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 “A Comprehensive Guide to Perpetual Futures Contracts in Cryptocurrency” 

 This article, delves into the world of perpetual futures contracts (or ‘perps’) in cryptocurrency. These are derivatives that enable traders to speculate on the future price of cryptocurrencies without an expiration date.

 Crypto Derivatives Explained: These financial tools are based on the value of underlying cryptocurrencies. They allow traders to gain exposure to crypto prices without owning the actual tokens.

 Futures vs. Perpetual Futures: Traditional futures contracts involve an agreement to buy or sell crypto at a set price in the future. Perpetual futures, however, don’t have an expiration date, allowing positions to be held indefinitely.

 Funding Mechanisms: Perpetual futures use a funding system to align their prices with the spot market price of the underlying asset. This ensures that the futures trade close to the real-time price of the crypto.

 Leverage Opportunities and Risks: These contracts offer leverage, meaning traders can open larger positions than their capital would normally allow. However, this also amplifies potential losses and risks, including liquidation.

 Risk Management: Perpetual futures are key for hedging risks in cryptocurrency holdings. They allow traders to lock in prices, potentially offsetting losses in the volatile crypto market.

 Final Thoughts: While perpetual futures offer attractive leverage opportunities, they come with significant risks. Traders should be cautious and well-informed to avoid substantial losses. The article emphasizes the importance of understanding these instruments thoroughly before engaging in trading.

Mastering Perpetual Futures in Cryptocurrency: An Essential Guide

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Base very cool blockchain it is evolving very fast. I would also like to see a native coin on the network sooner 

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Nos últimos anos, a tecnologia de blockchain evoluiu além de sua aplicação inicial como um mecanismo para criptomoedas, transformando-se em uma plataforma robusta para uma variedade de aplicações descentralizadas. Entre as diversas inovações neste espaço, a rede BASE se destaca como uma solução inovadora projetada para otimizar a performance e escalabilidade de aplicações descentralizadas. Este artigo explora a arquitetura, funcionalidades e potenciais aplicações da rede BASE no ecossistema de blockchain.

A rede BASE é uma infraestrutura de blockchain que visa superar alguns dos desafios enfrentados por plataformas mais antigas, como o Ethereum. Uma das principais características da BASE é sua arquitetura única que permite uma maior escalabilidade e eficiência operacional. Ela utiliza uma abordagem de camadas que separa o processamento de transações do armazenamento de dados, o que permite uma maior flexibilidade e rapidez nas operações.

A rede também implementa mecanismos de consenso inovadores que são mais eficientes que o tradicional Proof of Work (PoW) ou mesmo o Proof of Stake (PoS), contribuindo para uma maior rapidez nas transações e redução no consumo de energia.

Uma das funcionalidades-chave da rede BASE é sua capacidade de suportar contratos inteligentes complexos e outras operações descentralizadas com maior eficiência. Graças ao seu design otimizado, a BASE pode processar um número significativamente maior de transações por segundo em comparação com redes mais antigas.

Além disso, a BASE oferece um ambiente altamente seguro para o desenvolvimento de aplicações descentralizadas (dApps), incorporando as mais recentes técnicas de segurança cibernética e criptografia para proteger contra ataques e vulnerabilidades.

As potenciais aplicações da rede BASE são vastas e variadas, abrangendo diversos setores. No setor financeiro, por exemplo, a BASE pode facilitar a criação de plataformas de financiamento descentralizado (DeFi) mais rápidas e seguras. No campo dos jogos digitais, a rede pode permitir a criação de jogos completamente descentralizados com economias internas baseadas em blockchain.

Outra aplicação promissora está na área de identidade digital e gestão de dados pessoais, onde a BASE pode oferecer soluções que respeitam a privacidade do usuário, enquanto fornecem a segurança e a imutabilidade proporcionadas pelo blockchain.

A rede BASE representa um avanço significativo na tecnologia de blockchain, oferecendo melhorias substanciais em termos de escalabilidade, segurança e eficiência. Com sua arquitetura inovadora e funcionalidades robustas, a BASE está bem posicionada para ser uma plataforma líder para o desenvolvimento de aplicações descentralizadas em diversos setores. Conforme mais desenvolvedores e empresas começam a explorar suas capacidades, é provável que vejamos uma expansão significativa no uso de tecnologias descentralizadas, impulsionadas pelas soluções que a rede BASE pode oferecer.

BASE: Uma Nova Abordagem na Infraestrutura de Blockchain para Aplicações Descentralizadas

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我国海洋面积辽阔，海岸线漫长，不仅拥有丰富的海洋资源，更是重要战略屏障，事关国家主权、安全、发展利益。一个时期以来，境外间谍情报机关采取各种手段加强对我国海域的侦察监控，开展了一系列情报搜集和技术窃密活动。4月15日，国家安全机关推出的《创新引领·国安砺剑》“十大公民举报案例”专题展播中，就公布了一起渔民老杨捕获海上窃密装置的典型案例。

国家安全机关经工作发现和群众举报，陆续在我国海域发现多种类型的“海洋间谍”，这些特殊技术装置隐藏在茫茫大海中，时刻窥探我海洋信息数据，威胁我国家安全。

这些“海洋间谍”功能各异，作用不同，但都有一个共同的目的，就是服务于境外间谍情报机关的非法活动，危害我国家安全。它们有的充当“暗哨”，长期潜伏于海底，隐蔽采集周围海洋水文信息及各类舰船活动数据，服务战场环境预置；有的充当“密探”，随波漂流沉浮，侦测掌握海域实时情况；有的充当水下“灯塔”，为侵入我国海域航行的他国潜艇指示方向，妄图隐匿行踪。

国家安全机关结合工作掌握情况，发现“海洋间谍”具有以下特点：

——技术性能先进。这些装置均为专门研发制造，大多采用最新科学技术成果，有的可长期自动工作，有的可远程遥控指挥，还有的既能“单兵作战”也可组网部署，能够隐蔽高效完成各种海洋探测任务。

——功能复杂强大。这些装置功能多样，在实现敏感数据动态感知、探测采集的同时，还具备数据的存储、分析、传输等功能。多数装置还具有自毁功能，可根据事先设定程序在完成任务后自动销毁。

——设备高度集成。这些装置内部空间有限，但通过精细化设计，完成了众多功能装置的高度集成，使其在方便使用的同时，能够适应海洋复杂、恶劣的环境，功能稳定而不易损坏。

——及时报告。第一时间拨打国家安全机关举报受理电话12339，提供有关线索和情况，并在国家安全机关指导下开展有关工作。

——稳妥打捞。在确保人身安全的前提下，对可疑装置进行打捞，并保证安全稳妥放置，待返港后及时上交国家安全机关。

——积极配合。学习掌握相关国家安全知识和防范海上安全风险技能，积极配合国家安全机关工作，不断提升识别境外窃密装置和维护国家安全的能力。

维护国家安全不仅需要国家安全机关发挥专门机关作用，更需要人民群众广泛参与、配合支持。如发现相关可疑情况，可通过12339国家安全机关举报受理电话、网络举报平台（

)、国家安全部微信公众号举报受理渠道或者直接向当地国家安全机关进行举报，配合协助开展调查取证。依据《公民举报危害国家安全行为奖励办法》，国家安全机关将根据公民举报线索发挥作用情况，给予相应精神和物质奖励。

渔民捕获海上窃密装置，国家安全机关公布“海洋间谍”画面

Josh Habka

Josh Habka is an analog astronaut, science communicator, biohacker, and CEO of Astrochain.

Rocky planets can be formed through two radically different processes, but it is unclear which built our Solar System’s landmasses. In our solar system, the rocky planets formed at the warmest interior part of the protoplanetary disk, whereas the gas giants formed farther out. Inner planets are far smaller than outer ones. As such, they have a relatively lower gravitational pull, unable to draw a lot of gas into an interior planet’s atmosphere.

The inner protoplanets’ rocky cores also include gases that are present in their environments. Still, unlike the inner planets, because of solar radiation effects and their greater distance from the Sun (Figure 1b), the outer planets did not lose the gases they acquired. This contrasts with the outer, giant planets, which have a primordial atmosphere; a primordial atmosphere is captured directly from the primordial solar nebula. While the rocky planets possess secondary atmospheres produced by outside factors, gas giants only possess the primary atmospheres created by the solar nebula.

As for gaseous planets, astronomers think gaseous planets are formed similarly to rocky planets, however, because they have very large cores (about 10 times that of the mass of the Earth), they take up hydrogen and helium from an initial cloud of gas. The gas giants were completely formed several million years after the start of the planet’s formation, as the planet-forming discs from the sun were dissolved (preventing the later formation of the gaseous planets). We believe the planets underwent the final gas-disk dissipation-driven impact of a giant, resulting in the moon’s formation.

It is possible that when Jovian proplanets broke up, smaller particles from the surrounding disk formed into some of the Moons now orbiting the individual outer planets. Even larger particles would have condensed under gravity to create planetesimals, which would have hit each other to form the solid inner planets.

The shapes made sense because individual outer planets had many moons and rings that orbited on the same plane, much as planets in our Solar System orbit the sun on the same plane. To make that work, a planet might simply form out of a loop of planetesimals starting somewhere in the middle between Venus’s orbit and the orbit of the Earth. Solar systems can form out of three rings of planetesimals: the inner rings of which contain some Earth masses in the rocky planetesimals, which would grow rocky planets, a second with 50–100 Earth masses, which would grow the cores of the giant planets, and the outer rings with the icy planetesimals, which would form comets and Kuiper Belts.

It is important to note that our Solar System’s terrestrial planets are composed of two distinct groups; the four planets closest to the Sun are rocky terrestrial planets, while the four farthest from the Sun are Jovians. The inner planets of Mercury, Venus, Earth, and Mars The outer planets are called the terrestrial planets because the inner planet of Mercury has a compact, rocky surface. The outer planets Venus and Mars, formed by the collision between smaller grains of dust and larger grains of the Solar Nebula, have formed larger grains over millions of years.

Researchers said that planetary embryos may have hit gigantic impacts in 30 to 100 million years to form the rocky planets and moons present in today’s Solar System. New research suggests that clumps of tiny, glassy particles could have been responsible for forming giant asteroids and planetary embryos that hit each other to form rocky planets such as Earth. Scientists are investigating how small groups of materials may have contributed to planet formation.

Current theories about planet formation describe worlds growing out of tiny seeds of rock and ice plants within the swirling discs of gas and dust surrounding newborn stars. According to one part of the science classroom, planets and stars would form out of pieces of dust originating in the Sun about 4.6 billion years ago. Planets are formed by either collision between embryonic planets in the inner Solar System or from the accretion of millimeter-sized pebbles displayed by the Sun outwards.

The buildup of materials to form planets this way is called accretion. The accretion process means the material is collected over time, layer by layer, to form a solid planet. Over time, those masses build up to planets in an accretion process, which means growth through gradually adding layers of matter.

When you add iron, nickel, oxygen, carbon, and other elements that form rocks, you will see enough matter in the Sun to form thousands of rocky planets. On Earth, we see the core of our planet, which has a middle mantle layer and a rocky crust. A silicic planet A solid planet, such as Venus, Earth, or Mars, is composed mostly of silicon-based, rocky mantles with metallic (iron) cores.

Mercury, the planet in the Solar System, has a metal core that is 60%-70% of the mass of the planet, sometimes called an iron planet, although its surface is made of silicates, which are poor in iron. Iron planets are thought to form in high-temperature regions near the star, such as Mercury, and if the protoplanetary disc is iron-rich. In fact, earlier studies showed that gas giant planets preferentially form around iron-rich stars.

Work by a team including Johanna Teske has shown that smaller, rocky planets, like our sun, do not preferentially form around stars that are abundant in metal elements like iron and silicon. A team including Johanna Teske found that stars with Earth-sized rocky planets are generally similar in their chemistry to stars with planets the size of Neptune and stars without planets, but not to stars with gas giant planets. In new research, the team showed that Earth and Mars are overwhelmingly composed of planetary bodies that have been accreted from the inner Solar System, including materials from the innermost disk not sampled by meteorites, and only a small fraction of a planet’s mass comes from bodies in the outer Solar System.

Planetary formation by a gas-and-dust disk surrounding a new star, as described above, has also raised the question of whether this process in and of itself exhausts stars for elements concentrated in the planets.

The heat given off by inner planets means only materials with higher melting temperatures, like metals and rocks, are likely to survive. If all the moons were formed simultaneously with the iron core (as is believed for the Earth), and the two Innermost Planets have no moons, they should also contain no iron core. Considered as such since a gaseous planet could be considered as one formed from solid, rock-like material, like Earth.

Note that the geologic timescale is in hundreds to millions of years, while rocky planets are formed in billions of years, allowing a process of differentiation to create structures that we see on rocky planets.

Mastering Perpetual Futures in Cryptocurrency: An Essential Guide

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渔民捕获海上窃密装置，国家安全机关公布“海洋间谍”画面

How Do Terrestrial Planets Form?

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