated with the continuous microfossil record. Proceedings of the Royal Society Series B, 273(1596), 1867-1872.Boone, D. R., R.W. Castenholz, and G.M. Garrity. 2001. Bergey's Manual of Systematic Bacteriology. Springer, New York.Borchiellini C., Boury-Esnault, N., Vacelet, J., and Le Parco, Y. (1998) Phylogenetic analysis of the Hsp70 sequences reveals the monophyly of metazoa and specific phylogenetic relationships between animals and fungi. Molecular Biology and Evolution, 15, 647-655.Borchiellini, C., M. Manuel, E. Alivon, N. Boury-Esnault, J. Vacelet, and Y. Le Parco. 2001. Sponge paraphyly and the origin of Metazoa. Journal of Evolutionary Biology 14:171-179.Briggs, D. E. G., D. H. Erwin, and F. J. Collier. 1994. The Fossils of the Burgess Shale. Smithsonian Institution Press, Washingthon, D.C.Brinkmann, H. and H. Phillippe. 1999. Archaea sister group of bacteria? Indications from Tree Reconstruction Artifacts from ancient Phylogenies. Molecular Biology and Evolution 16:817-825.Brochier, C., E. Bapteste, D. Moreira, and H. Philippe. 2002. Eubacterial phylogeny based on translational apparatus proteins.Brocks, J. J., G. A. Logan, R. Buick, and R. E. Summons. 1999. Archean molecular fossils and the early rise of eukaryotes. Science 285:1033-1036.Brown, J. R. , C. J. Douady, M. J. Italia, W. E. Marshall, and M. J. Stanhope. 2001. Universal trees based on large combined protein sequence data sets. Nature Genetics 28:281-285.Brown, J. R. 2001. Genomic and phylogenetic perspectives on the evolution of prokaryotes. Systematic Biology 50:497-512.Brown, J. R. and W. F. Doolittle. 1995. Root of the universal tree of life based on ancient aminoacyl-tRNA synthetase gene duplications. Proceedings of the National Academy of Sciences of the United States of America 92:2441-2445.Brown, J. R. and W. F. Doolittle. 1997. Archaea and the prokaryote-to-eukaryote transition. Microbiology and Molecular Biology Reviews 61:456-502.Brusca, R. C. and G. J. Brusca. 2002. Invertebrates. Second Edition. Sinauer Associates, Inc., Sunderland, Massachusetts.Budd, G. E. 2008. The earliest fossil record of the animals and its significance. Philosophical Transactions of the Royal Society Series B 363(1496):1425-1434.Budin, K. and Philippe, H. (1998) New insights into the phylogeny of eukaryotes based on Ciliate Hsp70 sequences. Molecular Biology and Evolution, 15, 943-956.Burki, F. and Pawlowski, J. (2006) Monophyly of Rhizaria and multigene phylogeny of unicellular bikonts. Molecular Biology and Evolution, 23(10), 1922-1930.Burki, F., Shalchian-Tabrizi, K. and Pawlowski, J. (2008) Phylogenomics reveals a new 'megagroup' including most photosynthetic eukaryotes. Biol. Lett., 4(4), 366-369.Burki, F., Shalchian-Tabrizi, K., Minge, M., Skjaeveland, A., Nikolaev, S.I., Jakobsen, K.S. and Pawlowski, J. (2007) Phylogenomics reshuffles the eukaryotic supergroups. PLoS ONE, 2, e790.Bustard, K. and R. S. Gupta. 1997. The sequences of heat shock protein 40 (DnaJ) homologs provide evidence for a close evolutionary relationship between the Deinococcus-Thermus group and cyanobacteria. 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(1998) Evolutionary relationships of Microsporidia. Pages 77-90 in Evolutionary Relationships among Protozoa (G. H. Coombs, K. Vickerman, M .A. Sleigh, and A. Warren, eds.) Chapman & Hall, London.Carroll, S. B., J. K. Grenier, and S. D. Weatherbee. 2001. From DNA to Diversity. Molecular Genetics and the Evolution of Animal Design. Blackwell Science, Malden, Massachusetts.Castro, H. F., N. H. Williams, and A. Ogram. 2000. Phylogeny of sulfate-reducing bacteria. FEMS Microbiology Ecology 31:1-9.Cavalier-Smith, T. (1987) The origin of fungi and pseudofungi. In Rayner, A.D.M., Brasier, C.M. and Moore, D. (eds.), Evolutionary biology of the fungi. Cambridge University Press, Cambridge, pp. 339-353.Cavalier-Smith, T. (1993) Kingdom Protozoa and its 18 phyla. Microbiol. Rev., 57, 953-94.Cavalier-Smith, T. (1998) A revised six-kingdom system of life. Biol. Rev. Camb. Philos. Soc., 73, 203-266.Cavalier-Smith, T. 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What's an explanation of dark matter in details, with very high accuracy?
To fulfill your stated requirements would require (1) a post the length of a book, and (2) a deeper understanding than I personally have. However, given that Quora is not the right place to write a book anyway, I may know enough to take a reasonable crack at this. With that said, though, if you're an actual expert on one of these areas and catch something I've explained incorrectly, please let me know in the comments so that I can fix it!Yes, it's still quite long, but keep in mind that this is the short version.What is Dark Matter (DM)?Dark Matter is just matter that doesn't interact via the Electromagnetic (EM) or Strong Nuclear forces. No EM interactions means that it can't give off light, or absorb light, or reflect, refract, or scatter light in any way. This, naturally, makes it rather difficult to see (thus "dark" matter, although I suppose it's more "transparent" than "dark"). Our current best measurements indicate that something like 85% of the matter in our observable Universe (about a quarter of the total mass-energy content) is Dark Matter.Isn't Dark Matter weird/spooky?Not at all. Neutrinos, for example, satisfy the definition of Dark Matter, they just represent such a tiny fraction of the total DM in the Universe that people tend to neglect them when they ask, "what is Dark Matter made of?"There is nothing at all strange or unusual about certain particles not interacting in certain ways. Neutrons have no electric charge (although they do have EM properties, but that's neither here nor there), and electrons don't interact via the Strong Force, so why shouldn't there be particles that interact with neither, like the neutrinos? Saying that interacting with light is "normal" is purely human bias, because we rely so much on sight. Having lots of DM in the Universe is in no way "weird"; it just means that the Universe doesn't revolve around what humanity finds convenient!Why are we confident that DM exists?This is by no means a complete list, but it should give a sense of the kinds of evidence we have. Each of these would take at least a chapter of a book to explain properly, but hopefully this will give the general idea.Galactic rotation curves.When one object orbits another, the orbiting object has to be constantly accelerating towards the central object (or, more precisely, they both accelerate towards their combined center of mass). Without that acceleration, the orbiting body would just fly off. The faster the orbiting body is moving, the more acceleration is needed to keep it in its orbit. Since in this case the acceleration is due to gravity, this means that the central mass has to be bigger. For a circular orbit of a small object [math]m[/math] at distance [math]r[/math] and velocity [math]v[/math] around a large (and assumed stationary) object [math]M[/math], the acceleration requirement gives[math]\frac{v^2}{r} = \frac{GM}{r^2}[/math]which in turn gives us the relation[math]v = \sqrt{\frac{GM}{r}}[/math].(I'm doing this with Newtonian gravity for simplicity; to do it with full rigor would require General Relativity. In this situation, the Newtonian approximation is actually generally pretty good.)For a more complicated object than just two point particles, as long as there's enough symmetry, the gravitational version of Gauss's law says that the relevant [math]M[/math] is the total mass of everything in the galaxy that's at a distance less than [math]r[/math] from the center. [Edited to note: For this to be exactly right, the matter distribution would have to be spherically symmetric, which galaxies aren't. As a result, actual calculations are a bit more complicated than shown here.]This allows us to "weigh" different parts of the galaxy, by measuring the relationship between [math]r[/math] and [math]v[/math]. (We can measure the rotational velocities by comparing redshifts on the approaching and receding sides of the galaxy.) This image from Wiki shows the result of this measurement:The "expected from visible disk" line is determined by adding up the masses of all the parts of the galaxy that we can see. (How we measure that mass is a whole different discussion.)Gravitational Lensing.In General Relativity, whenever light passes through a gravitational field, that field bends its path slightly. This acts like a Gravitational lens, and can produce, for example, "Einstein Rings", like this image from Wiki:The "ring" is a distorted image of a single blue galaxy located behind the red galaxy at the center. Light from the blue galaxy goes out in all directions, but is bent by the red galaxy's gravity. This means that the light that starting out on a "direct path" to us never signNowes us, but light that was originally missing us by a specific amount (in any direction) gets bent back towards us, which makes it look like it's coming from a bunch of different directions, resulting in the ring image seen here.This is a highly dramatic example of gravitational lensing, but there are much more subtle effects that can still be useful. In Weak gravitational lensing, statistical analysis of distortions in the light we receive allows us to "map out" the gravitational field between us and distant galaxies. Often, this just shows more mass than we know how to account for, but that could be explained away by just assuming that our understanding of gravity is off. There's something else, however, that's a lot harder to explain away in that manner: the Bullet Cluster.(Image from A Matter of Fact on nasa.gov)What's going on here? Well, two galaxy clusters collided with each other, and this is the aftermath. The red coloring represents where the visible matter is, while the blue coloring represents where the dark matter is, as inferred by gravitational lensing. Why are they separated so much? Well, most of the luminous matter in a galaxy cluster is in the Intracluster medium, a hot, dense, plasma. When these plasmas collide with each other, a signNow amount of the matter slows down. However, since Dark Matter interacts only very weakly, the DM components of the two clusters were free to pass through each other unimpeded, resulting in a separation (as seen here). Not only is there "not enough" luminous matter... it's in the wrong place! A small number of scientists remain committed to finding ways to explain this without DM, and they have had partial success, but only by including as-of-yet-unmeasured things that are far stranger than DM (for example, a rank-3 tensor field, which, while possible, would be the first tensor field of such a high rank ever found).Effect on the Cosmic Microwave Background.For the first few hundred thousand years after the Big Bang, The Universe was hot enough that it was highly ionized, which made it more or less opaque to light; photons were pinballing around just like any other particle. However, once things cooled down enough, signNow amounts of the protons and electrons combined into neutral Hydrogen, which is (more or less) transparent to most of the light that was around at the time. This happened fairly quickly (in terms of cosmological time), and so it was as if all of the light pinballing around all over the Universe were suddenly released all at once, effectively capturing a snapshot of the Universe at that moment in its evolution. Since this light was released everywhere in the Universe, we can point our radio telescopes in any direction we like, and there it is: the Cosmic microwave background (CMB). It's almost the same temperature in every direction, but there are small differences (generally around one part in [math]10^5[/math]), and we have measured these tiny variations with extraordinary accuracy: first via the COBE satellite, which was then replaced by the more advanced WMAP, which was then replaced by the more advanced Planck (spacecraft), which is currently in operation.These tiny variations can tell us a lot about the early universe. For example, statistical analyses of these variations show the distinct signature of pressure waves propagating through that early plasma, and the nature of these Baryon acoustic oscillations can tell us a lot about what kinds of things were around. Specifically, the protons and electrons would be dragged along by the (dominant) photons, becoming part of the wave, but Dark Matter wouldn't, and would only be indirectly affected by the resulting small changes in gravity. The presence and abundance of Dark Matter therefore affects how these waves impact the temperature variations in the CMB.The formation of large-scale structure.The standard story given in popular science explanations goes like this: the Universe started out hot and dense and more or less uniform, then it expanded and cooled and clumped into stars and galaxies. However, this story is incomplete, in a way that means that galaxies wouldn't exist without dark matter.At a surface level, the story makes sense; heck, I got almost half-way through a Ph.D. in Physics without noticing any problem with it! It sounds so plausible because of how gravity works: if matter is distributed more or less evenly, but some places are a tiny bit more dense than others, gravity will tend to make those overdensities bigger and bigger. Why? Well, even if a region is just a little denser than its neighbors, it's still going to win the gravitational tug-of-war and gradually accumulate more and more mass. Of course, once it has more mass, it wins the tug-of-war by even more, and so it's a run-away process that ends in big gravitationally-bound clumps.So, what's the problem? Well, consider the air in the room with you right now. Are there tiny density variations? Of course, since perfect uniformity is impossible. But, is it forming into exponentially denser clumps? Certainly not! The reason for this is that, under these kinds of conditions, when the density of a gas goes up, so does its pressure. That pressure makes the over-dense region expand outwards again, returning the density back to average!Now, of course, the scales and temperatures involved are totally different. A huge region of gas will have more gravitational attraction than a tiny pocket of denser air in your room, and gas in space has no need to be at room temperature, either. So, if the gas can cool down enough, that can reduce the pressure enough for gravity to win. But, the more it compresses, the more it heats up, because it's converting gravitational energy into thermal energy, and so the pressure goes up again. This means that forming a galaxy is a very gradual process, during which it has to constantly be getting rid of tremendous amounts of energy. If it were just a cloud of gas, without any outside interference, this process wouldn't be nearly fast enough, and we wouldn't have galaxies today.But, as you know, hot things give off heat much faster than cold things. So, if we want galaxies to form by the present day (or, indeed, before the expansion of space makes matter too dilute to form galaxies at all), something has to be forcing the gas to compress and become denser and hotter than it would be able to under its own gravity. Enter: Dark Matter. Because it interacts only weakly, Dark Matter doesn't have pressure like gas does. So, the argument about the run-away gravitational process actually works for Dark Matter. DM can't get rid of energy very easily, and so conservation of energy and angular momentum mean that it can only collapse to about 200 times the background density, but the resulting Dark matter halo provides enough of a gravity well to "seed" the formation of visible galaxies. So, it's not a coincidence that the galactic rotational curves showed large amounts of dark matter... the galaxies wouldn't have formed there without it!As a result of this DM "seeding" process, theoretical models and computer simulations of the formation of DM structures have been fairly successful in describing the statistical properties of how galaxies are distributed now, as well as how they were distributed earlier in the history of the Universe (which we can measure by looking at very distant galaxies).Okay, so that's why we think Dark Matter exists. But, the next obvious question is... well... what is it? What's it actually made of? What are its properties? Here, we have only very partial knowledge, and multiple different theories, any combination of which could be correct (or, perhaps, none of them). This leads us to:What do we know about the properties of Dark Matter?Again, this is in no way exhaustive, but it should give you a decent idea.It's "cold".This is why the current dominant model of cosmology is called the Lambda-CDM model: "Lambda" ([math]\Lambda[/math]) stands for the Cosmological constant, and "CDM" stands for "Cold Dark Matter".When an astrophysicist describes something as "cold", they generally mean that the associated thermal velocity is much less than the speed of light. By this standard, the air in Death Valley is "cold". But, then again, to cosmologists, galaxies are basically point-particles, so everything's a matter of scale and perspective!So, why does DM need to be "cold"? Well, remember that DM clumping together was integral to the formation of structures like galaxies. However, if DM were very hot (and therefore the particles were moving very fast), this would prevent it from clumping properly. I have explained it in very vague terms, but the effects are actually well-understood mathematically. In fact, it's similar to something that does happen, with photons: Diffusion damping (or "Silk damping"). However, in the case of Dark Matter, the result would be a signNow delay (or even outright prevention) of the formation of galaxies, to the extent that "warm" Dark Matter can be observationally ruled out.Incidentally, this is how we know that it's not all just neutrinos: given what we know about the early Universe, they would be far too hot!It interacts only very weakly.This is somewhat part of the definition of Dark Matter, but it's good to see observational confirmation. I know fewer of the details on this, but I do know that there are observational bounds in the "interaction cross-section" of Dark Matter, both in terms of its interactions with luminous matter and for its theorized self-annihilation processes (in which two DM particles could interact and annihilate each other). Also, as discussed before, the Bullet Cluster shows giant dark matter halos more or less just passing through each other, which suggests very weak interactions.So... given those properties,What might Dark Matter be made of?There are two leading theories (as far as I'm aware) that suggest the existence of specific types of new particles. Both are well-motivated theoretically (as in, we have good reasons for suspecting that particles with those particular properties might exist), but neither has been experimentally confirmed yet. Interestingly, the two predicted particles are totally different from one another, not slight variations on the same theme.At the end of the day, either of these theories could be right, or both (given the existence of neutrinos, there's no need for all the rest of the DM to be a single type of particle), or, of course, neither.So, what are the theories?Axions.I feel morally obliged to put this one first, even though the other one is more popular at the moment, because my university is heavily involved in the Axion Dark Matter Experiment (ADMX), and so of course I'm rooting for my colleagues!The existence of Axions has been theorized since the 1970s, but we only recently have the technology to even properly start to try to measure them in the lab. Axions are extremely tiny particles (unlike WIMPs, the other leading option), and so they would have to exist in truly huge quantities. Still, because they interact so weakly, it's hard to detect them, even with billions of them passing through your detector in a tiny fraction of a second. The linked wiki articles do a better job of explaining the theoretical motivation and experimental search than I could. It's really quite elegant, and would solve a lot of outstanding mysteries in particle physics (like the Strong CP Problem), but I can't do it justice.Weakly Interacting Massive Particles (WIMPs)(Wiki reference: Weakly interacting massive particles)To explain why WIMPs are theoretically attractive, I have to take a little detour into "relic abundance", i.e., how many particles of a given type were left over after the Universe cooled down and generally became a more stable place.In the early universe, everything was very dense, and many different kinds of particles were "tightly coupled" (i.e., they interacted with each other frequently). However, as the universe got larger and cooler, these interaction rates slowed down, more or less to a stop, a phenomenon known as "freezing out". The time at which something "freezes out" depends on a number of things, including its mass and how strongly it interacts with other things. This "freezing out" has a huge effect on the abundances of various particles in the Universe. For example, consider the process[math]n \Leftrightarrow p + e^- + \overline{\nu_e}[/math],in which a neutron can turn into a proton, electron, and electron anti-neutrino (or vice versa). If you go back far enough, this reaction will be in thermodynamic equilibrium, just like with any chemical reaction that can go either direction. However, once the neutrinos "freeze out", equilibrium can't be maintained anymore (although other processes, like beta decay, can still happen). The relative abundance of protons and neutrons at the moment of freeze-out is determined by two factors: the mass difference [math]\Delta m[/math] between the two particles, and the temperature of the Universe when freeze-out occurred. These factors combine to determine by how much the lighter particle is thermodynamically favored, with an exponential dependence:[math] \frac{N_n}{N_p} \propto e^{-\Delta m c^2 / k T}[/math]where [math]k[/math] is Boltzmann's constant.This clearly impacts the "relic abundance" of the particles involved (here, protons and neutrons). So, in general, the abundance of a given particle in the Universe today is signNowly influenced by the mass of that particle and how strongly it interacts (since that affects freeze-out time and thus freeze-out temperature). This brings us to the so-called "WIMP miracle": a particle that interacts predominantly via the Weak Nuclear Force, and that has a mass near the mass scale associated with Weak interactions ([math]\sim 100 \text{ GeV}/c^2[/math]), would have a relic abundance that would match the measured abundance of Dark Matter in the Universe. Given that such a particle was already speculated to exist (in the context of Supersymmetry), this was very theoretically attractive to a lot of people, although our inability to find it so far has damped some of their spirits.So, there you have it: my summary of Dark Matter. Hope it was worth the time it took to read! (Let alone write...)
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How are the girls' hostel facilities at VIT?
I'd lived in around 6 boardings, hostels and PG accommodations by the time I joined VIT. I was mind-blown by the privileges. I lived in a 4 bed non-AC room (I have sinusitis and AC with less moisture in the air gives me a lot of discomfort) and it was incredible!You are given one table, a chair, a night light, a plug point, a pair of shelves and a whole wardrobe. There are two fans and to mirrors in the room.The windows are huge and they provide good air circulation if the door is left slightly ajar.You are provided with space to dry your clothes outside the room. There are washing stones and washing machines available for laundry. There is also laundry service which costs around Rs 150 a month (for extra lazy people).There is filtered water (chilled and normal) available always. There are water heaters provided on some floors for hot drinking water. They will be available either on your floor, or one floor above or below you.There are water heaters in the bathroom areas too on every floor. Both Indian and European toilets are available.Two elevators are present, one for odd floors and the other for even floors. The room is swept and mopped every day.Convenience stores(2), restaurants (2), a salon and a nescafe are present in the hostel campus. A pool, indoor gyms(AC and non AC) and indoor tennis courts are present. Besides these, a badminton court and a basketball court are also available outdoors.Inside, in the F - block courtyard, there are to courts to play.The facilities available are good and even the rules aren't that bad. Hope you have a good stay!
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What is difference between Consulting Services Agreement and Master Services Agreement?
what is difference between Consulting Services Agreement and Master Services Agreement ? When you negotiate services with a client or supplier, the process can take time and culminate in a contract that spells out the obligations and requirements of all signatories. If both parties repeatedly contract for the same service with each other, you might both discover that though negotiations take the same amount of time, most of the terms remain the same. All parties can reduce time and involvement by settling first on a master services agreement.DefinitionsA master services agreement is a contract that spells out most but not all of the terms between the signing parties. Its purpos...
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Do you think cold email is still a good business practice?
Yes, it definitely is. Absolutely.BUT there’s certain etiquette you need to follow to succeed with cold emailing. In other words, cold email now is all about personalization - at scale.And sadly, this is exactly where most businesses fail with cold outsignNow (cold calling+cold emailing). Traditionally, the concept of personalization meant hours of research culminating in a 1:1 email to only the top (1%) leads. Now, with the growing power of data, it has become possible to target accounts at scale with the same level of customization - without hours of time wasted on research.It really does come down to the quality of your data.For my part, I’ve managed a response rate of about 1 in 5 with various cold email templates I’ve experimented with, which really is higher than the usual open and response rates. A major factor in finding success with cold emailing is the data you are working with. Many data providers out there have pre-made lists with numerous pseduo companies and bad data like outdated contact details etc. Also remember that you should build lists on your ideal customer profile.Hence, it is critical to find the right B2B data provider for your business.You should try a provider like Cloudlead - B2B contact data, intent data and sales intelligence for building targeted lists on your ideal customer profile. Benefits of using Cloudlead for lead generation include:replacements on anything above 5% hard bounces95% accurate datasales triggers and intent data for your niche/product or industryHere is a short guide on the 4 Tools for Perfecting Your B2B Sales Funnel - Entrepreneur - very useful readOther B2B data providers include:-Discoveror-Leadenius-Uplead-LeadIQ-Seamless(dot)aiHere is how you should incorporate cold emailing in your lead generation strategy:You can adopt a combination of cold emailing and cold calling. For example, after the 2nd or 3rd email in your drip campaign, you can try calling prospects who’ve opened your email multiple times.1 - First cold email (introduction)2 - Second cold email (follow up)3 - First follow up call4 - Third cold email (reminder+follow up)5 - Second Follow up call6 - Fourth cold email (follow up)7 - Fifth cold email (follow up)8 - Third follow-up call9 - Sixth cold email (reminder +follow up)10 - 7th cold email (break up email)There is a lot of debate in the sales industry regarding the number of emails to maximize each campaign - some suggest up to 8 emails, while others claim that going 10+ yields better results.My advice is: EXPERIMENT. Try different number of emails, content, subject lines, CTAs, delivery times etc to know what works for YOU. here is a resource I wrote containing B2B cold email templates on our website: 5 Cold Email Templates For Generating Warm LeadsOther than this, I would recommend you visit the following sites for some quality cold email templates:-Yesware-hubspot-Woodpecker-Close(dot)ioGood luck!For more tips, you can always visit my Quora profile here: Zobia Zuberi
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