BASIC INTERACTIONS BETWEEN X RAYS AND MATTER.ppt
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X-rays can interact with matter through several interactions, the most significant in diagnostic radiology being coherent scattering (Rayleigh scattering and Thomson scattering) and Compton scattering. In Rayleigh scattering, photons are scattered by bound electrons in an atom without exciting or ionizing the atom. In Compton scattering, a high energy photon collides with and ejects a loosely bound electron, becoming deflected and losing some energy. The patient's body is the main source of scattered radiation during an x-ray procedure, degrading image quality and increasing radiation exposure to personnel.
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Intercation with matter
X-rays can interact with matter through various interactions such as coherent scattering, photoelectric effect, Compton scattering, pair production, and photodisintegration. The photoelectric effect and Compton scattering are the most important interactions for diagnostic x-rays. The photoelectric effect accounts for about 75% of interactions and results in the emission of characteristic x-rays. Compton scattering accounts for about 20% of interactions and scatters x-rays without energy loss, producing scatter radiation. The interaction that occurs depends on the photon energy and the atomic number of the absorbing material.
Interactions of X rays with matter
This document discusses the interactions between x-rays and matter. There are three main interactions - photoelectric effect, Compton scattering, and coherent scattering. The photoelectric effect occurs when a photon ejects an inner shell electron from an atom. This produces characteristic x-rays and leaves the atom ionized. Compton scattering involves the deflection of photons by outer shell electrons, producing scattered radiation. At diagnostic energies, Compton scattering is the most common interaction. The photoelectric effect dominates for high atomic number materials and low energy x-rays. These two interactions are most important in diagnostic radiology, while coherent scattering, pair production and photodisintegration occur at higher energies.
Interaction of x ray with matter
This slide contains the Information regarding what changes takes place when the X-ray Interacts with matter.
Basic Interaction Between X-Rays & Matter.pptx
X-ray photons can interact with matter through five basic interactions: coherent scattering, photoelectric effect, Compton scattering, pair production, and photodisintegration. At diagnostic energies, the most common interactions are coherent scattering, the photoelectric effect, and Compton scattering. The photoelectric effect produces high quality images but also results in higher patient radiation exposure. Compton scattering is the main source of scatter radiation in diagnostic radiology and can reduce image quality.
ppt-150711165239-lva1-app6892.pdf
This document discusses the dual wave-particle nature of X-rays and their interaction with matter. It notes that X-rays can behave as both waves that propagate through space, as well as particles called photons. The key interactions discussed are photoelectric effect, Compton scattering, and pair production.
The photoelectric effect results in a photon being absorbed by an atom, ejecting an electron and leaving the atom ionized. Compton scattering involves a photon ejecting an electron from an atom but also being deflected and losing some energy. Pair production occurs when a photon interacts near the nucleus of an atom and transforms into an electron-positron pair.
Ppt
This document discusses the dual wave-particle nature of X-rays and their interaction with matter. It notes that X-rays can behave as both waves that propagate through space, as well as particles called photons. The two main interactions discussed are the photoelectric effect and Compton scattering.
The photoelectric effect occurs when a photon ejects an inner shell electron from an atom. This produces characteristic radiation, a photoelectron, and an ionized atom. It is most likely with low-energy photons and high atomic number elements. Compton scattering occurs when a high-energy photon ejects a loosely bound outer shell electron. This produces a recoil electron and scattered photon, with energy distributed between the two. Scattered photons are
interaction of xray with matter
X-rays can interact with matter through various interactions such as the photoelectric effect, Compton scattering, and coherent scattering. The photoelectric effect is the predominant interaction for low energy x-rays and high atomic number materials, producing no scatter radiation and high contrast images. Compton scattering is the most common interaction at higher diagnostic x-ray energies and is responsible for generating scatter radiation. Only the photoelectric effect and Compton scattering are important for diagnostic radiology.
Basic Interactions Between X Rays and Matter
X-rays can interact with matter through various processes. The most common interactions in diagnostic radiology are the photoelectric effect, Compton scattering, and coherent scattering. In the photoelectric effect, an incoming x-ray photon ejects an inner shell electron, leaving behind characteristic radiation. Compton scattering involves x-ray photon deflection by a free electron, producing scatter radiation. Coherent scattering changes a photon's direction but not its energy. These interactions have different probabilities depending on the photon energy and the electron binding energy.
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Intercation with matter
X-rays can interact with matter through various interactions such as coherent scattering, photoelectric effect, Compton scattering, pair production, and photodisintegration. The photoelectric effect and Compton scattering are the most important interactions for diagnostic x-rays. The photoelectric effect accounts for about 75% of interactions and results in the emission of characteristic x-rays. Compton scattering accounts for about 20% of interactions and scatters x-rays without energy loss, producing scatter radiation. The interaction that occurs depends on the photon energy and the atomic number of the absorbing material.
Interactions of X rays with matter
This document discusses the interactions between x-rays and matter. There are three main interactions - photoelectric effect, Compton scattering, and coherent scattering. The photoelectric effect occurs when a photon ejects an inner shell electron from an atom. This produces characteristic x-rays and leaves the atom ionized. Compton scattering involves the deflection of photons by outer shell electrons, producing scattered radiation. At diagnostic energies, Compton scattering is the most common interaction. The photoelectric effect dominates for high atomic number materials and low energy x-rays. These two interactions are most important in diagnostic radiology, while coherent scattering, pair production and photodisintegration occur at higher energies.
Interaction of x ray with matter
This slide contains the Information regarding what changes takes place when the X-ray Interacts with matter.
Basic Interaction Between X-Rays & Matter.pptx
X-ray photons can interact with matter through five basic interactions: coherent scattering, photoelectric effect, Compton scattering, pair production, and photodisintegration. At diagnostic energies, the most common interactions are coherent scattering, the photoelectric effect, and Compton scattering. The photoelectric effect produces high quality images but also results in higher patient radiation exposure. Compton scattering is the main source of scatter radiation in diagnostic radiology and can reduce image quality.
ppt-150711165239-lva1-app6892.pdf
This document discusses the dual wave-particle nature of X-rays and their interaction with matter. It notes that X-rays can behave as both waves that propagate through space, as well as particles called photons. The key interactions discussed are photoelectric effect, Compton scattering, and pair production.
The photoelectric effect results in a photon being absorbed by an atom, ejecting an electron and leaving the atom ionized. Compton scattering involves a photon ejecting an electron from an atom but also being deflected and losing some energy. Pair production occurs when a photon interacts near the nucleus of an atom and transforms into an electron-positron pair.
Ppt
This document discusses the dual wave-particle nature of X-rays and their interaction with matter. It notes that X-rays can behave as both waves that propagate through space, as well as particles called photons. The two main interactions discussed are the photoelectric effect and Compton scattering.
The photoelectric effect occurs when a photon ejects an inner shell electron from an atom. This produces characteristic radiation, a photoelectron, and an ionized atom. It is most likely with low-energy photons and high atomic number elements. Compton scattering occurs when a high-energy photon ejects a loosely bound outer shell electron. This produces a recoil electron and scattered photon, with energy distributed between the two. Scattered photons are
interaction of xray with matter
X-rays can interact with matter through various interactions such as the photoelectric effect, Compton scattering, and coherent scattering. The photoelectric effect is the predominant interaction for low energy x-rays and high atomic number materials, producing no scatter radiation and high contrast images. Compton scattering is the most common interaction at higher diagnostic x-ray energies and is responsible for generating scatter radiation. Only the photoelectric effect and Compton scattering are important for diagnostic radiology.
Basic Interactions Between X Rays and Matter
X-rays can interact with matter through various processes. The most common interactions in diagnostic radiology are the photoelectric effect, Compton scattering, and coherent scattering. In the photoelectric effect, an incoming x-ray photon ejects an inner shell electron, leaving behind characteristic radiation. Compton scattering involves x-ray photon deflection by a free electron, producing scatter radiation. Coherent scattering changes a photon's direction but not its energy. These interactions have different probabilities depending on the photon energy and the electron binding energy.
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Photon interaction with matter rahul
1. Photons interact with matter through various processes depending on their energy level. Low energy photons mainly undergo coherent scattering, while intermediate energies result in the Compton effect. Higher energy photons above 1.02 MeV can undergo pair production.
2. During interactions, photons may be deflected without energy loss, deflected with some energy loss, disappear by ejecting electrons, or pass through unchanged. Common interaction types include the photoelectric effect, Compton scattering, and pair production.
3. The dominant interaction mechanism depends on photon energy and the atomic number of the absorber. Low energies favor photoelectric effect in high Z materials, while Compton scattering does not depend strongly on Z. Pair production rises with both energy
physical interaction of x ray with matter
Dr. Chaudhary's presentation discussed the dual wave-particle nature of X-rays and their interaction with matter. X-rays can behave as both waves, which allows them to be reflected, and particles called photons. The photoelectric effect occurs when a photon interacts with and ejects an electron from an atom, becoming absorbed. This produces characteristic radiation as the electron vacancy is filled. The photoelectric effect yields an ion, photoelectron, and photon, and is more likely with low energy photons and high atomic number elements if the photon energy exceeds the electron's binding energy. It provides excellent radiographic images with no scatter but maximum radiation exposure to the patient.
Basic interaction of X-rays with matter
This document summarizes the five main types of interactions that can occur between x-ray photons and matter:
1. Coherent scattering: The photon changes direction but not wavelength without energy transfer.
2. Photoelectric effect: The photon is absorbed and an electron is ejected from an atom.
3. Compton scattering: The photon scatters off an electron, imparting some energy to the electron and losing energy itself.
4. Pair production: A high energy photon interacts with the nucleus and converts into an electron-positron pair.
5. Photodisintegration: A very high energy photon ejects part of an atom's nucleus.
Interaction Between Matter and X ray
X-rays can interact with matter through various interactions including the photoelectric effect, Compton scattering, and coherent scattering. The photoelectric effect and Compton scattering are the most important interactions in diagnostic radiology. Scatter radiation is a major source of reduced image quality and increased patient dose in x-rays, and various techniques like grids and filters are used to control scatter.
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from the book "Radiobiology for the Radiologist, 7th Ed by E.J Hall"
I'll delete the file immediately, if it is illegal to upload the file.
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This document discusses the interactions of various types of radiation with matter. It describes five main interactions that x-rays and gamma rays can undergo: photoelectric effect, Compton scattering, coherent scattering, pair production, and photodisintegration. It explains that the photoelectric effect and Compton scattering are most important for diagnostic and therapeutic radiology respectively. It also discusses the interactions of particulate radiation such as electrons, protons, neutrons, alpha particles, and heavy ions with matter and how they deposit energy.
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X-rays can interact with matter through five main interactions:
1) Coherent scattering - X-rays change direction without energy loss.
2) Photoelectric effect - High energy photons eject tightly bound electrons.
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4) Pair production - High energy photons convert into electron-positron pairs in the nucleus.
5) Photodisintegration - Very high energy photons eject parts of the nucleus. Coherent scattering and the photoelectric effect are most relevant for medical and industrial X-ray applications.
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1) The document discusses the interaction of radiation with matter, including the different types of radiation and their properties. It describes electromagnetic radiation and the electromagnetic spectrum.
2) The main interactions that occur between radiation and matter are photoelectric effect, Compton scattering, and pair production. The photoelectric effect involves the ejection of an electron from an atom when a photon transfers all its energy. Compton scattering is the scattering of photons by loosely bound electrons, resulting in energy transfer. Pair production occurs when a photon converts into an electron-positron pair in the vicinity of a nucleus.
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Interactions of X-ray & matter & Attenuation - Dr. Sayak Datta
Slideshow on Radio-physics covering different interactions between X-ray and matter along with Attenuation. It includes Photo-electric effect, Compton scatter, Coherent scatter, Attenuation of Monochromatic & Polychromatic radiation, Diagnostic Xray applications, Scatter radiations.
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1. Photons interact with matter through various processes depending on their energy level. Low energy photons mainly undergo coherent scattering, while intermediate energies result in the Compton effect. Higher energy photons above 1.02 MeV can undergo pair production.
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Basic interaction of X-rays with matter
This document summarizes the five main types of interactions that can occur between x-ray photons and matter:
1. Coherent scattering: The photon changes direction but not wavelength without energy transfer.
2. Photoelectric effect: The photon is absorbed and an electron is ejected from an atom.
3. Compton scattering: The photon scatters off an electron, imparting some energy to the electron and losing energy itself.
4. Pair production: A high energy photon interacts with the nucleus and converts into an electron-positron pair.
5. Photodisintegration: A very high energy photon ejects part of an atom's nucleus.
Interaction Between Matter and X ray
X-rays can interact with matter through various interactions including the photoelectric effect, Compton scattering, and coherent scattering. The photoelectric effect and Compton scattering are the most important interactions in diagnostic radiology. Scatter radiation is a major source of reduced image quality and increased patient dose in x-rays, and various techniques like grids and filters are used to control scatter.
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The document discusses various interactions between radiation and matter, including excitation, ionization, and radiative losses. It describes the processes of excitation, ionization, specific ionization, linear energy transfer, scattering, bremsstrahlung, and the four main interactions of x-rays and gamma rays with matter: Rayleigh scattering, Compton scattering, photoelectric absorption, and pair production. The probability and characteristics of each interaction depends on factors like the atomic number of the absorbing material and the energy of the incident radiation. These interactions are important in diagnostic imaging and radiation therapy.
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This document discusses the interaction of x-ray photons with matter and their attenuation. There are five main interaction types: coherent scattering, Compton scattering, photoelectric effect, pair production, and photodisintegration. In diagnostic medical imaging, the dominant interactions are the Compton effect and photoelectric effect. The Compton effect involves the x-ray scattering off and ejecting an outer shell electron. This produces scattered x-rays and reduces image contrast. The photoelectric effect fully absorbs the x-ray when it ejects an inner shell electron. This is the primary means of x-ray absorption and produces high quality images. The degree of x-ray attenuation is dependent on factors like energy, density, and atomic number of
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I'll delete the file immediately, if it is illegal to upload the file.
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This document discusses the interactions of various types of radiation with matter. It describes five main interactions that x-rays and gamma rays can undergo: photoelectric effect, Compton scattering, coherent scattering, pair production, and photodisintegration. It explains that the photoelectric effect and Compton scattering are most important for diagnostic and therapeutic radiology respectively. It also discusses the interactions of particulate radiation such as electrons, protons, neutrons, alpha particles, and heavy ions with matter and how they deposit energy.
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X-rays can interact with matter through five main interactions:
1) Coherent scattering - X-rays change direction without energy loss.
2) Photoelectric effect - High energy photons eject tightly bound electrons.
3) Compton scattering - Photons collide with loosely bound electrons, losing some energy.
4) Pair production - High energy photons convert into electron-positron pairs in the nucleus.
5) Photodisintegration - Very high energy photons eject parts of the nucleus. Coherent scattering and the photoelectric effect are most relevant for medical and industrial X-ray applications.
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It gives some easy and detailed information about the basics of a radiological physics and will explain about the interactions of Electron in the target atoms.
lecture_6_20.ppt
This document discusses the interactions of ionizing radiation with matter. It begins by introducing the objectives of understanding how radiation interacts with matter and the effects on physical, chemical, and biological levels. It then covers the three main interactions of photons (photoelectric effect, Compton scattering, pair production) and how they lead to attenuation. Key points include how probability depends on photon energy and atomic number, and the byproducts of each interaction. It also discusses the interactions of particulate radiation like electrons, protons, neutrons, and how they ionize matter through excitation, ionization, and bremsstrahlung. Factors like linear energy transfer and specific ionization are addressed. The document is intended to provide background knowledge on radiation detection and
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2) The main interactions that occur between radiation and matter are photoelectric effect, Compton scattering, and pair production. The photoelectric effect involves the ejection of an electron from an atom when a photon transfers all its energy. Compton scattering is the scattering of photons by loosely bound electrons, resulting in energy transfer. Pair production occurs when a photon converts into an electron-positron pair in the vicinity of a nucleus.
3) The dominant interaction depends on the photon energy - photoelectric effect dominates at low energies, Compton scattering in the soft
Interactions of radiation with matter
I do not have enough context to answer these questions. The document provided is a lecture on interactions of radiation with matter and does not contain questions.
Interaction of x rays with matter
In this lecture, we will be talking only about the interaction of an ionizing electromagnetic radiation with matter, specifically about the interaction of X-Rays with the matter
Note: Gamma rays interact with the matter by the same way that X-rays interact with matter. In this lecture, we just focused on X-rays to complete our previous lecture about the production of X-rays
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Interactions of X-ray & matter & Attenuation - Dr. Sayak Datta
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Osteomyelitis is an infection of bone that is usually caused by bacteria entering through the bloodstream or direct inoculation via injury. It can be acute, subacute, or chronic. Common symptoms include fever, pain, and swelling near the infected bone. Diagnosis involves blood tests, imaging like x-rays, MRI, and bone scans, and bone/blood cultures. Treatment consists of antibiotics tailored to the identified bacteria as well as possible surgical drainage of abscesses.
retroperitonealmasses-pptx
This document discusses primary retroperitoneal neoplasms, which arise outside of major retroperitoneal organs. It notes that 70-80% of retroperitoneal masses are malignant in nature. The document then categorizes and describes several specific types of solid neoplastic masses that can occur in the retroperitoneum, including mesodermal neoplasms (such as liposarcomas and leiomyosarcomas), neurogenic tumors, and others. For each type of mass, it provides details on prevalence, appearance on CT and MRI scans, characteristics, associated syndromes, and other relevant clinical information.
ULTRASOUND IN FIRST TRIMESTER.ppt
1. The goals of first trimester ultrasound include visualization of the gestational sac, identification of embryonic demise, determination of gestational age, and early diagnosis of fetal anomalies.
2. A normal intrauterine gestation will demonstrate a gestational sac, yolk sac, embryo, amnion, and cardiac activity on ultrasound. Measurement of the mean sac diameter, crown-rump length, and biometric measurements can be used to estimate gestational age.
3. Absence of cardiac activity along with signs of bleeding have a high probability of embryonic demise. Criteria such as large sac size without visualizing fetal structures indicate a poor pregnancy outcome.
OSTEONECROSIS 2003.ppt
This document discusses Legg-Calve-Perthes disease, which is avascular necrosis of the femoral head that occurs in children. It begins by describing the etiology as an ischemic episode affecting the capital femoral epiphysis, though the exact cause is unknown. The stages of the disease are then outlined based on radiographic appearance, from initial avascular necrosis to revascularization and bone remodeling. Complications including deformities of the femoral head and neck are also summarized. The document provides detailed information on the radiographic signs and classifications systems used to evaluate the progression and prognosis of Legg-Calve-Perthes disease.
GRIDS.ppt
X-ray grids are devices used to remove scattered radiation from radiographic images. They consist of alternating strips of lead and transparent material. Grids work by absorbing most of the multidirectional scattered radiation while allowing the directional primary radiation to pass through. Grid performance is evaluated based on primary transmission, Bucky factor, and contrast improvement factor. Proper grid selection and positioning are important to avoid grid cutoff and increased patient radiation dose. Moving grids eliminate grid line artifacts but have some disadvantages.
fluoro1-principles.PPT
This document discusses fluoroscopy, including conventional fluoroscopy units and modern fluoroscopic units. It describes the key components of a fluoroscopic unit, including the image intensifier, vidicon camera, and TV monitor. It also discusses factors that influence fluoroscopic image quality such as radiation dose rates, image resolution both vertically and horizontally, and techniques to reduce image noise like frame averaging.
FLUOROSCOPIC IMAGING.ppt
A fluoroscope uses x-rays and a fluorescent screen to enable direct observation of internal organs. It consists of an x-ray tube, table, and image intensifier. The image intensifier converts x-rays into visible light images and amplifies them for viewing. It works by accelerating photoelectrons emitted from a photocathode onto a phosphor screen, producing light photons and gaining brightness. Newer generations of image intensifiers use additional electron multiplication for higher sensitivity. Fluoroscopy provides real-time moving images for procedures while fluorography captures still diagnostic images.
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一比一原版(macewan学位证书)加拿大麦科文大学毕业证如何办理
原版一模一样【微信：741003700 】【(macewan学位证书)加拿大麦科文大学毕业证成绩单】【微信：741003700 】学位证，留信认证（真实可查，永久存档）原件一模一样纸张工艺/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。
本公司拥有海外各大学样板无数，能完美还原。
1:1完美还原海外各大学毕业材料上的工艺：水印，阴影底纹，钢印LOGO烫金烫银，LOGO烫金烫银复合重叠。文字图案浮雕、激光镭射、紫外荧光、温感、复印防伪等防伪工艺。材料咨询办理、认证咨询办理请加学历顾问Q/微741003700
【主营项目】
一.毕业证【q微741003700】成绩单、使馆认证、教育部认证、雅思托福成绩单、学生卡等！
二.真实使馆公证(即留学回国人员证明,不成功不收费)
三.真实教育部学历学位认证（教育部存档！教育部留服网站永久可查）
四.办理各国各大学文凭(一对一专业服务,可全程监控跟踪进度)
如果您处于以下几种情况：
◇在校期间，因各种原因未能顺利毕业……拿不到官方毕业证【q/微741003700】
◇面对父母的压力，希望尽快拿到；
◇不清楚认证流程以及材料该如何准备；
◇回国时间很长，忘记办理；
◇回国马上就要找工作，办给用人单位看；
◇企事业单位必须要求办理的
◇需要报考公务员、购买免税车、落转户口
◇申请留学生创业基金
留信网认证的作用:
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
6:个人职称评审加20分
7:个人信誉贷款加10分
8:在国家人才网主办的国家网络招聘大会中纳入资料，供国家高端企业选择人才
办理(macewan学位证书)加拿大麦科文大学毕业证【微信：741003700 】外观非常简单，由纸质材料制成，上面印有校徽、校名、毕业生姓名、专业等信息。
办理(macewan学位证书)加拿大麦科文大学毕业证【微信：741003700 】格式相对统一，各专业都有相应的模板。通常包括以下部分：
校徽：象征着学校的荣誉和传承。
校名:学校英文全称
授予学位：本部分将注明获得的具体学位名称。
毕业生姓名：这是最重要的信息之一，标志着该证书是由特定人员获得的。
颁发日期：这是毕业正式生效的时间，也代表着毕业生学业的结束。
其他信息：根据不同的专业和学位，可能会有一些特定的信息或章节。
办理(macewan学位证书)加拿大麦科文大学毕业证【微信：741003700 】价值很高，需要妥善保管。一般来说，应放置在安全、干燥、防潮的地方，避免长时间暴露在阳光下。如需使用，最好使用复印件而不是原件，以免丢失。
综上所述，办理(macewan学位证书)加拿大麦科文大学毕业证【微信：741003700 】是证明身份和学历的高价值文件。外观简单庄重，格式统一，包括重要的个人信息和发布日期。对持有人来说，妥善保管是非常重要的。
Mapping the Growth of Supermassive Black Holes as a Function of Galaxy Stella...
The growth of supermassive black holes is strongly linked to their galaxies. It has been shown that the population
mean black hole accretion rate (BHAR) primarily correlates with the galaxy stellar mass (Må) and redshift for the
general galaxy population. This work aims to provide the best measurements of BHAR as a function of Må and
redshift over ranges of 109.5 < Må < 1012 Me and z < 4. We compile an unprecedentedly large sample with 8000
active galactic nuclei (AGNs) and 1.3 million normal galaxies from nine high-quality survey fields following a
wedding cake design. We further develop a semiparametric Bayesian method that can reasonably estimate BHAR
and the corresponding uncertainties, even for sparsely populated regions in the parameter space. BHAR is
constrained by X-ray surveys sampling the AGN accretion power and UV-to-infrared multiwavelength surveys
sampling the galaxy population. Our results can independently predict the X-ray luminosity function (XLF) from
the galaxy stellar mass function (SMF), and the prediction is consistent with the observed XLF. We also try adding
external constraints from the observed SMF and XLF. We further measure BHAR for star-forming and quiescent
galaxies and show that star-forming BHAR is generally larger than or at least comparable to the quiescent BHAR.
Unified Astronomy Thesaurus concepts: Supermassive black holes (1663); X-ray active galactic nuclei (2035);
Galaxies (573)
The Limited Role of the Streaming Instability during Moon and Exomoon Formation
It is generally accepted that the Moon accreted from the disk formed by an impact between the proto-Earth and
impactor, but its details are highly debated. Some models suggest that a Mars-sized impactor formed a silicate
melt-rich (vapor-poor) disk around Earth, whereas other models suggest that a highly energetic impact produced a
silicate vapor-rich disk. Such a vapor-rich disk, however, may not be suitable for the Moon formation, because
moonlets, building blocks of the Moon, of 100 m–100 km in radius may experience strong gas drag and fall onto
Earth on a short timescale, failing to grow further. This problem may be avoided if large moonlets (?100 km)
form very quickly by streaming instability, which is a process to concentrate particles enough to cause gravitational
collapse and rapid formation of planetesimals or moonlets. Here, we investigate the effect of the streaming
instability in the Moon-forming disk for the first time and find that this instability can quickly form ∼100 km-sized
moonlets. However, these moonlets are not large enough to avoid strong drag, and they still fall onto Earth quickly.
This suggests that the vapor-rich disks may not form the large Moon, and therefore the models that produce vaporpoor disks are supported. This result is applicable to general impact-induced moon-forming disks, supporting the
previous suggestion that small planets (<1.6 R⊕) are good candidates to host large moons because their impactinduced disks would likely be vapor-poor. We find a limited role of streaming instability in satellite formation in an
impact-induced disk, whereas it plays a key role during planet formation.
Unified Astronomy Thesaurus concepts: Earth-moon system (436)
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
一比一原版美国佩斯大学毕业证如何办理
原版一模一样【微信：741003700 】【美国佩斯大学毕业证成绩单】【微信：741003700 】学位证，留信认证（真实可查，永久存档）原件一模一样纸张工艺/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。
本公司拥有海外各大学样板无数，能完美还原。
1:1完美还原海外各大学毕业材料上的工艺：水印，阴影底纹，钢印LOGO烫金烫银，LOGO烫金烫银复合重叠。文字图案浮雕、激光镭射、紫外荧光、温感、复印防伪等防伪工艺。材料咨询办理、认证咨询办理请加学历顾问Q/微741003700
【主营项目】
一.毕业证【q微741003700】成绩单、使馆认证、教育部认证、雅思托福成绩单、学生卡等！
二.真实使馆公证(即留学回国人员证明,不成功不收费)
三.真实教育部学历学位认证（教育部存档！教育部留服网站永久可查）
四.办理各国各大学文凭(一对一专业服务,可全程监控跟踪进度)
如果您处于以下几种情况：
◇在校期间，因各种原因未能顺利毕业……拿不到官方毕业证【q/微741003700】
◇面对父母的压力，希望尽快拿到；
◇不清楚认证流程以及材料该如何准备；
◇回国时间很长，忘记办理；
◇回国马上就要找工作，办给用人单位看；
◇企事业单位必须要求办理的
◇需要报考公务员、购买免税车、落转户口
◇申请留学生创业基金
留信网认证的作用:
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
6:个人职称评审加20分
7:个人信誉贷款加10分
8:在国家人才网主办的国家网络招聘大会中纳入资料，供国家高端企业选择人才
办理美国佩斯大学毕业证【微信：741003700 】外观非常简单，由纸质材料制成，上面印有校徽、校名、毕业生姓名、专业等信息。
办理美国佩斯大学毕业证【微信：741003700 】格式相对统一，各专业都有相应的模板。通常包括以下部分：
校徽：象征着学校的荣誉和传承。
校名:学校英文全称
授予学位：本部分将注明获得的具体学位名称。
毕业生姓名：这是最重要的信息之一，标志着该证书是由特定人员获得的。
颁发日期：这是毕业正式生效的时间，也代表着毕业生学业的结束。
其他信息：根据不同的专业和学位，可能会有一些特定的信息或章节。
办理美国佩斯大学毕业证【微信：741003700 】价值很高，需要妥善保管。一般来说，应放置在安全、干燥、防潮的地方，避免长时间暴露在阳光下。如需使用，最好使用复印件而不是原件，以免丢失。
综上所述，办理美国佩斯大学毕业证【微信：741003700 】是证明身份和学历的高价值文件。外观简单庄重，格式统一，包括重要的个人信息和发布日期。对持有人来说，妥善保管是非常重要的。
SDSS1335+0728: The awakening of a ∼ 106M⊙ black hole⋆
Context. The early-type galaxy SDSS J133519.91+072807.4 (hereafter SDSS1335+0728), which had exhibited no prior optical variations during the preceding two decades, began showing significant nuclear variability in the Zwicky Transient Facility (ZTF) alert stream from December 2019 (as ZTF19acnskyy). This variability behaviour, coupled with the host-galaxy properties, suggests that SDSS1335+0728 hosts a ∼ 106M⊙ black hole (BH) that is currently in the process of ‘turning on’. Aims. We present a multi-wavelength photometric analysis and spectroscopic follow-up performed with the aim of better understanding the origin of the nuclear variations detected in SDSS1335+0728. Methods. We used archival photometry (from WISE, 2MASS, SDSS, GALEX, eROSITA) and spectroscopic data (from SDSS and LAMOST) to study the state of SDSS1335+0728 prior to December 2019, and new observations from Swift, SOAR/Goodman, VLT/X-shooter, and Keck/LRIS taken after its turn-on to characterise its current state. We analysed the variability of SDSS1335+0728 in the X-ray/UV/optical/mid-infrared range, modelled its spectral energy distribution prior to and after December 2019, and studied the evolution of its UV/optical spectra. Results. From our multi-wavelength photometric analysis, we find that: (a) since 2021, the UV flux (from Swift/UVOT observations) is four times brighter than the flux reported by GALEX in 2004; (b) since June 2022, the mid-infrared flux has risen more than two times, and the W1−W2 WISE colour has become redder; and (c) since February 2024, the source has begun showing X-ray emission. From our spectroscopic follow-up, we see that (i) the narrow emission line ratios are now consistent with a more energetic ionising continuum; (ii) broad emission lines are not detected; and (iii) the [OIII] line increased its flux ∼ 3.6 years after the first ZTF alert, which implies a relatively compact narrow-line-emitting region. Conclusions. We conclude that the variations observed in SDSS1335+0728 could be either explained by a ∼ 106M⊙ AGN that is just turning on or by an exotic tidal disruption event (TDE). If the former is true, SDSS1335+0728 is one of the strongest cases of an AGNobserved in the process of activating. If the latter were found to be the case, it would correspond to the longest and faintest TDE ever observed (or another class of still unknown nuclear transient). Future observations of SDSS1335+0728 are crucial to further understand its behaviour. Key words. galaxies: active– accretion, accretion discs– galaxies: individual: SDSS J133519.91+072807.4
Post translation modification by Suyash Garg
overview of PTM helps to the students who wants to clear their basics about it.
Gadgets for management of stored product pests_Dr.UPR.pdf
Insectsplayamajorroleinthedeteriorationoffoodgrainscausingbothquantitativeandqualitativelosses
Wellprovedthatnogranariescanbefilledwithgrainswithoutinsectsastheharvestedproducecontainegg(or)larvae(or)pupae(or)adultinsectinthembecauseoffieldcarryoverinfestationwhichcannotbeavoidedindevelopingcountrieslikeIndia
Simpletechnologiesfortimelydetectionofinsectsinthestoredproduceandtherebyplantimelycontrolmeasures
BIRDS DIVERSITY OF SOOTEA BISWANATH ASSAM.ppt.pptx
Ahota Beel, nestled in Sootea Biswanath Assam , is celebrated for its extraordinary diversity of bird species. This wetland sanctuary supports a myriad of avian residents and migrants alike. Visitors can admire the elegant flights of migratory species such as the Northern Pintail and Eurasian Wigeon, alongside resident birds including the Asian Openbill and Pheasant-tailed Jacana. With its tranquil scenery and varied habitats, Ahota Beel offers a perfect haven for birdwatchers to appreciate and study the vibrant birdlife that thrives in this natural refuge.
Synopsis presentation VDR gene polymorphism and anemia (2).pptx
I am the PhD scholar of FND department, Assam down town University
Evidence of Jet Activity from the Secondary Black Hole in the OJ 287 Binary S...
Wereport the study of a huge optical intraday flare on 2021 November 12 at 2 a.m. UT in the blazar OJ287. In the binary black hole model, it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact based on a prediction made 8 yr earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R–I spectral index by 1.0 ±0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary BH. We then ask why we have not seen this phenomenon before. We show that OJ287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability using the Krakow data set of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In machine-readable Tables 1 and 2, we give the full orbit-linked historical light curve of OJ287 as well as the dense monitoring sample of Krakow.
Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDS
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
Embracing Deep Variability For Reproducibility and Replicability
Embracing Deep Variability For Reproducibility and ReplicabilityUniversity of Rennes, INSA Rennes, Inria/IRISA, CNRS
Embracing Deep Variability For Reproducibility and Replicability
Abstract: Reproducibility (aka determinism in some cases) constitutes a fundamental aspect in various fields of computer science, such as floating-point computations in numerical analysis and simulation, concurrency models in parallelism, reproducible builds for third parties integration and packaging, and containerization for execution environments. These concepts, while pervasive across diverse concerns, often exhibit intricate inter-dependencies, making it challenging to achieve a comprehensive understanding. In this short and vision paper we delve into the application of software engineering techniques, specifically variability management, to systematically identify and explicit points of variability that may give rise to reproducibility issues (eg language, libraries, compiler, virtual machine, OS, environment variables, etc). The primary objectives are: i) gaining insights into the variability layers and their possible interactions, ii) capturing and documenting configurations for the sake of reproducibility, and iii) exploring diverse configurations to replicate, and hence validate and ensure the robustness of results. By adopting these methodologies, we aim to address the complexities associated with reproducibility and replicability in modern software systems and environments, facilitating a more comprehensive and nuanced perspective on these critical aspects.
https://hal.science/hal-04582287
MICROBIAL INTERACTION PPT/ MICROBIAL INTERACTION AND THEIR TYPES // PLANT MIC...
MICROBIAL INTERACTION PPT/ MICROBIAL INTERACTION AND THEIR TYPES // PLANT MIC...ABHISHEK SONI NIMT INSTITUTE OF MEDICAL AND PARAMEDCIAL SCIENCES , GOVT PG COLLEGE NOIDA
Microbial interaction
Microorganisms interacts with each other and can be physically associated with another organisms in a variety of ways.
One organism can be located on the surface of another organism as an ectobiont or located within another organism as endobiont.
Microbial interaction may be positive such as mutualism, proto-cooperation, commensalism or may be negative such as parasitism, predation or competition
Types of microbial interaction
Positive interaction: mutualism, proto-cooperation, commensalism
Negative interaction: Ammensalism (antagonism), parasitism, predation, competition
I. Mutualism:
It is defined as the relationship in which each organism in interaction gets benefits from association. It is an obligatory relationship in which mutualist and host are metabolically dependent on each other.
Mutualistic relationship is very specific where one member of association cannot be replaced by another species.
Mutualism require close physical contact between interacting organisms.
Relationship of mutualism allows organisms to exist in habitat that could not occupied by either species alone.
Mutualistic relationship between organisms allows them to act as a single organism.
Examples of mutualism:
i. Lichens:
Lichens are excellent example of mutualism.
They are the association of specific fungi and certain genus of algae. In lichen, fungal partner is called mycobiont and algal partner is called
II. Syntrophism:
It is an association in which the growth of one organism either depends on or improved by the substrate provided by another organism.
In syntrophism both organism in association gets benefits.
Compound A
Utilized by population 1
Compound B
Utilized by population 2
Compound C
utilized by both Population 1+2
Products
In this theoretical example of syntrophism, population 1 is able to utilize and metabolize compound A, forming compound B but cannot metabolize beyond compound B without co-operation of population 2. Population 2is unable to utilize compound A but it can metabolize compound B forming compound C. Then both population 1 and 2 are able to carry out metabolic reaction which leads to formation of end product that neither population could produce alone.
Examples of syntrophism:
i. Methanogenic ecosystem in sludge digester
Methane produced by methanogenic bacteria depends upon interspecies hydrogen transfer by other fermentative bacteria.
Anaerobic fermentative bacteria generate CO2 and H2 utilizing carbohydrates which is then utilized by methanogenic bacteria (Methanobacter) to produce methane.
ii. Lactobacillus arobinosus and Enterococcus faecalis:
In the minimal media, Lactobacillus arobinosus and Enterococcus faecalis are able to grow together but not alone.
The synergistic relationship between E. faecalis and L. arobinosus occurs in which E. faecalis require folic acid
Signatures of wave erosion in Titan’s coasts
The shorelines of Titan’s hydrocarbon seas trace flooded erosional landforms such as river valleys; however, it isunclear whether coastal erosion has subsequently altered these shorelines. Spacecraft observations and theo-retical models suggest that wind may cause waves to form on Titan’s seas, potentially driving coastal erosion,but the observational evidence of waves is indirect, and the processes affecting shoreline evolution on Titanremain unknown. No widely accepted framework exists for using shoreline morphology to quantitatively dis-cern coastal erosion mechanisms, even on Earth, where the dominant mechanisms are known. We combinelandscape evolution models with measurements of shoreline shape on Earth to characterize how differentcoastal erosion mechanisms affect shoreline morphology. Applying this framework to Titan, we find that theshorelines of Titan’s seas are most consistent with flooded landscapes that subsequently have been eroded bywaves, rather than a uniform erosional process or no coastal erosion, particularly if wave growth saturates atfetch lengths of tens of kilometers.
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- 1. BASIC INTERACTIONS BETWEEN X RAYS AND MATTER
- 2. Atoms are bound into molecules by electrons in the outermost shell.x ray photons interact either with the orbital electrons or with the nucleus In the diagnostic range, the interactions are with orbital electrons Interaction between X-rays and matter •Coherent Scattering •Photoelectric effect •Compton Scattering •Pair Production •Photodisintegration
- 6. Low energy photons,only scattering,no ionisation and only little energy loss,
- 7. • Two types of coherent scattering • Thomson scattering-a single electron is involved in the interaction • Rayleigh scattering-results from a cooperative interaction with all electrons of an atom
- 8. • Rayleigh Scattering (Coherent Scattering) 1 . Photons are scattered by bound electrons 2. Atoms are neither excited or ionized 3. Scattering from different parts of electron cloud - coherent scattering
- 10. The tighter an electron is bound,more likely it is involved in photoelectric reaxn
- 14. • The charecteristic radiation– secondary radiation • Only iodine and barium in diagnostic radiology emit charecteristic radiation energetic enough to leave the patient and fog film • Application of photoelectric effect-produces images of good quality becoz there is no scatter and it enhances tissue contrast • But patient gets more radiation
- 15. Compton scattering • Almost all scatter in diagnostic radiology comes from compton scatter • Rel high energy incident photon strikes a free outer shell electron and ejects it • The photon is deflected.part of its energy goes to the electron.rest is retained.the amount retained dep on initial energy and angle of deflection off the electron • At narrow angles of deflection,the scattered photon retains more of its org energy
- 17. Compton scatter
- 19. The most significant object producing scattered radiation in an x-ray procedure is the patient's body. The portion of the patient's body that is within the primary x-ray beam becomes the actual source of scattered radiation. This has two undesirable consequences. The scattered radiation that continues in the forward . direction and reaches the image receptor decreases the quality (contrast) of the image; the radiation that is scattered from the patient is the predominant source of radiation exposure to the personnel conducting the examination.
- 21. Pair production and photo disintegration do not occur in diagnostic energy range A photon with Energy > 1.02Mev might completely disappear under the production of an electron and a positron (electron with positive charge) Pair production