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RIP, Microsoft Paint. MS Paint, the first app you used for editing images, will probably be killed off in future updates of Windows 1. Paint 3. D. Microsoft lists the 3. Windows 1. 0’s next autumn update, a little X marking the end of an era. The app is certainly a relic, from a time when the casual computer user couldn’t crack open Photoshop or Skitch or Pixelmator or thousands of web apps. MS Paint can’t save image components as layers or vectors; it’s for making flat static images only. It doesn’t smooth lines or guess at your best intentions. It does what you tell it and nothing more, faithfully representing the herky- jerky motion of drawing freehand with a computer mouse. It’s from a time before touch, a time before trackpads. As more sophisticated options appeared, Paint’s janky aesthetic became a conscious choice. Paint” became the metonym for that aesthetic, even if an image was actually created in another app. TV Tropes lists major limitations that came to define a certain look: the wobbly freehand lines, awkward color handling, and inappropriate export settings that give Paint its distinctive look. In 2. 01. 4, Gawker’s Sam Biddle noted Paint’s influence on conspiracy theory images, calling the form “Chart Brut.” In amateur detectives’ attempts at identifying the Boston Marathon bombers, the simplicity and jaggedness of Paint evokes the “crazy wall” aesthetic of red string and scribbled notes, apparently without irony. The same year, internet historian Patrick Davison explored Paint’s influence on the last decade of meme culture, particularly Rage Comics. The outsider- art aesthetic feels appropriate to the relatable everyday content, and makes the art form unthreatening. Of course, Paint offered a few features to smooth things out, like the circle and line tools and the “fill” tool, all used in the stoner comics of the early 1. Crucially, those circles still had jagged curves. The bright colors of stoner comics are flat, as MS Paint didn’t support gradients (without an elaborate hack). Contrary to popular opinion, some tweetstorms are good, but reading them on Twitter can be a pain in the ass. Thread Reader reformats a tweetstorm into a readable. Tabtight professional, free when you need it, VPN service. Contrast those pixellated lines with the slick, stylish face from this art tutorial: This slickness is built into Paint’s successor, Paint 3. D. From the moment you start sketching, Paint 3. Citation Machine™ helps students and professionals properly credit the information that they use. Cite sources in APA, MLA, Chicago, Turabian, and Harvard for free. D smooths out your art. It also supports automatic selection tools and content- aware fill to rival Photoshop’s.)By automatically improving art, Paint 3. D hides the process behind the image. Paint’s sloppiness is probably why rage comics got so popular. Looking at a rage comic, you can tell exactly how it was drawn, and how you might draw one yourself. By delivering exactly what the artist draws, MS Paint forms an image that the viewer can mentally reverse- engineer and imitate. Unless you go absolutely nuts with it. Reddit user Toweringhorizon painstakingly assembled the drawing “To a Little Radio” using MS Paint tools like the oil brush, stretching the medium while maintaining a pixelated look. It’s one of the top submissions to MS Paint subreddit, a beautiful collaborative art gallery. Scrolling through this art feels like flipping through the sketchbook of the most artistic kid in high school. There’s an accepted roughness, a desired minimalism. 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My previous article on radio communication was a primer that went into detail about why you’d want to learn about radios, the way they operate and what frequencies are available for you to operate on. Today I’m going to address what kind of radios are out there for you to use with those different frequencies, the advantages to programming your radio, what kind of upgrades are available and even how to create your own comms, or frequency card. I’m going to be referencing quite a bit of information from my last article when it comes to frequencies, so if you’re not up to speed yet on the difference between say, VHF and UHF, check out my first article. What to Look for in a Handheld Radio. First off, my recommendations for radios are going to be primarily based on handheld applications. While there are certainly pros to having a larger base station transceiver, the handhelds have it when it comes to portability, ease of use, versatility and more. They can be used at home, in a vehicle, or even in the field. What’s a Transceiver? A transceiver, which I’ll be referring to frequently in this article, is essentially your radio. A transceiver is a unit which contains both a receiver and a transmitter. While these used to be separate units until the 1. Occasionally you’ll see just a receiver, but this is mostly for shortwave listening and beyond the scope of this article. What Radio to Buy? This is a loaded topic and one that I mentioned I’ll be approaching from a handheld- only angle. I’m also going to keep this as budget conscious as possible, too. Like many of you that enjoy shooting, you’ve probably also amassed quite a collection of holsters, as you try different types out to find what works best for you. Handheld transceivers can be just as bad, but my hope is that with the info I’ll be providing, you’ll avoid amassing a box of radios that you no longer use like I have. Some important considerations when looking at radios, are asking yourself some hard questions ahead of time. What do I want to do with my radio? What frequencies do I have access to and what are my power limits on those frequencies? My last article did a good job of laying out all the different frequencies available to you and which require a license to operate on. If you don’t already know which of the different frequencies you want to operate on, like FRS, GMRS, or MURS, reference that first article I wrote. I hate to keep mentioning that first article, but I know there are some of you that are reading this that may think I’m breezing over important topics and I’m doing that for the sake of those that have the baseline info from that article. Frequency and Power. Addressing each of these questions one at a time will give you a background of what essentials to look for. What you want to do with the radio is important, are you just talking outside within line of sight of another person? FRS radios are great for this application, but if distance is a concern, they’re not for you. FRS transmits and receives on UHF, which by nature doesn’t travel as far as VHF due to UHF’s shorter wavelength. This of course completely discounts obstacles you may encounter, which will decrease range even more. Remember that more power equals better range, so the FCC legal limit of 0. FRS is a real let down, when you can move to VHF and MURS frequencies and bump up to 2 watts of power. Pay your $9. 0 to the FCC for a GMRS license and you can transmit at 5 watts to 5. Have a HAM license? That changes things too. Suffice to say, I’m trying to talk you out of FRS. FRS radio manufacturers like to inflate their range, which I got into on that last article. They make claims that seem to violate the laws of physics and the curvature of the earth. What I mean by FRS radios, are the two packs of walkie- talkie looking transceivers you commonly find at Wal- Mart and sporting goods stores. What you’re looking for in a good handheld is as much wattage as you can buy, while keeping in mind the legal limits you can operate on within your chosen frequencies. The frequency range the transceiver operates on is also very important. Obviously if your intent is programming MURS frequencies into your handheld, a handheld set up for CB with an operating range only in the High Frequency 2. MHz range, isn’t going to work with MURS and its 1. MHz range. The radios I’ll be recommend in this article are going to speak directly to versatility and can handle MURS, GMRS, NWR (Weather) and some HAM frequencies. Typically, you’re only going to find a 5 watt max on handhelds, but what’s also important is ensuring they have different settings for power. Meaning that they have the ability to switch between a low power setting and a high power setting. This will ensure you have a handheld that can function well for GMRS and HAM wattage, but can also dial down for operating on MURS frequencies and not violate any FCC laws. A good example of this is the Wouxun KG- UV5. D radios we have here at ITS. They feature a selectable 1. W low and 5. W high setting for VHF and a 1. W low and 5. W high for UHF. By setting them to the low wattage setting, they’re able to be used with the FCC MURS requirement of not exceeding 2 watts of transmit power, yet with a programming change, they can be boosted to the high setting for GMRS or HAM frequencies at 5 watts. GMRS and HAM is obviously limited to licensed individuals only. More on those licenses and certifications here. While I could link to the KG- UV5. D, the KG- UV6. D is the newest version and is what I’d recommend if you’re buying one new. Dual Band and More. Having a dual band monitor feature on your handheld can be quite helpful. This feature will allow you to monitor two different frequencies at once. These can be VHF/VHF, VHF/UHF and even UHF/UHF. This might be hard to understand, so I’ll put it in the perspective of how we’ve used dual band before. During our recent ITS Muster, we assigned a radio to each of our squads and they had a designated main frequency to talk to the ITS staff on. The staff also had a frequency that we’d use to talk to each other on that the attendees didn’t have programmed into their radios. So we’d “monitor” both of these frequencies simultaneously with the dual band function of our radio transceivers and were easily able to select the specific frequency we wanted to transmit back on. So in theory if the main frequency was channel 1 and our inner- staff channel was channel 2, we’d just have to make sure we were transmitting on channel 2 if we didn’t want the attendees to hear our conversation. One more thing about dual band is that you want to ensure your antenna can support dual band as well. If you’re buying a radio with dual band built- in, the antenna that comes with the radio will more than likely support it, it’s aftermarket antennas you have to worry about. Another important thing to look for in a radio transceiver its the ability to program it manually, as well as with programming software using a cable. More on programming in the next section. What I mean by programmed manually is that it has a keypad, a digital display and that all menu options can be set with that keypad and display. The display also provides visual feedback on what channel/frequency you’re operating on. A few other considerations are as follows: Does the transceiver have a memory bank to store your favorite frequencies? What’s the battery type? Is it rechargeable? Is a charger included? Is there an external mic/push- to- talk connection? 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The Symposium’s main objectives were to bring together scientists working in different areas of the study of the origin and early evolution of life, to stimulate discussion on this fundamental process and to have an appraisal of the most recent advances in this multidisciplinary field that combines research from space sciences and astrophysics, to chemistry, geology, paleontology, genomics, molecular biology, history and philosophy of science, among others. The meeting was attended by about 3. This volume collects almost all the contributions, which are an up- to- date account of the state of the knowledge on this exciting area of scientific and educational pursuits. It is with great pleasure that I acknowledge the contributions of different authors in assuring the prompt publication of the OLEB Special Issue. I would also like to express my thanks to the Editor of OLEB, Alan W. Schwartz, and Springer for the publication of the Proceedings. Enzo Gallori. University of Florence. President of the Local Organizing Committee. Invited Lectures. Search for Potentially Primordial Genetic Systems. Thirty years after the seminal contribution by Warshel and Levitt, we review the state of the art of combined quantum-mechanics/molecular-mechanics (QM/MM) methods. Adjuvants such as surfactants improve pesticide efficiency by multiple mechanisms. In particular surfactants increase the foliar uptake of herbicides, growth. Ramanarayanan Krishnamurthy. The Department of Chemistry at The Scripps Research Institute 1. North Torrey Pines Road, MB1. La Jolla, CA- 9. 20. USAExtensive base- pairing studies of oligonucleotides consisting of canonical bases tagged to a variety of cyclic sugar- phosphate backbones—conducted in the context of work toward an etiology of the structure type of the natural nucleic acids—have led to a broadening of the scope of investigations to include informational oligomer systems that are not confined to typical sugar- backbones and canonical bases. The lecture will present some recent results: the base- pairing properties of a series of acyclic backbone derived oligomeric systems tagged with alternative heterocycles as recognition elements. E- mail: rkrishna@scripps. The Formation of Planetary Systems. Alan P. Boss. Carnegie Institution, Washington DC, USAPlanetary systems form out of the leftovers of the star formation process. Dense interstellar clouds of gas and dust collapse under their self- gravity to form central protostars orbited by rotationally supported, flattened disks in which planets later form. The disk that formed the Solar System is called the solar nebula. Terrestrial planets form by the slow process of collisions and sticking between increasingly larger dust grains, pebbles, boulders, and mountains of rock and ice termed planetesimals. Km- size planetesimals are large enough to grow by gravitationally deflecting bodies that might otherwise not collide with them, leading to a period of runaway growth to lunar- sized planetary embryos. The final phase of terrestrial planet formation involves giant impacts between the protoplanets and planetary embryos and requires on the order of 1. While there is a general consensus about the formation of terrestrial planets, two very different mechanisms have been proposed for the formation of the gas and ice giant planets. The conventional explanation for the formation of gas giant planets, core accretion, presumes that a gaseous envelope collapses upon a roughly ten Earth- mass, solid core of rock and ice that was formed by the collisional accumulation of planetary embryos orbiting in the solar nebula. The more radical explanation, disk instability, hypothesizes that the gaseous portion of the nebula underwent a gravitational instability, leading directly to the formation of self- gravitating clumps, within which dust grains coagulated and settled to form cores. Core accretion appears to require several million years or more to form a gas giant planet, implying that only relatively long- lived disks would form gas giants. Disk instability, on the other hand, is so rapid (forming clumps in thousands of years), that gas giants could form in even the shortest- lived disks. Terrestrial planets seem to be likely to form under either scenario for giant planet formation, though the likelihood does depend strongly on the orbital properties of the giant planets in the system. Core accretion has difficulty in explaining the formation of the ice giant planets, unless two extra protoplanets are formed in the gas giant planet region and thereafter migrate outward. An alternative mechanism for ice giant planet formation has been proposed, based on observations of protoplanetary disks in the Orion nebula cluster and Eta Carina star- forming region: disk instability leading to the formation of four gas giant protoplanets with cores, followed by photoevaporation of the disk and gaseous envelopes of the protoplanets outside about 1. AU by ultraviolet radiation from nearby massive stars, producing ice giants. In this scenario, Jupiter survives unscathed, while Saturn is a transitional planet. The ultraviolet fluxes photoevaporate the outer disk, freezing the orbits of the giant planets, and converting the outer gas giants into ice giants. Because most stars form in regions of high- mass star formation, if this alternative scenario is appropriate for the formation of the Solar System, extrasolar planetary systems similar to our own may then be commonplace. This heretical idea also offers a head start on the formation of prebiotic molecules necessary for the origin of life, as well as a natural explanation for thermally processing primitive materials (chondrules and refractory inclusions) found in meteorites, large scale radial transport of refractories and ices, mixing and homogenization of initially heterogeneous short- lived radioactivities, and transport of stable oxygen isotopes inward from the outer disk surface, as required by cosmochemical constraints on the formation of the Solar System. E- mail: boss@dtm. Gas- Phase Prebiotic Chemistry in the Solar System: How and Where. Nadia Balucani. Dipartimento di Chimica, Università degli Studi di Perugia, Perugia, Italy. In the sequence of steps which are believed to have led from elementary particles to the emergence of life, an important one is certainly the formation of simple prebiotic molecules from parent species abundant in the Universe. The aggregation of H, O, N, C (and other element) atoms into molecules and the subsequent chemical evolution are occurring also now in the Universe, as witnessed by the identification of more than one hundred molecules in the interstellar medium (encompassing also prebiotic molecules such as glycolaldehyde, formamide and, tentatively, glycine) and by the gas- phase chemical evolution of the atmospheres of several solar objects like Titan. Simple as they might seem compared to other processes of relevance in astrobiology, the formation mechanisms of many of the observed gaseous prebiotic molecules and radicals are far from being understood. In this contribution, the focus will be on the gas- phase chemical evolution of planetary atmospheres and cometary comae, the gaseous environments of our Solar System where gaseous organic molecules have been observed. Similarly to the atmosphere of Earth, the atmospheres of the other planets (or satellites, like Titan) can be described as giant photo- reactors, where the energy deposited mainly by solar photons, but also by cosmic rays and other energetic particles, drives a complex gas- phase chemistry. In this specific context, gas- phase neutral–neutral reactions are expected to play a dominant role. |
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