Astronomy: Stars
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This document discusses different types of stars and their characteristics. It defines key star classifications like clusters, luminosity, and the Hertzsprung-Russell diagram. It also notes there are 7 types of stars and provides examples like the Sun being a yellow dwarf. Spectroscopy is used to study star compositions by analyzing their visible light. The largest and hottest stars called supergiants have the shortest lifespans, while cooler red stars emit most energy as red and infrared light.
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2. Stars are classified into seven spectral classes based on their colors, from hottest blue class O to coolest red class M.
3. The Hertzsprung-Russell diagram plots stars based on their luminosity and temperature, showing locations for main sequence stars like the Sun as well as red giants, blue giants, and other stages.
Life Cycle Of A Star
The document discusses the life cycle of stars from their birth in nebulae to their death. Stars are born when gas and dust clouds collapse under gravity and heat up. During their main sequence phase, stars fuse hydrogen into helium in their cores. Later, larger stars become red giants or supergiants as their cores shrink and outer layers expand. Eventually, stars die and eject their outer layers, leaving behind dense remnants like white dwarfs, neutron stars, or black holes.
Stars - Basic Properties/H- R Diagram
The document discusses properties of stars and methods astronomers use to study them. It describes the composition of the Sun and how its composition is similar to other stars and gas giants. It then explains different types of groups stars can be found in, including constellations, clusters, and binary systems. The document also discusses methods astronomers use to measure stellar distances and properties, including parallax, apparent and absolute magnitude, luminosity, and spectral classification. It introduces the Hertzsprung-Russell diagram and how it relates stellar properties like mass, luminosity, temperature and size.
Ch 26 2 characteristics of stars
Stars have common characteristics including size, mass, color, temperature, and brightness. Size ranges from neutron stars the size of a city to supergiant stars 1000 times the size of the sun. Composition is primarily hydrogen and helium. Color indicates surface temperature from red stars at 3,000 K to blue-white stars at 50,000 K. Brightness depends on size, temperature, and distance from Earth. The Hertzsprung-Russell diagram shows the relationship between absolute magnitude and surface temperature for stars.
The gaia eso_survey_stellar_content_and_elemental_abundances_in_the_massive_c...
Estudo sobre o conteúdo estelar e os elementos que estão presentes no aglomerado estelar aberto NGC 6705, também conhecido como Aglomerado do Pato Selvagem.
Star life cycles
The document summarizes information about the formation and evolution of stars, including our sun. It discusses how stars are formed from collapsing gas clouds, and how stars of different masses will evolve differently. Lower mass stars like our sun will become red giants and end as white dwarfs, while very massive stars may explode as supernovae and form neutron stars or black holes. It also provides information about classifying and identifying properties of stars using tools like spectroscopy and star charts.
Characteristics of stars
This document provides information about stars, including their characteristics, sizes, colors, brightness, and life cycles. It describes how stars can be viewed through telescopes and the largest telescopes in the Philippines. Stars are classified based on their spectral type, which determines their color and temperature. They range greatly in size from red supergiants over 1,000 times the sun's radius to tiny white dwarfs only 1% of the sun's radius. The document also explains how astronomers measure and compare the apparent and absolute magnitudes of stars to determine their brightness.
The Star
This document provides an overview of the characteristics, classifications, motions, and significance of stars. It discusses their sizes, colors, temperatures, compositions, and magnitudes. Stars are classified based on their spectral types, which relate to their surface temperatures. The Hertzsprung-Russell diagram plots stars' luminosities and temperatures. Stars exhibit both apparent and actual motions, including proper motion across the sky. Studying stars helps us understand how elements are formed, how our solar system evolved, and the dynamics influencing galaxies.
Components of our universe
1) The document is an astronomy homework assignment that includes questions about the components of the universe. It asks students to identify the correct diagram showing the relationship between different regions of space, describe the Milky Way galaxy, define what a light year is, and indicate where Earth's solar system is located within the Milky Way.
2) It also includes questions based on a newspaper article about astronomers detecting the faintest and most distant galaxies ever observed using the Hubble Space Telescope. These galaxies are over 12 billion light years away and provide the first glimpse within 1 billion light years of the beginning of the universe.
3) The distant galaxies are seen as they were when the universe was only about 5% of its present age
The Stars of the Sky and their Life Cycles (2).pptx
The document discusses the life cycles of stars from their birth in molecular clouds to their evolution on the main sequence and eventual death. It begins by explaining how stars are born from collapsing gas and dust in molecular clouds. It then describes how protostars form and evolve into pre-main sequence stars. Next, it discusses how stars exist on the main sequence fusing hydrogen until more massive stars die in supernovae while less massive stars become white dwarfs. The document also provides details on properties of stars like luminosity, temperature, and how the Hertzsprung-Russell diagram is used to study stellar evolution.
Constituents and Structure, Processes of Nature, Natural Hazards and Disaster...
General science covers topics like the physical, biological, environmental, food, and information sciences. It also covers general abilities like quantitative reasoning, logical reasoning, and mental abilities. The document provides details on the formation of the universe according to the Big Bang Theory, including the early singularity, the expansion and formation of subatomic particles, atoms, and galaxies. It discusses evidence that supports the Big Bang Theory, such as Hubble's law of the expanding universe and the discovery of cosmic microwave background radiation.
Star Formation.pdf
1. Stars are formed from the collapse of dense pockets of gas and dust within nebulae. As the protostar contracts under gravity, nuclear fusion begins in the core, marking the start of the main sequence phase.
2. During the main sequence, stars fuse hydrogen into helium through nuclear fusion, emitting energy. After hydrogen is exhausted, stars evolve into red giants as the core contracts and outer layers expand.
3. The eventual fate of a star depends on its mass. Lower mass stars become white dwarfs, while very massive stars end as supernovae, leaving behind neutron stars or black holes. Supernovae help astronomers measure distances in the universe.
Eso1147a
This document introduces the VLT-FLAMES Tarantula Survey, which obtained multi-epoch optical spectroscopy of over 800 massive stars in the 30 Doradus region of the Large Magellanic Cloud. The survey aims to detect massive binary systems through variations in radial velocities and to characterize the properties of O- and B-type stars, addressing questions about stellar and cluster evolution. Spectral classifications are provided for newly discovered emission-line stars, including a new Wolf-Rayet star. The survey data and reduction procedures are overviewed, and upcoming analyses of the massive star properties are announced.
Astro Review Packet 1
This document contains a 20 question astronomy review packet covering topics like the formation of the solar system, stellar evolution, properties of stars and galaxies. It includes diagrams and tables to reference in answering multiple choice and short answer questions. The review covers the life cycles of stars of different masses, including our Sun, as well as properties of planets, asteroids and galaxies.
Interactive PowerPoint: Classifying Stars
Stars form from clouds of dust and gas called nebulae. Gravity causes the gas and dust to collapse into a dense protostar at the center. When the protostar becomes hot and dense enough, nuclear fusion occurs, releasing energy and causing the star to shine. A star's lifespan depends on its mass - lower mass stars last for billions of years, while higher mass stars only last millions of years before ending their lives in supernova explosions. Scientists classify stars based on their temperature and the elements they absorb, with classifications ranging from hottest O-type stars to coolest M-type stars.
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The gaia eso_survey_stellar_content_and_elemental_abundances_in_the_massive_c...
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The Stars of the Sky and their Life Cycles (2).pptx
The Stars of the Sky and their Life Cycles (2).pptx
Constituents and Structure, Processes of Nature, Natural Hazards and Disaster...
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Recently uploaded
The binding of cosmological structures by massless topological defects
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
Deep Software Variability and Frictionless Reproducibility
Deep Software Variability and Frictionless ReproducibilityUniversity of Rennes, INSA Rennes, Inria/IRISA, CNRS
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.
I will then present some software engineering and AI techniques that can support the strategic exploration of variability spaces. These include the use of abstractions and models (e.g., feature models), sampling strategies (e.g., uniform, random), cost-effective measurements (e.g., incremental build of software configurations), and dimensionality reduction methods (e.g., transfer learning, feature selection, software debloating).
I will finally argue that deep variability is both the problem and solution of frictionless reproducibility, calling the software science community to develop new methods and tools to manage variability and foster reproducibility in software systems.
Exposé invité Journées Nationales du GDR GPL 2024
bordetella pertussis.................................ppt
Bordettela is a gram negative cocobacilli spread by air born drop let
Applied Science: Thermodynamics, Laws & Methodology.pdf
When I was asked to give a companion lecture in support of ‘The Philosophy of Science’ (https://shorturl.at/4pUXz) I decided not to walk through the detail of the many methodologies in order of use. Instead, I chose to employ a long standing, and ongoing, scientific development as an exemplar. And so, I chose the ever evolving story of Thermodynamics as a scientific investigation at its best.
Conducted over a period of >200 years, Thermodynamics R&D, and application, benefitted from the highest levels of professionalism, collaboration, and technical thoroughness. New layers of application, methodology, and practice were made possible by the progressive advance of technology. In turn, this has seen measurement and modelling accuracy continually improved at a micro and macro level.
Perhaps most importantly, Thermodynamics rapidly became a primary tool in the advance of applied science/engineering/technology, spanning micro-tech, to aerospace and cosmology. I can think of no better a story to illustrate the breadth of scientific methodologies and applications at their best.
Randomised Optimisation Algorithms in DAPHNE
Slides from talk:
Aleš Zamuda: Randomised Optimisation Algorithms in DAPHNE .
Austrian-Slovenian HPC Meeting 2024 – ASHPC24, Seeblickhotel Grundlsee in Austria, 10–13 June 2024
https://ashpc.eu/
Bob Reedy - Nitrate in Texas Groundwater.pdf
Presented at June 6-7 Texas Alliance of Groundwater Districts Business Meeting
Phenomics assisted breeding in crop improvement
As the population is increasing and will reach about 9 billion upto 2050. Also due to climate change, it is difficult to meet the food requirement of such a large population. Facing the challenges presented by resource shortages, climate
change, and increasing global population, crop yield and quality need to be improved in a sustainable way over the coming decades. Genetic improvement by breeding is the best way to increase crop productivity. With the rapid progression of functional
genomics, an increasing number of crop genomes have been sequenced and dozens of genes influencing key agronomic traits have been identified. However, current genome sequence information has not been adequately exploited for understanding
the complex characteristics of multiple gene, owing to a lack of crop phenotypic data. Efficient, automatic, and accurate technologies and platforms that can capture phenotypic data that can
be linked to genomics information for crop improvement at all growth stages have become as important as genotyping. Thus,
high-throughput phenotyping has become the major bottleneck restricting crop breeding. Plant phenomics has been defined as the high-throughput, accurate acquisition and analysis of multi-dimensional phenotypes
during crop growing stages at the organism level, including the cell, tissue, organ, individual plant, plot, and field levels. With the rapid development of novel sensors, imaging technology,
and analysis methods, numerous infrastructure platforms have been developed for phenotyping.
Describing and Interpreting an Immersive Learning Case with the Immersion Cub...
Current descriptions of immersive learning cases are often difficult or impossible to compare. This is due to a myriad of different options on what details to include, which aspects are relevant, and on the descriptive approaches employed. Also, these aspects often combine very specific details with more general guidelines or indicate intents and rationales without clarifying their implementation. In this paper we provide a method to describe immersive learning cases that is structured to enable comparisons, yet flexible enough to allow researchers and practitioners to decide which aspects to include. This method leverages a taxonomy that classifies educational aspects at three levels (uses, practices, and strategies) and then utilizes two frameworks, the Immersive Learning Brain and the Immersion Cube, to enable a structured description and interpretation of immersive learning cases. The method is then demonstrated on a published immersive learning case on training for wind turbine maintenance using virtual reality. Applying the method results in a structured artifact, the Immersive Learning Case Sheet, that tags the case with its proximal uses, practices, and strategies, and refines the free text case description to ensure that matching details are included. This contribution is thus a case description method in support of future comparative research of immersive learning cases. We then discuss how the resulting description and interpretation can be leveraged to change immersion learning cases, by enriching them (considering low-effort changes or additions) or innovating (exploring more challenging avenues of transformation). The method holds significant promise to support better-grounded research in immersive learning.
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
Although Artemia has been known to man for centuries, its use as a food for the culture of larval organisms apparently began only in the 1930s, when several investigators found that it made an excellent food for newly hatched fish larvae (Litvinenko et al., 2023). As aquaculture developed in the 1960s and ‘70s, the use of Artemia also became more widespread, due both to its convenience and to its nutritional value for larval organisms (Arenas-Pardo et al., 2024). The fact that Artemia dormant cysts can be stored for long periods in cans, and then used as an off-the-shelf food requiring only 24 h of incubation makes them the most convenient, least labor-intensive, live food available for aquaculture (Sorgeloos & Roubach, 2021). The nutritional value of Artemia, especially for marine organisms, is not constant, but varies both geographically and temporally. During the last decade, however, both the causes of Artemia nutritional variability and methods to improve poorquality Artemia have been identified (Loufi et al., 2024).
Brine shrimp (Artemia spp.) are used in marine aquaculture worldwide. Annually, more than 2,000 metric tons of dry cysts are used for cultivation of fish, crustacean, and shellfish larva. Brine shrimp are important to aquaculture because newly hatched brine shrimp nauplii (larvae) provide a food source for many fish fry (Mozanzadeh et al., 2021). Culture and harvesting of brine shrimp eggs represents another aspect of the aquaculture industry. Nauplii and metanauplii of Artemia, commonly known as brine shrimp, play a crucial role in aquaculture due to their nutritional value and suitability as live feed for many aquatic species, particularly in larval stages (Sorgeloos & Roubach, 2021).
The debris of the ‘last major merger’ is dynamically young
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Cytokines and their role in immune regulation.pptx
This presentation covers the content and information on "Cytokines " and their role in immune regulation .
3D Hybrid PIC simulation of the plasma expansion (ISSS-14)
3D Particle-In-Cell (PIC) algorithm,
Plasma expansion in the dipole magnetic field.
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留信网认证的作用:
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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
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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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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.
Travis Hills' Endeavors in Minnesota: Fostering Environmental and Economic Pr...
Travis Hills of Minnesota developed a method to convert waste into high-value dry fertilizer, significantly enriching soil quality. By providing farmers with a valuable resource derived from waste, Travis Hills helps enhance farm profitability while promoting environmental stewardship. Travis Hills' sustainable practices lead to cost savings and increased revenue for farmers by improving resource efficiency and reducing waste.
SAR of Medicinal Chemistry 1st by dk.pdf
In this presentation include the prototype drug SAR on thus or with their examples .
Syllabus of Second Year B. Pharmacy
2019 PATTERN.
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The binding of cosmological structures by massless topological defects
The binding of cosmological structures by massless topological defects
Deep Software Variability and Frictionless Reproducibility
Deep Software Variability and Frictionless Reproducibility
bordetella pertussis.................................ppt
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aziz sancar nobel prize winner: from mardin to nobel
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Applied Science: Thermodynamics, Laws & Methodology.pdf
Applied Science: Thermodynamics, Laws & Methodology.pdf
Describing and Interpreting an Immersive Learning Case with the Immersion Cub...
Describing and Interpreting an Immersive Learning Case with the Immersion Cub...
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
The debris of the ‘last major merger’ is dynamically young
The debris of the ‘last major merger’ is dynamically young
Cytokines and their role in immune regulation.pptx
Cytokines and their role in immune regulation.pptx
3D Hybrid PIC simulation of the plasma expansion (ISSS-14)
3D Hybrid PIC simulation of the plasma expansion (ISSS-14)
Authoring a personal GPT for your research and practice: How we created the Q...
Authoring a personal GPT for your research and practice: How we created the Q...
mô tả các thí nghiệm về đánh giá tác động dòng khí hóa sau đốt
mô tả các thí nghiệm về đánh giá tác động dòng khí hóa sau đốt
Travis Hills' Endeavors in Minnesota: Fostering Environmental and Economic Pr...
Travis Hills' Endeavors in Minnesota: Fostering Environmental and Economic Pr...
Astronomy: Stars
- 2. Measuring the stars, Giants, Dwarfs and the Main Sequence
- 4. 1.) ________ is born when an enormous cloud of hydrogen gas collapses until it is hot enough to burn nuclear fuel. STAR
- 5. 2.) The group of stars are called ________. CLUSTERS
- 6. 3.) It is the rate at which a star radiates energy into space. Luminosity
- 7. 4.) It is a graph that plots stars color and its luminosity. Hertzsprung - Russell Diagram
- 8. 5.) How many types are there to classify a star? 7
- 9. 6.) ________ is an example of a yellow dwarf. SUN
- 10. 7.) The composition of stars is studied using _____________ in which their visible light is studied. SPECTROSCOP Y
- 11. 8.) These are the classification of stars; O, B, A, T, F, G, K, which letter does not belong to the group? T
- 12. 9.) Sirius and Vega are examples of a type A star. TRUE or FALSE TRUE
- 13. 10.) ___________ is the rate at which a star's radiated energy reaches an observer on Earth. APPARENT BRIGHTNESS
- 14. 11.) _____ stars radiate most of their energy in the red and infrared region of the electromagnetic spectrum and thus appear red. COOL
- 15. 12.) Hot stars emit mostly _______ and ultra-violet rays. BLUE
- 16. 13.) It is the largest known type of star, some are almost as large as our entire solar system. SUPERGIANT STARS
- 17. 14.) A rapidly spinning neutron star that emits energy in pulses. PULSAR
- 18. 15.) The largest stars have the shortest life span. TRUE or FALSE TRUE