Ulysses achieved a solar orbit with an inclination of 80.200 , perihelion of 1.34 AU, aphelion of 5.4 AU and a period of 6.2 years. By comparing observations taken over nearly all heliolatitudes and two different intervals covering the same radial distances, we are able to separate the radial and latitudinal variations in the solar wind. This paper describes the detailed results of the studies devoted to the solar activity impact on the Earth’s upper atmosphere and ionosphere. The methods used in this study are based on the data driven from the Ulysses spacecraft. The primary objective of the Ulysses solar wind plasma investigation uses SWOOPS (Solar Wind Observations over the Poles of the Sun) instrument to investigate and establish bulk flow parameters and internal state conditions of the solar wind as a function of solar latitude. The electron temperature Te and the electron density Ne are found to exhibit a sharp enhancement during the ascending half of the solar cycle 23 (1996 – 2004)
On the possibility of through passage of asteroid bodies across the Earth’s a...Sérgio Sacani
We have studied the conditions of through passage of asteroids with diameters 200, 100, and
50 m, consisting of three types of materials – iron, stone, and water ice, across the Earth’s
atmosphere with a minimum trajectory altitude in the range 10–15 km. The conditions of this
passage with a subsequent exit into outer space with the preservation of a substantial fraction
of the initial mass have been found. The results obtained support our idea explaining one of the
long-standing problems of astronomy – the Tunguska phenomenon, which has not received
reasonable and comprehensive interpretations to date. We argue that the Tunguska event was
caused by an iron asteroid body, which passed through the Earth’s atmosphere and continued
to the near-solar orbit.
High-resolution UV/Optical/IR Imaging of Jupiter in 2016–2019Sérgio Sacani
Imaging observations of Jupiter with high spatial resolution were acquired beginning in 2016, with a cadence of 53
days to coincide with atmospheric observations of the Juno spacecraft during each perijove pass. The Wide Field
Camera 3 (WFC3) aboard the Hubble Space Telescope (HST) collected Jupiter images from 236 to 925 nm in 14
filters. The Near-Infrared Imager (NIRI) at Gemini North imaged Jovian thermal emission using a lucky-imaging
approach (co-adding the sharpest frames taken from a sequence of short exposures), using the M′ filter at 4.7 μm.
We discuss the data acquisition and processing and an archive collection that contains the processed WFC3 and
NIRI data (doi:10.17909/T94T1H). Zonal winds remain steady over time at most latitudes, but significant
evolution of the wind profile near 24°N in 2016 and near 15°S in 2017 was linked with convective superstorm
eruptions. Persistent mesoscale waves were seen throughout the 2016–2019 period. We link groups of lightning
flashes observed by the Juno team with water clouds in a large convective plume near 15°S and in cyclones near
35°N–55°N. Thermal infrared maps at the 10.8 micron wavelength obtained at the Very Large Telescope show
consistent high brightness temperature anomalies, despite a diversity of aerosol properties seen in the HST data.
Both WFC3 and NIRI imaging reveal depleted aerosols consistent with downwelling around the periphery of the
15°S storm, which was also observed by the Atacama Large Millimeter/submillimeter Array. NIRI imaging of
the Great Red Spot shows that locally reduced cloud opacity is responsible for dark features within the vortex. The
HST data maps multiple concentric polar hoods of high-latitude hazes.
A study on severe geomagnetic storms and earth’s magnetic field H variations,...IJERA Editor
For our study, we have selected ten severe geomagnetic storms. Which occurred during the years 1994 to 2015. Here great geomagnetic storm of Dst index from -422 nT to -17 nT are taken. These storms are significant not only because of the extremely high magnetic activity but also due to their great impact on the geomagnetosphere. We have studied the relation between severe geomagnetic storms with Earth’s magnetic field in horizontal component (H constant) and also studied the relation between Dst index with sunspots number. The H constant data from Kyoto data centre and Dst index, Ap index, Kp index from OMNI data centre. We have found that the Dst is at very lowest level in this storm period, Ap index Kp index are increased in severe geomagnetic storm period and H Constant is at very lowest level in storm period. We have found that geomagnetic storms were induced to form the cyclones within 29 days. The Sunspots numbers are increased to induce to geomagnetic storm within 5 – 15 days
On the possibility of through passage of asteroid bodies across the Earth’s a...Sérgio Sacani
We have studied the conditions of through passage of asteroids with diameters 200, 100, and
50 m, consisting of three types of materials – iron, stone, and water ice, across the Earth’s
atmosphere with a minimum trajectory altitude in the range 10–15 km. The conditions of this
passage with a subsequent exit into outer space with the preservation of a substantial fraction
of the initial mass have been found. The results obtained support our idea explaining one of the
long-standing problems of astronomy – the Tunguska phenomenon, which has not received
reasonable and comprehensive interpretations to date. We argue that the Tunguska event was
caused by an iron asteroid body, which passed through the Earth’s atmosphere and continued
to the near-solar orbit.
High-resolution UV/Optical/IR Imaging of Jupiter in 2016–2019Sérgio Sacani
Imaging observations of Jupiter with high spatial resolution were acquired beginning in 2016, with a cadence of 53
days to coincide with atmospheric observations of the Juno spacecraft during each perijove pass. The Wide Field
Camera 3 (WFC3) aboard the Hubble Space Telescope (HST) collected Jupiter images from 236 to 925 nm in 14
filters. The Near-Infrared Imager (NIRI) at Gemini North imaged Jovian thermal emission using a lucky-imaging
approach (co-adding the sharpest frames taken from a sequence of short exposures), using the M′ filter at 4.7 μm.
We discuss the data acquisition and processing and an archive collection that contains the processed WFC3 and
NIRI data (doi:10.17909/T94T1H). Zonal winds remain steady over time at most latitudes, but significant
evolution of the wind profile near 24°N in 2016 and near 15°S in 2017 was linked with convective superstorm
eruptions. Persistent mesoscale waves were seen throughout the 2016–2019 period. We link groups of lightning
flashes observed by the Juno team with water clouds in a large convective plume near 15°S and in cyclones near
35°N–55°N. Thermal infrared maps at the 10.8 micron wavelength obtained at the Very Large Telescope show
consistent high brightness temperature anomalies, despite a diversity of aerosol properties seen in the HST data.
Both WFC3 and NIRI imaging reveal depleted aerosols consistent with downwelling around the periphery of the
15°S storm, which was also observed by the Atacama Large Millimeter/submillimeter Array. NIRI imaging of
the Great Red Spot shows that locally reduced cloud opacity is responsible for dark features within the vortex. The
HST data maps multiple concentric polar hoods of high-latitude hazes.
A study on severe geomagnetic storms and earth’s magnetic field H variations,...IJERA Editor
For our study, we have selected ten severe geomagnetic storms. Which occurred during the years 1994 to 2015. Here great geomagnetic storm of Dst index from -422 nT to -17 nT are taken. These storms are significant not only because of the extremely high magnetic activity but also due to their great impact on the geomagnetosphere. We have studied the relation between severe geomagnetic storms with Earth’s magnetic field in horizontal component (H constant) and also studied the relation between Dst index with sunspots number. The H constant data from Kyoto data centre and Dst index, Ap index, Kp index from OMNI data centre. We have found that the Dst is at very lowest level in this storm period, Ap index Kp index are increased in severe geomagnetic storm period and H Constant is at very lowest level in storm period. We have found that geomagnetic storms were induced to form the cyclones within 29 days. The Sunspots numbers are increased to induce to geomagnetic storm within 5 – 15 days
1980 öncesi deprem istasyon sayısı Türkiye'de herhalde 50'den azdı ve bu nedenle deprem istatistiği çalışmaları Türkiye boyunca çok büyük alanlara bölünerek yapılmış. Okla gösterdiğim yerlerde magnitüd aralığı çok yetersiz. Bu çalışmada, 4x4 şeklinde dilimleme yapılmış. 400kmx400 km olarak dilimlere ayrılarak yapılmış. Veri olmadığı zaman mecbur ALANI büyütmek zorunda kalıyorsunuz... bu nedenle Makro-İstatistik İnceleme yapılmış oluyor.a/b oranını çalışmalarımda hiç kullanmadım fakat bana kalırsa yararlı bir parametre olarak görünüyor. Bir yıl içinde olması beklenen en büyük deprem büyüklüğünü veriyor. Buna göre bu çalışmada, bir yıl içinde beklenen en büyük deprem M=5 bulunmuş ve alan 39 E ve 41 B arasında bir yere denk geliyor... muhtemelen Karlıova Üçlü Bileşimi çevresi olabilir.
Storm in teacup_a_radio_quiet_quasar_with_radio_emitting_bubblesSérgio Sacani
Artigo descreve descoberta feita com o VLA de uma tempestade nas ondas de rádio em uma galáxia até então calma, o que traz conclusões sobre a evolução das galáxias.
Um dos artigos da edição especial da revista Science, mostrando as alterações nas propriedades do cometa Churyumov-Gerasimenko, à medida que ele se aproxima do Sol.
Interrelation of Extreme Climatic Events with Air Masses in Antakya (Hatay, T...inventionjournals
Due to its mechanism and effects, climatic events have been significant facts for humanbeings all times. In this study,the interrelation between the extreme climatic events in Antakya, air masses and, their routes was examined. Using the data related with extreme climatic events received from Turkish State Meteorological Service (TSMS) and NOAA HYSPLIT model (Hybrid Single-Particle Lagrangian Integrated Trajectory), it was aimed to determine the relation between air masses their routes, and the extreme climatic events in Antakya. The routes of air masses that generate the extreme climatic conditions in 96 hours back trajectory plane at 500, 1500 and 3000m heights, according to HYSPLIT model, are given to enable the comparison in terms of altitude and event. During the analysis carried out for various climatic parameters, it was determined that Siberian and Azore anticyclone played an active role for maximum and minimum temperatures, maximum precipitation, and highest snow thickness and during fastest wind periods. The field of study was influenced by the continental polar air mass during the periods of heavy colds in particular, when Azore dynamic cyclone was dominant the highest pluvial period as a flood disaster has been occurred. Furthermore, it was understood that extreme climatic conditions, in particular maximum precipitation periods resulted in severe material damages in the territory
Micro-Tensile Behavior of AA7020/Carbon Black Nanoparticle Metal Matrix Compo...researchinventy
The micro-tensile behavior of AA7020/carbon black nanoparticle composites was examined by using finite element analysis and representative volume element models for three different volume fractions. The uniform distributions of the nanoparticles were constructed to produce a representative volume element of the composites. The predicted mechanical properties and overall tensile stress-strain by finite element analysis corresponded well to the experimental results at the elastic region and near the yield surface, but the model slightly overestimated the strength of the composites at higher stress. This deviation possibly occurs from micromechanical factors, which were not considered in the RVE models. In contrast to FE analysis, fracture of the nanoparticle-matrix debonding occurred because of large localized stress. In the case of a high applied load, non-linear behavior of reinforcements and interfacial strength should be considered to obtain accurate results.
Comparative study of fluoride with chemical parameters of brine solutions, sa...researchinventy
Variations in the fluoride content of saline water, salt and pan soil from nine different salt pans located at the East Coast belt of Tamil Nadu have been documented. Fluoride which is non-degradable and persists in the environment was estimated by Zirconyl-alizarin method. The fluoride level varied from 0.6 to 1.7 ppm. Fluoride level in the salt of Marakkanam (Bore well) was found to be slightly higher than other salt pans.The chemical parameters which are used to study the level of fluoride in saline waters included chloride, sulphate, sodium, magnesium, potassium and calcium.
1980 öncesi deprem istasyon sayısı Türkiye'de herhalde 50'den azdı ve bu nedenle deprem istatistiği çalışmaları Türkiye boyunca çok büyük alanlara bölünerek yapılmış. Okla gösterdiğim yerlerde magnitüd aralığı çok yetersiz. Bu çalışmada, 4x4 şeklinde dilimleme yapılmış. 400kmx400 km olarak dilimlere ayrılarak yapılmış. Veri olmadığı zaman mecbur ALANI büyütmek zorunda kalıyorsunuz... bu nedenle Makro-İstatistik İnceleme yapılmış oluyor.a/b oranını çalışmalarımda hiç kullanmadım fakat bana kalırsa yararlı bir parametre olarak görünüyor. Bir yıl içinde olması beklenen en büyük deprem büyüklüğünü veriyor. Buna göre bu çalışmada, bir yıl içinde beklenen en büyük deprem M=5 bulunmuş ve alan 39 E ve 41 B arasında bir yere denk geliyor... muhtemelen Karlıova Üçlü Bileşimi çevresi olabilir.
Storm in teacup_a_radio_quiet_quasar_with_radio_emitting_bubblesSérgio Sacani
Artigo descreve descoberta feita com o VLA de uma tempestade nas ondas de rádio em uma galáxia até então calma, o que traz conclusões sobre a evolução das galáxias.
Um dos artigos da edição especial da revista Science, mostrando as alterações nas propriedades do cometa Churyumov-Gerasimenko, à medida que ele se aproxima do Sol.
Interrelation of Extreme Climatic Events with Air Masses in Antakya (Hatay, T...inventionjournals
Due to its mechanism and effects, climatic events have been significant facts for humanbeings all times. In this study,the interrelation between the extreme climatic events in Antakya, air masses and, their routes was examined. Using the data related with extreme climatic events received from Turkish State Meteorological Service (TSMS) and NOAA HYSPLIT model (Hybrid Single-Particle Lagrangian Integrated Trajectory), it was aimed to determine the relation between air masses their routes, and the extreme climatic events in Antakya. The routes of air masses that generate the extreme climatic conditions in 96 hours back trajectory plane at 500, 1500 and 3000m heights, according to HYSPLIT model, are given to enable the comparison in terms of altitude and event. During the analysis carried out for various climatic parameters, it was determined that Siberian and Azore anticyclone played an active role for maximum and minimum temperatures, maximum precipitation, and highest snow thickness and during fastest wind periods. The field of study was influenced by the continental polar air mass during the periods of heavy colds in particular, when Azore dynamic cyclone was dominant the highest pluvial period as a flood disaster has been occurred. Furthermore, it was understood that extreme climatic conditions, in particular maximum precipitation periods resulted in severe material damages in the territory
Micro-Tensile Behavior of AA7020/Carbon Black Nanoparticle Metal Matrix Compo...researchinventy
The micro-tensile behavior of AA7020/carbon black nanoparticle composites was examined by using finite element analysis and representative volume element models for three different volume fractions. The uniform distributions of the nanoparticles were constructed to produce a representative volume element of the composites. The predicted mechanical properties and overall tensile stress-strain by finite element analysis corresponded well to the experimental results at the elastic region and near the yield surface, but the model slightly overestimated the strength of the composites at higher stress. This deviation possibly occurs from micromechanical factors, which were not considered in the RVE models. In contrast to FE analysis, fracture of the nanoparticle-matrix debonding occurred because of large localized stress. In the case of a high applied load, non-linear behavior of reinforcements and interfacial strength should be considered to obtain accurate results.
Comparative study of fluoride with chemical parameters of brine solutions, sa...researchinventy
Variations in the fluoride content of saline water, salt and pan soil from nine different salt pans located at the East Coast belt of Tamil Nadu have been documented. Fluoride which is non-degradable and persists in the environment was estimated by Zirconyl-alizarin method. The fluoride level varied from 0.6 to 1.7 ppm. Fluoride level in the salt of Marakkanam (Bore well) was found to be slightly higher than other salt pans.The chemical parameters which are used to study the level of fluoride in saline waters included chloride, sulphate, sodium, magnesium, potassium and calcium.
Conceptualization of a Domain Specific Simulator for Requirements Prioritizationresearchinventy
This paper conceptualizes a domain specific simulator for requirements prioritization; its aims at helping to identify appropriate prioritization strategies for a project in hand. The possible existing scenarios are difficult to analyze; they involve different variables, like the selection of: stakeholders (their availability, expertise, and importance); prioritization criteria; and prioritization methods. To demonstrate the feasibility of the proposed simulator elements, a well established general purpose simulator, called Arena, was used. The results demonstrate that, it is possible to build the suggested scenarios in order to study and make inferences about the prioritization strategies.
Improved Stability of Formate Dehydrogenase by Coating with Didodecyldimethyl...researchinventy
Hydrophilic formate dehydrogenase (FDH) from candida boidinii was chemically modified by coating it with didodecyldimethylammonium bromide (DDAB). This coating changed the phase behavior of the enzyme, making it highly soluble in hydrophobic solvents and thereby offering the chance for biphasic enzyme recycling from hydrophilic substrates and products. Different coating procedures of FDH with DDAB were investigated and all proved suitable for efficient coating of the enzyme’s outer surface. A 50 mM Tris- (hydroxymethyl)-amminomethan (tris) buffer at pH 8 was chosen to make DDAB soluble and avoid aggregation. The reaction of NAD+ with uncoated and coated FDH to NADH and CO2 was monitored by UV-vis spectroscopy and kinetic parameters (rmax, Km, KI , EA) for the the FDH were determined. The coated enzyme resulted in a lower relative initial activity between 40-60% compared to the uncoated one. The stability of the coated enzyme (FDH*) was improved significantly and remained stable in long-term experiments, resulting in a deactivation rate kD smaller than 3% per day and a half-life time t1/2largerthan 23 days, while the deactivation rate of the uncoated enzyme was 260% per daywitha t1/2of 0.3 days. Both activation energies were similar, with 42 kJ mol-1 for the coated and 48 kJ mol-1 for the uncoated enzyme.This result suggests that there is not significant transport resistance originating from the DDAB coating layer. The reason for the significantly lower activity of the coated FDH probably stems from accumulation of formed CO2 in the coating layer, thereby preventing high equilibrium conversions
The Acute Effects Of Vibroacoustically-Induced Microvibrations On EEG Activit...researchinventy
A 7-13 c/s mechanographic signal (amplitude 1-5μV) is detectable over relaxed limbs, phenomenon termed microvibration (MV). Exposure to mechanographic signals, low frequency noise, on other side, results in vibroacoustic disease. The aim of this study was to investigate the acute effects of vibroacoustically-induced MV in regio nuchae (vibroacoustic device Vitafon, St. Petersburg, Russian Federation) using four different modes of MV of specific amplitude (2.8 μm - 12.3 μm) and frequency (30 Hz – 18 kHz) on native undulating electrical CNS activity (EEG registration) in the adult rats. The experiments were performed on Wistar male rats and were divided into control and experimental groups. Rats subjected to the same experimental protocol, but with vibroacoustic treatment switched off, served as controls. EEG activity was registered during application of vibroacoustic MV and following was observed regardless of working regime: none of the graphoelements indicating hyperexcitability; there were no reduction in vigilance; beta rhythm and moderate transition alpha in beta rhythm were observed. Slightly override the beta waves in relation to alpha EEG band, under the stimulus of vibroacoustically-induced microvibration by Vitafon, suggests that mental alertness increased as well as focused attention, with no signs of hyperexcitability in rats
How to Build a Dynamic Social Media PlanPost Planner
Stop guessing and wasting your time on networks and strategies that don’t work!
Join Rebekah Radice and Katie Lance to learn how to optimize your social networks, the best kept secrets for hot content, top time management tools, and much more!
Watch the replay here: bit.ly/socialmedia-plan
http://inarocket.com
Learn BEM fundamentals as fast as possible. What is BEM (Block, element, modifier), BEM syntax, how it works with a real example, etc.
Lightning Talk #9: How UX and Data Storytelling Can Shape Policy by Mika Aldabaux singapore
How can we take UX and Data Storytelling out of the tech context and use them to change the way government behaves?
Showcasing the truth is the highest goal of data storytelling. Because the design of a chart can affect the interpretation of data in a major way, one must wield visual tools with care and deliberation. Using quantitative facts to evoke an emotional response is best achieved with the combination of UX and data storytelling.
Content personalisation is becoming more prevalent. A site, it's content and/or it's products, change dynamically according to the specific needs of the user. SEO needs to ensure we do not fall behind of this trend.
Succession “Losers”: What Happens to Executives Passed Over for the CEO Job?
By David F. Larcker, Stephen A. Miles, and Brian Tayan
Stanford Closer Look Series
Overview:
Shareholders pay considerable attention to the choice of executive selected as the new CEO whenever a change in leadership takes place. However, without an inside look at the leading candidates to assume the CEO role, it is difficult for shareholders to tell whether the board has made the correct choice. In this Closer Look, we examine CEO succession events among the largest 100 companies over a ten-year period to determine what happens to the executives who were not selected (i.e., the “succession losers”) and how they perform relative to those who were selected (the “succession winners”).
We ask:
• Are the executives selected for the CEO role really better than those passed over?
• What are the implications for understanding the labor market for executive talent?
• Are differences in performance due to operating conditions or quality of available talent?
• Are boards better at identifying CEO talent than other research generally suggests?
Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun CoronaSérgio Sacani
Arch-like loop structures filled with million Kelvin hot plasma form the building blocks of the quiet-Sun corona.
Both high-resolution observations and magnetoconvection simulations show the ubiquitous presence of magnetic
fields on the solar surface on small spatial scales of ∼100 km. However, the question of how exactly these quietSun coronal loops originate from the photosphere and how the magnetic energy from the surface is channeled to
heat the overlying atmosphere is a long-standing puzzle. Here we report high-resolution photospheric magnetic
field and coronal data acquired during the second science perihelion of Solar Orbiter that reveal a highly dynamic
magnetic landscape underlying the observed quiet-Sun corona. We found that coronal loops often connect to
surface regions that harbor fleeting weaker, mixed-polarity magnetic field patches structured on small spatial
scales, and that coronal disturbances could emerge from these areas. We suggest that weaker magnetic fields with
fluxes as low as 1015 Mx and/or those that evolve on timescales less than 5 minutes are crucial to understanding
the coronal structuring and dynamics.
PHY 1301, Physics I 1 Course Learning Outcomes forajoy21
PHY 1301, Physics I 1
Course Learning Outcomes for Unit VII
Upon completion of this unit, students should be able to:
7. Describe fundamental thermodynamic concepts.
7.1 Explain the various heat transfer mechanisms with practical examples.
7.2 Recognize the ideal gas law and apply it to daily life.
7.3 Describe the relationship between kinetic energy and the Kelvin temperature.
Course/Unit
Learning Outcomes
Learning Activity
7.1
Unit Lesson
Chapter 13
Chapter 14
Unit VII PowerPoint Presentation
7.2
Unit Lesson
Chapter 13
Chapter 14
Unit VII PowerPoint Presentation
7.3
Unit Lesson
Chapter 13
Chapter 14
Unit VII PowerPoint Presentation
Required Unit Resources
Chapter 13: The Transfer of Heat, pp. 360–379
Chapter 14: The Ideal Gas Law and Kinetic Theory, pp. 380–400
Unit Lesson
UNIT VII STUDY GUIDE
Heat Mechanism and Kinetic Theory
PHY 1301, Physics I 2
UNIT x STUDY GUIDE
Title
The Three Methods to Transfer Heat
The above image illustrates the three heat transfer methods. The sun heats the Earth by radiation, the
surface of the Earth heats the air by conduction, and the warm air rises by convection.
What is heat? Heat is energy that moves from a high-temperature object to a low-temperature object. Its unit
is the Joule (J), but sometimes it is measured with the kilocalorie (kcal). The conversion factor between the
two units is 1 kcal = 4186 J. The transfer of heat is processed by the following mechanisms.
Conduction is the process in which heat is transferred through a material. The atoms or molecules in a hotter
part of the material have greater energy than those in a colder part of the material, and thus the energy is
transferred from the hotter place to the colder place. Notice that the bulk motion of the material has nothing to
do with this process. You can easily find examples of conduction. A radiator in your house is one of them. If
you put an object on the radiator, the object will become warmer. Another example is when you pour the
brewed hot coffee into a cold cup; the heat from the hot coffee makes the cup itself hot.
The heat Q conducted during a time t through a bar of length L and cross-sectional area A is expressed as
Q = kA (dT) t / L. Here, k is thermal conductivity, and it depends on the substance; dT is the temperature
difference between the higher temperature and the lower temperature of the bar.
Convection is the process in which heat is transferred by the bulk motion of a fluid. According to the ideal gas
law for constant pressure, the volume (V) is proportional to the temperature (T). V increases as T increases,
and the density decreases within the constant mass. Warm air rises and cooler air goes down; this circulation
makes the energy transported. The generated energy from the center of the sun is transported by convection
near the photosphere. Cool gas sinks while bubbles of hot gas rise. There is a patchwork patte ...
Jupiter’s interior and deep atmosphere: The initial pole-to-pole passes with ...Sérgio Sacani
On 27 August 2016, the Juno spacecraft acquired science observations of Jupiter,
passing less than 5000 kilometers above the equatorial cloud tops. Images of Jupiter’s
poles show a chaotic scene, unlike Saturn’s poles. Microwave sounding reveals weather
features at pressures deeper than 100 bars, dominated by an ammonia-rich, narrow
low-latitude plume resembling a deeper, wider version of Earth’s Hadley cell. Near-infrared
mapping reveals the relative humidity within prominent downwelling regions. Juno’s
measured gravity field differs substantially from the last available estimate and is one
order of magnitude more precise. This has implications for the distribution of heavy
elements in the interior, including the existence and mass of Jupiter’s core. The observed
magnetic field exhibits smaller spatial variations than expected, indicative of a rich
harmonic content.
Magnetic field and_wind_of_kappa_ceti_towards_the_planetary_habitability_of_t...Sérgio Sacani
We report magnetic field measurements for κ
1 Cet, a proxy of the young Sun when life arose on Earth. We carry out an analysis
of the magnetic properties determined from spectropolarimetric observations and reconstruct its large-scale surface magnetic
field to derive the magnetic environment, stellar winds and particle flux permeating the interplanetary medium around κ
1 Cet.
Our results show a closer magnetosphere and mass-loss rate of M˙ = 9.7 × 10−13 M yr−1
, i.e., a factor 50 times larger than the
current solar wind mass-loss rate, resulting in a larger interaction via space weather disturbances between the stellar wind and
a hypothetical young-Earth analogue, potentially affecting the planet’s habitability. Interaction of the wind from the young Sun
with the planetary ancient magnetic field may have affected the young Earth and its life conditions.
Earth’s magnetic field, called the geomagnetic field, is the magnetic field that extends from the earth’s interior out into space. When the solar wind, a stream of charged particles emanating from the sun, interacts with the earth’s magnetic field, most of them are trapped in the Van Allen radiation belt and protects the earth from the harmful charged particles and cosmic rays. The earth exhibits like a bar magnet in which the North geographic pole actually represents the South pole of the earth’s magnetic field, and conversely the South geographic pole corresponds to the North pole of the earth’s magnetic field. The scientists described the cause of the earth’s magnetism that the magnetic field is generated by electric currents due to the motion of convection currents from a mixture of molten iron and nickel in the earth’s outer core these convection currents are caused by heat escaping from the core, a natural process called a geodynamo. The circulating ions that are highly conducting in the outer core of the earth result in the formation of the current loops. These current loops are the reason behind the formation of the magnetic field. Then paleomagnetism is developed to measure the magnetism in rocks that was induced by the earth’s magnetic field. In this paper, cause of the earth’s magnetism is enlightened in a new way. The existence of molten iron and nickel in the earth’s outer core is incorrect because of this high temperature evolving in the outer core of the earth, the materials in other layers also melt. Actually the cause of the earth’s magnetism is the interaction of electric fields electric current induced by the solar wind coronal discharge and the movement of the earth including both rotations about its own axis and the sun as per Faraday and Lenz’s laws of electromagnetic induction. For this cause, all other planets and the satellites e.g., moon in the solar system are having magnetic field which obstructs the maximum high energy particles from the sun solar wind to discharge on their surfaces. Dr. Pijush Kanti Bhattacharjee "Identification Cause of Earth’s Magnetism" Published in International Journal of Trend in Scientific Research and Development (ijtsrd), ISSN: 2456-6470, Volume-6 | Issue-3 , April 2022, URL: https://www.ijtsrd.com/papers/ijtsrd49534.pdf Paper URL: https://www.ijtsrd.com/engineering/electrical-engineering/49534/identification-cause-of-earth’s-magnetism/dr-pijush-kanti-bhattacharjee
Interior Heating of Rocky Exoplanets from Stellar Flares with Application to ...Sérgio Sacani
Many stars of different spectral types with planets in the habitable zone are known to emit flares. Until now, studies
that address the long-term impact of stellar flares and associated coronal mass ejections (CMEs) assumed that the
planet’s interior remains unaffected by interplanetary CMEs, only considering the effect of plasma/UV
interactions on the atmosphere of planets. Here, we show that the magnetic flux carried by flare-associated CMEs
results in planetary interior heating by ohmic dissipation and leads to a variety of interior–exterior interactions. We
construct a physical model to study this effect and apply it to the TRAPPIST-1 star whose flaring activity has been
constrained by Kepler observations. Our model is posed in a stochastic manner to account for uncertainty and
variability in input parameters. Particularly for the innermost planets, our results suggest that the heat dissipated in
the silicate mantle is both of sufficient magnitude and longevity to drive geological processes and hence facilitate
volcanism and outgassing of the TRAPPIST-1 planets. Furthermore, our model predicts that Joule heating can
further be enhanced for planets with an intrinsic magnetic field compared to those without. The associated
volcanism and outgassing may continuously replenish the atmosphere and thereby mitigate the erosion of the
atmosphere caused by the direct impact of flares and CMEs. To maintain consistency of atmospheric and
geophysical models, the impact of stellar flares and CMEs on atmospheres of close-in exoplanetary systems needs
to be studied in conjunction with the effect on planetary interiors.
Evidence for Long-Lasting Electrical Leader Discharges in NonSpecular Meteor ...researchinventy
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Disturbances in Solar Wind Electrons during the Ascending Half of the Solar Cycle 23
1. Research Inventy: International Journal of Engineering And Science
Vol.6, Issue 8 (September 2016), PP -01-06
Issn (e): 2278-4721, Issn (p):2319-6483, www.researchinventy.com
1
Disturbances in Solar Wind Electrons during the Ascending Half
of the Solar Cycle 23
Antony Dhivya Tharshini.S*, 1
, Nisha Rani.T*
& Shanthi.G*
*
Department of Physics & Research Centre, Women’s Christian College, Nagercoil, 629 001, India
Abstract: Ulysses achieved a solar orbit with an inclination of 80.200
, perihelion of 1.34 AU, aphelion of 5.4
AU and a period of 6.2 years. By comparing observations taken over nearly all heliolatitudes and two different
intervals covering the same radial distances, we are able to separate the radial and latitudinal variations in the
solar wind. This paper describes the detailed results of the studies devoted to the solar activity impact on the
Earth’s upper atmosphere and ionosphere. The methods used in this study are based on the data driven from the
Ulysses spacecraft. The primary objective of the Ulysses solar wind plasma investigation uses SWOOPS (Solar
Wind Observations over the Poles of the Sun) instrument to investigate and establish bulk flow parameters and
internal state conditions of the solar wind as a function of solar latitude. The electron temperature Te and the
electron density Ne are found to exhibit a sharp enhancement during the ascending half of the solar cycle 23
(1996 – 2004).
Keywords: solar wind electrons, solar activity, ionosphere, solar cycle.
I. INTRODUCTION
The solar wind is generally well characterized by fast and slow regions around solar minimum, with the
solar wind confined around the sun’s streamer belt and the fast solar wind observed at higher latitudes
(McComas et al., 2000). When solar activity increases, the low speed solar wind region extends to higher
latitudes. Ulysses observed the solar wind at solar maximum with its second latitudinal polar pass (November
2000 – October 2001). At this time a more complex solar wind structure was found compared to similar bimodal
solar wind observed near solar minimum. (Hamzah and Homam., 2015). Electron temperature (Te) in
ionosphere is measured by the heat balance between the photoelectrons, cooling through coulomb collisions
with ions, and heat conduction along the magnetic field lines.
Electron density (Ne) is produced by solar EUV (Extreme Ultraviolet Radiation) radiation, since the
solar photons have significant energy to ionize the natural atmosphere, Simultaneously photoelectron produced
in this ionization process heat the local ambient electrons as well as remote electrons along the magnetic field
(Panahi et al., 2013). The determination of the temperature and density structure of the solar corona, both in the
regions of closed magnetic field and in the coronal holes, has therefore been of considerable interest for many
years (Fludra et al., 1999).
For relation between electron density and electron thermal energy as electron temperature, many
studies have shown a negative correlation during daytime and a positive correlation was measured using
incoherent scatter radar. Previous studies have concluded that the positive correlation between Ne and Te
accompanies an increase of solar flux. However, a recent study indicates that the positive correlation occurs
when Ne is significantly high irrespective of solar flux. The result implies that Ne is an important factor that
determines Te in the topside ionosphere (Panahi et al., 2013; Yoshihiro et al., 2011).
Ulysses is providing an exciting opportunity to explore and characterize the heliospheric medium from
the ecliptic plane to above the solar poles at distances from the Sun extending from 1AU to 5AU. Observations
made on the way out to Jupiter are extending our knowledge of the interplanetary medium in the ecliptic plane,
gained from the pioneer and voyager flights, while observations made after Ulysses encounters Jupiter and
journeys over the solar poles will be unique (Bame et al., 1992).The ionospheric electron density variation under
different conditions has a very vital role to play in understanding the lower as well as the upper atmosphere. The
ionosphere is strongly coupled to other regions like the magnetosphere and interplanetary space, whose states
affect activities on earth (Namgaladze et al., 2003). Signals transmitted for communication and navigational
purposes from satellite must definitely pass through the ionosphere, which acts as a perturbing medium on
satellite based navigation systems (Okeke Francisca et al 2009).
Ionosphere is the upper layer of the Earth atmosphere which has a great impact on signal from
telecommunication system. It consists of free electrons and ions that are mostly concentrated in the F-region and
produced mainly by solar radiation (Wasiu Akande Ahmed et al., 2016). The plasmaspheric electron
temperature is an important indicator of the thermal balance between the topside ionosphere and the
plasmasphere, and is a useful parameter with which to determine the thermal coupling between them (Denton et
al., 1999). The elementary mechanisms that play an important role in the electron temperature (Te) variation
2. Disturbances in Solar Wind Electrons during the Ascending Half of the Solar Cycle 23
2
with solar flux seem to be broadly understood. Recently, interest in the electron temperature (Te) behaviour at
high latitudes has been renewed with the measurements of extremely high electron temperatures (Te > 5000 K)
at altitudes below 500 km (Xuemin Zhang et al., 2013). These temperatures and temperature gradients were
measured with the radar in the vicinity of both the late morning and early afternoon convection reversals. Very
high electron temperatures (Te ~ 4000 – 6000 K) were also measured near 500 km in red aurora (Schunk et al.,
1986; Truhlik et al., 2012).
The temperature overshoot occurs because the heating rate is approximately linear in the electron
density while the cooling rate is quadratic in the electron density. The electron heating depends on the electron
density, because the primary heat source for the thermal electrons is by collision with the photoelectrons that are
generated by the photo ionization of the neural gases (Stolle et al., 2011; Schunk et al., 1986). The results shows
the comparison of measured and modelled electron densities and electron temperatures for magnetically quiet
and moderate solar activity conditions at locations close to the geomagnetic equator and equatorial anomaly
crests along 2010
geomagnetic meridian (Bhuyan et al., 2008)
II. DATA DESCRIPTION
In the life time, Ulysses completed three polar pass around the Sun (1992-2008) in a roughly polar
orbit (Bame et al., 1992; Brahmanandam et al., 2011). The orbit perihelion (aphelion) is located in the solar
equatorial plane at the distance of about 1.3 AU. Ulysses was constantly in the solar wind during the solar
minimum. The data submitted to the National Space Science Data Center (NSSDC) for the electron analyzer has
been used for the analysis. The first step in the electron data reduction process is determination of the bulk,
scalar spacecraft potential (Yiding Chen et al., 2008; Guidoni et al., 2015). Ulysses data are indeed unique since
the spacecraft was mainly measuring fast solar wind originating from the large polar coronal holes .Ulysses
solar wind data are provided by the Ulysses final archieve [ http://ufa.esac.esa.int] .
The SWOOPS Instrument:
Ulysses achieved a solar orbit with an inclination of 80.200
, perihelion of 1.34 AU, aphelion of 5.4 AU,
and a period of 6.2 years. In route to solar polar orbit, it made a close flyby of Jupiter and made measurements
of solar system’s largest planet. The SWOOPS electron spectrometer is a 120o
spherical section electrostatic
analyzer which measures the 3 dimensional velocity space distributions of solar wind electrons. In its normal
solar wind mode, the instrumental energy range is 1.6 to 862 ev in the spacecraft frame. The approach to the
SWOOPS design was to attempt to strike a balance between the conflicting requirements so as to optimize the
overall plasma science yield from the mission and support other Ulysses investigations while staying within the
available mission resources. Solar wind electron measurements are made with a spherical section electrostatic
analyzer (Hamidi et al., 2016). Electrons that pass through the entrance aperture with proper angles are selected
in energy with appropriate voltages applied across the curved plates. These distributions are, of course from in-
ecliptic measurements, but high speed solar wind is emphasized since it is expected that at high latitudes the
flow will be somewhat similar to high speed flows observed in the ecliptic plane (Frederic Ouattara et al., 2012).
III. RESULTS AND DISCUSSION
3.1. Solar activity variations of Ne and Te :
In order to investigate the solar activity variations effect on the parameters are observed using
SWOOPS instrument and presented from height 900 km to 2000 km within the polar pass latitude as 80.20
S –
80.20
N. It must be proved that obviously the electron temperature (Te) does not remain same throughout the
solar activity, which means both for solar activity minimum and maximum. Most often, a beamed,
unidirectional heat flux component is also present in the distributions, carrying energy from the hot corona out
into the colder interplanetary space along the interplanetary magnetic field. Sometimes, the heat flux is observed
to be counter – streaming, or bidirectional. At other times, the heat flux electrons disappear from the
distributions, suggesting field merging and disconnection sunward of the spacecraft (Karine Issautier et al.,
1998; Fahmi et al., 2016). These heat flux features contribute important information on the global magnetic
topology of the interplanetary magnetic field on the nature of the interplanetary solar wind and on its source.
3. Disturbances in Solar Wind Electrons during the Ascending Half of the Solar Cycle 23
3
Figure 1 – variation of electron density (Ne) for the Ulysses second polar pass from September 2001 to
December 2001 in the ascending half of the solar cycle 23, shows sharp peaks with the polar pass latitude > 70
N.
Figure (1) shows the directly increasing daily average mean values of the solar activity respectively as
a function of electron density (Ne) concentration during the descending phase of year 2001. The Ne and Te data
in the figure (1 & 2) is measured by the Ulysses spacecraft; the peaks presented below reveal a positive
correlation between them for high values of Ne, where high values of Ne with high Te are most abundant in all
seasons and all levels of solar activity. Interestingly, in all month except with a small difference in September
and December, minimum value of Te corresponds to maximum value of Ne. To investigate the annual variation
of Ne and Te, it should be noted that obviously the electron temperature didn’t keep the same for both solar
activity minimum and maximum. The peak electron density varies throughout the year as 1x105
cm-3
and the
temperature below 3x105
(K). The beginning of second polar pass the electron density maximum (1.37342 cm-3
)
is comparatively less than the maximum of electron temperature (1.6x105
K). One of the features which are
seasonal variation is a typical phenomenon during summer and winter. The effect of winter anomaly is large
during solar maximum and small during solar minimum. According to this interpretation when Ne is sufficiently
high, the differences in the temperature of electrons during the solar activity is high.
Figure 2 – variation of electron temperature (Te) for the Ulysses second polar pass from September 2001 to
December 2001 in the ascending half of the solar cycle 23, shows sharp peaks with the polar pass latitude > 70
N.
4. Disturbances in Solar Wind Electrons during the Ascending Half of the Solar Cycle 23
4
3.2. Analysis of Electron density (Ne):
The study of electron density within 80.20
N latitude is a model algorithm presented for the time period
of 1996-2004. As illustrated in the figures, the electron density variation trends are almost similar in 2002-2004.
In these years the electron density Ne increases initially with sharp peaks at 3.8cm-3
, from August to December
the solar wind plasma significantly decreases. Absolutely a different pattern of Ne is observed in the year 1996
till August very less variation is been observed the peak reaches 1.4cm-3
. There are similar variations observed
in the years 1998-1999 and 2000-2001. In the range of 1100km to 1500km electron density changes are reliable.
Figure 3 – Annual variation total electron density (Ne) for the year (1996 – 2004) has been plotted for the
hourly averaged Ulysses second polar pass
Figure (3) depicts that the density of electron varies gradually with the temperature of electrons but in
few cases the manifesto is reversible this may be due to the velocity distribution in the particular medium. As
the results the maximum density during the beginning of the year is about 1.373 cm-3
which gradually shows the
greatest peak during the middle of the year as 2.11018 cm-3
and the temperature ranges from 1x105
to 4x106
.
The above figure shows, that there is no large difference in the total and core density of electrons but the halo
density is comparatively less than the core electron density, but it is reversible in the temperature of electron
where the halo temperature of electron is higher than the total and the core which says the temperature is more
when it reaches the ionosphere.
3.3. Analysis of Electron temperature (Te):
One of the prime objectives of SWOOPS is to establish a global picture of the internal plasma state of
the solar wind. The solar activity has occurred with different temperature throughout the year. Here we discuss
about the electron temperature Te which changes by time during the initial phase of the solar cycle 23. The
electron temperature Te pattern has no similar variations throughout the solar cycle. Figure (4) shows a day
average for the Ulysses second polar pass (1996-2004), on which the biggest solar event has observed where
initially the Te has raised above 1.5x105
(K) but the core temperature remains less than 1x105
(k) and then there
occur a sudden variation in the last month of the year. Furthermore with the decreasing temperature ranges
between 3.2x105
K – 1.4x105
K.
5. Disturbances in Solar Wind Electrons during the Ascending Half of the Solar Cycle 23
5
Figure 4 – Annual variation total electron temperature (Te) for the year (1996 – 2004) has been plotted for the
hourly averaged Ulysses second polar pass.
IV. CONCLUSION
During the period from 1999-2001, the electron density Ne of solar wind was highest just after solar
maximum and decreased by nearly a factor of 2 over the rest of the solar cycle. The sun’s approach to solar
maximum, coronal structure becomes increasingly complex, and the magnetic field becomes less dipolar. The
electron temperature Te in the second polar pass from September 2000 to January 2001 with the polar pass
latitude greater than 700
N along with the maximum latitude as 80.20
N polar shows a temperature drop seems to
be slightly cooler than the south polar orbit, during this time the temperature ranges from 1.2x105
.We
investigated that the integrated Ne decreases with an increase of the integrated Te along with the average
distribution in observed with more number of spikes below 2x106
K. The maximum and minimum phase
variations of Ne are possible during every plasma waves with respect to the solar events. The electron
temperature increases with increasing solar activity at altitudes above 2000 km. The day-time differences
between high and low activity can be as much as 1000 K. Between 1000 km and 2000 km altitude, a reverse
variation occurs and Te is comparatively higher during low solar activity.
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