Sun
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The document summarizes key facts about the Sun:
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The document discusses principles of electromagnetic radiation relevant to remote sensing. It describes how energy from the sun interacts with the atmosphere and earth's surface before being detected by sensors. The energy can be described using wave or particle models. As a wave, it has properties like wavelength and frequency. As particles called photons, it has energy levels defined by Planck's constant. The sun's energy comes from nuclear fusion and is emitted as blackbody radiation. Its spectrum and intensity are influenced by absorption, scattering, and transmission processes in the atmosphere.
In and out of sun
The Sun is a typical star composed of gas held together by gravity that produces energy through nuclear fusion. It is around 5 billion years old and will become a red giant in approximately 10 billion years, expanding and consuming the inner planets. The Sun emits electromagnetic radiation across all wavelengths, with visible light making up 40% of its output. Its internal structure can be studied through helioseismology, which observes oscillations on its surface to learn about conditions in its interior.
Properties of the sun
The document provides an introduction to stars, focusing on the sun. It discusses the layers of the sun's atmosphere and interior. The sun's core generates its enormous energy output through nuclear fusion. The solar wind consists of high-energy particles escaping the sun's gravity. The sun emits across the electromagnetic spectrum, including x-rays studied by orbital telescopes. The sun's total luminosity is calculated based on the energy received by a detector at Earth's distance. Sunspots occur in pairs of opposite magnetic fields and vary in a roughly 11-year solar cycle.
Solar exploration
This document provides an overview of solar exploration. It summarizes that the sun is a normal star that is made up mostly of hydrogen and helium. It discusses the sun's structure, temperature, magnetic field, and 11-year solar cycle. The document also describes various solar phenomena observed at different wavelengths, such as sunspots, flares, prominences, and coronal mass ejections, as well as their potential effects on Earth. It briefly mentions some open questions in the field and lists some past and present space missions that observe the sun.
sun properties.ppt
The Sun is a glowing ball of gas held together by gravity that is powered by nuclear fusion. It has a diameter of 1.392 million km and is made up primarily of hydrogen and helium. Nuclear fusion in the core converts hydrogen to helium, releasing enormous amounts of energy over billions of years. Features on the Sun include sunspots, solar flares, and prominences, which can impact Earth.
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student presentation
Temperature of the Earth
General Physics 1
Presentation 1 group 2
24 Jan 2009
trimester 2, 2008-2009
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The Sun is the largest object in the solar system, containing approximately 98% of the total solar system mass. It is a yellow dwarf main sequence star composed primarily of hydrogen (71%) and helium (27%). The Sun's immense mass and high temperatures at its core (15-25 million degrees Celsius) enable nuclear fusion, converting hydrogen to helium and releasing enormous amounts of energy in the process.
Astronomy - State of the Art - Stars
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Solar and wind students lecture notes with exercises
The document discusses solar energy and its applications. It begins by explaining how nuclear fusion in the sun's core converts hydrogen to helium, releasing energy in the process. It then describes the structure of the sun and how solar radiation reaches Earth's surface and atmosphere. Applications of solar energy include heating and cooling buildings, generating electricity via photovoltaic cells, water pumping, and more. Solar collectors are also discussed as a means of capturing solar thermal energy.
The Sun Activity and Genesis of Energy
The document discusses the sun and its activity. It begins by providing data on the sun such as its radius, mass, temperature, and composition. It then describes the interior structure of the sun including its core, radiation zone, and convection zone. It discusses how nuclear fusion in the core produces energy and how that energy is transmitted outward. The document also covers sunspots and other active regions on the sun's surface that can influence conditions on Earth.
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EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
Authoring a personal GPT for your research and practice: How we created the Q...
Thematic analysis in qualitative research is a time-consuming and systematic task, typically done using teams. Team members must ground their activities on common understandings of the major concepts underlying the thematic analysis, and define criteria for its development. However, conceptual misunderstandings, equivocations, and lack of adherence to criteria are challenges to the quality and speed of this process. Given the distributed and uncertain nature of this process, we wondered if the tasks in thematic analysis could be supported by readily available artificial intelligence chatbots. Our early efforts point to potential benefits: not just saving time in the coding process but better adherence to criteria and grounding, by increasing triangulation between humans and artificial intelligence. This tutorial will provide a description and demonstration of the process we followed, as two academic researchers, to develop a custom ChatGPT to assist with qualitative coding in the thematic data analysis process of immersive learning accounts in a survey of the academic literature: QUAL-E Immersive Learning Thematic Analysis Helper. In the hands-on time, participants will try out QUAL-E and develop their ideas for their own qualitative coding ChatGPT. Participants that have the paid ChatGPT Plus subscription can create a draft of their assistants. The organizers will provide course materials and slide deck that participants will be able to utilize to continue development of their custom GPT. The paid subscription to ChatGPT Plus is not required to participate in this workshop, just for trying out personal GPTs during it.
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hematic appreciation test is a psychological assessment tool used to measure an individual's appreciation and understanding of specific themes or topics. This test helps to evaluate an individual's ability to connect different ideas and concepts within a given theme, as well as their overall comprehension and interpretation skills. The results of the test can provide valuable insights into an individual's cognitive abilities, creativity, and critical thinking skillsDeep Software Variability and Frictionless Reproducibility
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The ability to recreate computational results with minimal effort and actionable metrics provides a solid foundation for scientific research and software development. When people can replicate an analysis at the touch of a button using open-source software, open data, and methods to assess and compare proposals, it significantly eases verification of results, engagement with a diverse range of contributors, and progress. However, we have yet to fully achieve this; there are still many sociotechnical frictions.
Inspired by David Donoho's vision, this talk aims to revisit the three crucial pillars of frictionless reproducibility (data sharing, code sharing, and competitive challenges) with the perspective of deep software variability.
Our observation is that multiple layers — hardware, operating systems, third-party libraries, software versions, input data, compile-time options, and parameters — are subject to variability that exacerbates frictions but is also essential for achieving robust, generalizable results and fostering innovation. I will first review the literature, providing evidence of how the complex variability interactions across these layers affect qualitative and quantitative software properties, thereby complicating the reproduction and replication of scientific studies in various fields.
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Exposé invité Journées Nationales du GDR GPL 2024
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The pygmy halfbeak Dermogenys colletei, is known for its viviparous nature, this presents an intriguing case of relatively low fecundity, raising questions about potential compensatory reproductive strategies employed by this species. Our study delves into the examination of fecundity and the Gonadosomatic Index (GSI) in the Pygmy Halfbeak, D. colletei (Meisner, 2001), an intriguing viviparous fish indigenous to Sarawak, Borneo. We hypothesize that the Pygmy halfbeak, D. colletei, may exhibit unique reproductive adaptations to offset its low fecundity, thus enhancing its survival and fitness. To address this, we conducted a comprehensive study utilizing 28 mature female specimens of D. colletei, carefully measuring fecundity and GSI to shed light on the reproductive adaptations of this species. Our findings reveal that D. colletei indeed exhibits low fecundity, with a mean of 16.76 ± 2.01, and a mean GSI of 12.83 ± 1.27, providing crucial insights into the reproductive mechanisms at play in this species. These results underscore the existence of unique reproductive strategies in D. colletei, enabling its adaptation and persistence in Borneo's diverse aquatic ecosystems, and call for further ecological research to elucidate these mechanisms. This study lends to a better understanding of viviparous fish in Borneo and contributes to the broader field of aquatic ecology, enhancing our knowledge of species adaptations to unique ecological challenges.
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原版纸张【微信：741003700 】【(carleton毕业证书)卡尔顿大学毕业证】【微信：741003700 】学位证，留信认证（真实可查，永久存档）offer、雅思、外壳等材料/诚信可靠,可直接看成品样本，帮您解决无法毕业带来的各种难题！外壳，原版制作，诚信可靠，可直接看成品样本。行业标杆！精益求精，诚心合作，真诚制作！多年品质 ,按需精细制作，24小时接单,全套进口原装设备。十五年致力于帮助留学生解决难题，包您满意。
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1:该专业认证可证明留学生真实身份
2:同时对留学生所学专业登记给予评定
3:国家专业人才认证中心颁发入库证书
4:这个认证书并且可以归档倒地方
5:凡事获得留信网入网的信息将会逐步更新到个人身份内，将在公安局网内查询个人身份证信息后，同步读取人才网入库信息
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7:个人信誉贷款加10分
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mô tả các thí nghiệm về đánh giá tác động dòng khí hóa sau đốt
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Sun
- 1. Go to http://uslargestsafelist.com/s.php?unknownresponse for $5 free dollars!
- 2. 1. The Sun is an ordinary middle-sized star 2. The sun creates energy by nuclear fusion in its core 3. The visible surface of the Sun is called the photosphere 4. A thin cool layer, the chromosphere, allows us to determine what the sun is made of 5. A very thin but very hot outer layer is called the corona 6. Convection in the sun is revealed by granulation 7. Features on the sun include sunspots, prominences, spicules and faculae 8. Disturbances on the sun affect electrical and electronic equipment on Earth
- 3. Distance: 150 million km (93 million miles) = 8.3 light minutes Diameter: 1.4 million km (870,000 miles) = 109 x Earth Mass = 330,000 x Earth Bulk density = 1.4 gm/cc Surface temperature = 5800 K Rotation: 25 days at equator, 34 at poles 1. The Sun is an ordinary middle-sized star
- 4. Ideal Gas Law: Pressure x Volume is proportional to Temperature Pressure = weight of overlying material 2. The sun creates energy by nuclear fusion in its core
- 5. % of Radius Temperature K Pressure (Atm) Density (gm/cc) % of Mass 100 5700 .07 2 x 10-7 100% 90 600,000 2,130,000 0.026 99.8% 80 1,360,000 17,000,000 0.09 99% 70 2,300,000 66,000,000 0.2 97% 60 3,100,000 210,000,000 0.56 94% 50 4,000,000 720,000,000 1.3 89% 40 5,100,000 2.7 billion 3.9 79% 30 6,800,000 11 billion 12 61% 20 9,370,000 43 billion 35 33% 10 13,100,000 130 billion 87 7.7% 0 15,700,000 230 billion 154 0%
- 6. Core: 0-20% of radius. Energy produced by nuclear fusion Radiative Zone: 20-70% of radius: Energy travels as thermal radiation Tachocline: Boundary of Radiative Zone: Exterior slips over interior Convective Zone: Outer 30% of Sun: Energy moves by convection 2. The sun creates energy by nuclear fusion in its core
- 7. Energy output: 90 billion megatons/second Energy output = 6 microwatts/kg – less than a candle Human body outputs 1.2 W/kg – 200,000 times greater By volume: Core of Sun = 0.9 W/m3 ; Human body = 1200 W/m3 . Trying to duplicate sun’s energy output not practical on Earth; We try to use other fusion processes Energy takes 10,000 – 100,000 years to reach surface 2. The sun creates energy by nuclear fusion in its core
- 8. 4 H He 4H = 4 x 1.00794 = 4.03176 He = 4.002602 Difference = 0.029158 = 0.7% = 1/140 Converted to energy via E=mc2 Once you get over being freaked out by Einstein, this is middle school math 2. The sun creates energy by nuclear fusion in its core
- 9. E=mc2 m = kg c = m/sec = 300,000,000 E = joules (one Watt = 1 J/sec) Sun’s energy output = 3.8 x 1026 W How much mass is that per second? m = E/c2 = 3.8 x 1026 /(300,000,000)2 = 4 billion kg/sec 2. The sun creates energy by nuclear fusion in its core
- 10. Sun converts 4 billion kg of matter to energy every second Matter conversion = 1/140 of original mass Sun converts 560 billion kg of H to He (5.6 x 1011 kg) every second Mass of Sun: 2 x 1030 kg 2 x 1030 kg/ 5.6 x 1011 kg/sec = 3.6 x 1018 sec = 114 billion years 2. The sun creates energy by nuclear fusion in its core
- 12. Photosphere: The Visible Disk More transparent than air We can see a couple of hundred kilometers deep Chromosphere Thin cooler atmosphere How we know what stars are made of Corona Very thin but very hot Why so hot is a mystery
- 14. Limb Darkening Granulation Sunspots Faculae Plages: hot clouds in the Chromosphere Flares Prominences