Nanosatellite Probes in Interplanetary Space

Total Page:16

File Type:pdf, Size:1020Kb

Nanosatellite Probes in Interplanetary Space NANOSATELLITE PROBES IN INTERPLANETARY SPACE: AN AUGMENTED CASSINI MISSION A Thesis presented to the Faculty of California Polytechnic State University, San Luis Obispo In Partial Fulfillment of the Requirements for the Degree Master of Science in Aerospace Engineering by Trent T Voris July 2017 © 2017 Trent T Voris ALL RIGHTS RESERVED ii COMMITTEE MEMBERSHIP TITLE: Nanosatellite Probes In Interplanetary Space: An Augmented Cassini Mission AUTHOR: Trent T Voris DATE SUBMITTED: July 2017 COMMITTEE CHAIR: Dr. Jordi Puig-Suari, Ph.D. Professor of Aerospace Engineering COMMITTEE MEMBER: Dr. Eric Mehiel, Ph.D. Professor of Aerospace Engineering COMMITTEE MEMBER: Dr. Kira Abercromby, Ph.D. Associate Professor of Aerospace Engineering COMMITTEE MEMBER: Dr. Ricardo Tubio-Pardavia, Ph.D. Systems Engineer iii ABSTRACT Nanosatellite Probes In Interplanetary Space: An Augmented Cassini Mission Trent T Voris The exploration of interplanetary space is one of the most challenging and costly ventures in human history. The relatively low amount of information on other sites beyond Earth is largely due to the rarity of effective trajectories as well as the high levels of risk and complexity inherent in innovative space exploration. One solution to this lack of information is the use of deployable satellite probes to help augment the main mission and its instrumentation. This “Mother-Daughter” architecture allows for the low-cost exploration of hazardous sites and numerous points of interest without compromising the primary mission. While the end goal is the use of nanosatellites on future interplanetary missions, this thesis focuses on an existing interplanetary mission, Cassini. The aim to demonstrate the scientific viability of this “Mother-Daughter” architecture can be achieved by locating numerous unexplored sites that could have been surveyed with a nanosatellite probe onboard Cassini. Each of these potential sites can be expanded into a unique science mission of its own, and in many cases the trajectories can be selected and optimized to better suit the practical design of a nanosatellite in the various interplanetary environments. Keywords: Architecture, Cassini, CubeSat, Daughter, Interplanetary, Mother, Nanosatellite, Probe, Saturn, Space, Spacecraft, Trajectory iv ACKNOWLEDGMENTS Thanks to Dr. Jordi Puig-Suari, my advisor, for working with me to create a thesis that was both interesting and applicable to the future of interplanetary space exploration, and for putting me in contact with the brightest minds in the field of nanosatellites from NASA’s Jet Propulsion Laboratory in Pasadena. My gratitude also extends out to Dr. Eric Mehiel for his patience and guidance that allowed me to work on a project that best fit my strengths and passions in Aerospace Engineering. Thanks to the scientists and engineers of NASA’s Jet Propulsion Laboratory for allowing me to participate in discussions and studies regarding nanosatellites in interplanetary space. Thanks to my peers at PolySat for showing interest in my results and processes through out this study. Thanks to friends and family for giving me a place to sleep and keeping me sane. Thanks to the baristas of Starbucks on Union, Blossom Hill, Five Cities, and Hermosa Beach for all of the Chai Lattes, Turkey Pesto Sandwiches, and Wi-Fi that allowed me to put in the long hours needed to finish this thesis. v TABLE OF CONTENTS Page LIST OF TABLES ............................................................................................... viii LIST OF FIGURES ................................................................................................ ix LIST OF ACRONYMS .......................................................................................... xi 1. INTRODUCTION ............................................................................................ 1 1.1 THE PROBLEM .............................................................................................. 1 1.2 THE SOLUTION ............................................................................................. 3 2. CASSINI MISSION ............................................................................................ 7 2.1 MISSION ....................................................................................................... 7 2.1.1 Saturn .................................................................................................... 7 2.1.2 Ring science objectives ......................................................................... 7 2.1.3 Icy satellite science objectives .............................................................. 8 2.1.4 Magnetosphere ...................................................................................... 8 2.2 DESIGN ........................................................................................................ 9 3. AUGMENTED MISSION ................................................................................ 10 3.1 GIVENS ...................................................................................................... 11 3.2 SATURN'S RINGS ........................................................................................ 13 3.2.1 Process ................................................................................................ 14 3.2.2 Results ................................................................................................. 15 3.2.3 Other Options ...................................................................................... 16 3.3 SATURN’S MOONS ..................................................................................... 17 vi Page 3.3.1 Setup .................................................................................................... 18 3.3.2 Impactors ............................................................................................. 19 3.3.2.1 Process ............................................................................................ 19 3.3.2.2 Unique Case .................................................................................... 23 3.3.2.3 Totals .............................................................................................. 26 3.3.3 Orbiters ................................................................................................ 31 3.3.3.1 Process ............................................................................................ 31 3.3.3.2 Results ............................................................................................. 32 3.3.4 Flybys .................................................................................................. 35 3.4 SUMMARY .................................................................................................. 35 4. ANCILLARY ANALYSIS ............................................................................... 37 4.1 GIVENS ...................................................................................................... 38 4.2 PLANETARY GRAVITY ASSISTS .................................................................. 40 4.2.1 Process ................................................................................................ 40 4.2.1.1 Deployment Phase .......................................................................... 40 4.2.1.2 Gravity Assist Phase ....................................................................... 42 4.2.1.3 Drift Phase ...................................................................................... 48 4.2.2 Results ................................................................................................. 50 4.3 SUMMARY .................................................................................................. 54 5. CONCLUSION ................................................................................................. 55 BIBLIOGRAPHY ................................................................................................. 58 APPENDIX ........................................................................................................... 61 vii LIST OF TABLES Page Table 1. Missions to the Outer Planets [2] .............................................................. 2 Table 2. Saturnian Moon Data [17] [18] ............................................................... 11 Table 3. Excerpt from Cassini's Tour of the Saturnian System [10] ..................... 13 Table 4. Saturn Ring Impactor Results [19] .......................................................... 16 Table 5. Significant Gravity Wells in the Saturnian System ................................. 19 Table 6. Excerpt of Moon Trajectory Data ........................................................... 23 Table 7. Impactor Proof of Concept ...................................................................... 24 Table 8. Saturn’s Moon Exploration Possibilities ................................................. 36 Table 9. Missions to the Outer Planets [23] .......................................................... 37 Table 10. Planetary Data [22] [14] ........................................................................ 38 Table 11. Planetary Gravity Assist Parameters [22] ............................................. 45 Table 12. Augmented Cassini's Planetary Possibilities ......................................... 54 Table 13. Augmented Cassini Possibilities ........................................................... 57 viii LIST OF FIGURES Page Figure 1. Cosmic Journey [1] .................................................................................
Recommended publications
  • Stability of the Moons Orbits in Solar System in the Restricted Three-Body
    Stability of the Moons orbits in Solar system in the restricted three-body problem Sergey V. Ershkov, Institute for Time Nature Explorations, M.V. Lomonosov's Moscow State University, Leninskie gory, 1-12, Moscow 119991, Russia e-mail: [email protected] Abstract: We consider the equations of motion of three-body problem in a Lagrange form (which means a consideration of relative motions of 3-bodies in regard to each other). Analyzing such a system of equations, we consider in details the case of moon‟s motion of negligible mass m₃ around the 2-nd of two giant-bodies m₁, m₂ (which are rotating around their common centre of masses on Kepler’s trajectories), the mass of which is assumed to be less than the mass of central body. Under assumptions of R3BP, we obtain the equations of motion which describe the relative mutual motion of the centre of mass of 2-nd giant-body m₂ (Planet) and the centre of mass of 3-rd body (Moon) with additional effective mass m₂ placed in that centre of mass (m₂ + m₃), where is the dimensionless dynamical parameter. They should be rotating around their common centre of masses on Kepler‟s elliptic orbits. For negligible effective mass (m₂ + m₃) it gives the equations of motion which should describe a quasi-elliptic orbit of 3-rd body (Moon) around the 2-nd body m₂ (Planet) for most of the moons of the Planets in Solar system. But the orbit of Earth‟s Moon should be considered as non-constant elliptic motion for the effective mass 0.0178m₂ placed in the centre of mass for the 3-rd body (Moon).
    [Show full text]
  • Stellar Dynamics and Stellar Phenomena Near a Massive Black Hole
    Stellar Dynamics and Stellar Phenomena Near A Massive Black Hole Tal Alexander Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, Rehovot, Israel 76100; email: [email protected] | Author's original version. To appear in Annual Review of Astronomy and Astrophysics. See final published version in ARA&A website: www.annualreviews.org/doi/10.1146/annurev-astro-091916-055306 Annu. Rev. Astron. Astrophys. 2017. Keywords 55:1{41 massive black holes, stellar kinematics, stellar dynamics, Galactic This article's doi: Center 10.1146/((please add article doi)) Copyright c 2017 by Annual Reviews. Abstract All rights reserved Most galactic nuclei harbor a massive black hole (MBH), whose birth and evolution are closely linked to those of its host galaxy. The unique conditions near the MBH: high velocity and density in the steep po- tential of a massive singular relativistic object, lead to unusual modes of stellar birth, evolution, dynamics and death. A complex network of dynamical mechanisms, operating on multiple timescales, deflect stars arXiv:1701.04762v1 [astro-ph.GA] 17 Jan 2017 to orbits that intercept the MBH. Such close encounters lead to ener- getic interactions with observable signatures and consequences for the evolution of the MBH and its stellar environment. Galactic nuclei are astrophysical laboratories that test and challenge our understanding of MBH formation, strong gravity, stellar dynamics, and stellar physics. I review from a theoretical perspective the wide range of stellar phe- nomena that occur near MBHs, focusing on the role of stellar dynamics near an isolated MBH in a relaxed stellar cusp.
    [Show full text]
  • The Pennsylvania State University Schreyer Honors College
    THE PENNSYLVANIA STATE UNIVERSITY SCHREYER HONORS COLLEGE DEPARTMENT OF AEROSPACE ENGINEERING LONG TERM ORBITAL MODELING FOR OBJECTS IN GEOSTATIONARY EARTH ORBIT PHILIP CHOW SPRING 2015 A thesis submitted in partial fulfillment of the requirements for a baccalaureate degree in Aerospace Engineering with honors in Aerospace Engineering Reviewed and approved* by the following: David B. Spencer Professor of Aerospace Engineering Thesis Supervisor Robert G. Melton Professor of Aerospace Engineering Honors Adviser George A. Lesieutre Professor of Aerospace Engineering Head of Aerospace Engineering * Signatures are on file in the Schreyer Honors College. i ABSTRACT The suitability of different numerical integrators for the long term orbital modeling of a satellite in geostationary Earth orbit is examined. The integrators used are the ODE45 Runge- Kutta Method from MATLAB and the symplectic Euler method, assuming only spherical harmonics of the Earth and n-body perturbations from the Sun, Moon, and other planets. Results show that the energy drift associated with both integrators makes them unsuitable for long term modeling, and that the symplectic Euler method does not actually maintain constant energy. A possible factor in the energy drift of both integrators includes the model used for n-body perturbations; future work should focus on determining the extent that this affected the results and the steps necessary to correct the errors. ii TABLE OF CONTENTS LIST OF FIGURES ....................................................................................................
    [Show full text]
  • Orbital Mechanics
    Danish Space Research Institute Danish Small Satellite Programme DTU Satellite Systems and Design Course Orbital Mechanics Flemming Hansen MScEE, PhD Technology Manager Danish Small Satellite Programme Danish Space Research Institute Phone: 3532 5721 E-mail: [email protected] Slide # 1 FH 2001-09-16 Orbital_Mechanics.ppt Danish Space Research Institute Danish Small Satellite Programme Planetary and Satellite Orbits Johannes Kepler (1571 - 1630) 1st Law • Discovered by the precision mesurements of Tycho Brahe that the Moon and the Periapsis - Apoapsis - planets moves around in elliptical orbits Perihelion Aphelion • Harmonia Mundi 1609, Kepler’s 1st og 2nd law of planetary motion: st • 1 Law: The orbit of a planet ia an ellipse nd with the sun in one focal point. 2 Law • 2nd Law: A line connecting the sun and a planet sweeps equal areas in equal time intervals. 3rd Law • 1619 came Keplers 3rd law: • 3rd Law: The square of the planet’s orbit period is proportional to the mean distance to the sun to the third power. Slide # 2 FH 2001-09-16 Orbital_Mechanics.ppt Danish Space Research Institute Danish Small Satellite Programme Newton’s Laws Isaac Newton (1642 - 1727) • Philosophiae Naturalis Principia Mathematica 1687 • 1st Law: The law of inertia • 2nd Law: Force = mass x acceleration • 3rd Law: Action og reaction • The law of gravity: = GMm F Gravitational force between two bodies F 2 G The universal gravitational constant: G = 6.670 • 10-11 Nm2kg-2 r M Mass af one body, e.g. the Earth or the Sun m Mass af the other body, e.g. the satellite r Separation between the bodies G is difficult to determine precisely enough for precision orbit calculations.
    [Show full text]
  • Interacting Binaries with Eccentric Orbits. Secular Orbital Evolution
    j-sepinsky, b-willems, [email protected], and [email protected] A Preprint typeset using LTEX style emulateapj v. 08/22/09 INTERACTING BINARIES WITH ECCENTRIC ORBITS. SECULAR ORBITAL EVOLUTION DUE TO CONSERVATIVE MASS TRANSFER J. F. Sepinsky, B. Willems, V. Kalogera, F. A. Rasio Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 j-sepinsky, b-willems, [email protected], and [email protected] ABSTRACT We investigate the secular evolution of the orbital semi-major axis and eccentricity due to mass transfer in eccentric binaries, assuming conservation of total system mass and orbital angular momen- tum. Assuming a delta function mass transfer rate centered at periastron, we find rates of secular change of the orbital semi-major axis and eccentricity which are linearly proportional to the magni- tude of the mass transfer rate at periastron. The rates can be positive as well as negative, so that the semi-major axis and eccentricity can increase as well as decrease in time. Adopting a delta-function −9 −1 mass-transfer rate of 10 M⊙ yr at periastron yields orbital evolution timescales ranging from a few Myr to a Hubble time or more, depending on the binary mass ratio and orbital eccentricity. Com- parison with orbital evolution timescales due to dissipative tides furthermore shows that tides cannot, in all cases, circularize the orbit rapidly enough to justify the often adopted assumption of instanta- neous circularization at the onset of mass transfer. The formalism presented can be incorporated in binary evolution and population synthesis codes to create a self-consistent treatment of mass transfer in eccentric binaries.
    [Show full text]
  • Post-Main-Sequence Planetary System Evolution Rsos.Royalsocietypublishing.Org Dimitri Veras
    Post-main-sequence planetary system evolution rsos.royalsocietypublishing.org Dimitri Veras Department of Physics, University of Warwick, Coventry CV4 7AL, UK Review The fates of planetary systems provide unassailable insights Cite this article: Veras D. 2016 into their formation and represent rich cross-disciplinary Post-main-sequence planetary system dynamical laboratories. Mounting observations of post-main- evolution. R. Soc. open sci. 3: 150571. sequence planetary systems necessitate a complementary level http://dx.doi.org/10.1098/rsos.150571 of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the Received: 23 October 2015 interpretation and modelling of currently known systems and Accepted: 20 January 2016 upcoming discoveries. 1. Introduction Subject Category: Decades of unsuccessful attempts to find planets around other Astronomy Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around Subject Areas: the millisecond pulsar PSR B1257+12 were the first confidently extrasolar planets/astrophysics/solar system reported extrasolar planets to withstand enduring scrutiny due to their well-constrained masses and orbits. However, a retrospective Keywords: historical analysis reveals even more surprises. We now know that dynamics, white dwarfs, giant branch stars, the eponymous celestial body that Adriaan van Maanen observed pulsars, asteroids, formation in the late 1910s [3,4]isanisolatedwhitedwarf(WD)witha metal-enriched atmosphere: direct evidence for the accretion of planetary remnants. These pioneering discoveries of planetary material around Author for correspondence: or in post-main-sequence (post-MS) stars, although exciting, Dimitri Veras represented a poor harbinger for how the field of exoplanetary e-mail: [email protected] science has since matured.
    [Show full text]
  • Orbital Manoeuvres
    AER506 - Fall 2019 B. Vatankhahghadim Lecture 8 Orbital Manoeuvres aving studied the dynamics of orbital motion and how to describe an orbit, we will now look at how H to control and modify spacecraft’s orbits. In particular, we will study the effects of applying thrusts in various directions, and discuss a few specific manoeuvre types. Overview Recall, from Orbit Description and Determination, that an orbit is completely determined by the knowledge of r(t) and v(t) at any given time, t. To move the v ~ ~ f spacecraft from one orbit to another, thruster force is applied, which results in Δ→v v a change in v. Therefore, if a single-impulse manoeuvre is desired, the initial i ~ and final orbits shall have at least one intersection point where the thrust will be applied, as depicted in Figure 8.1. It is assumed that an instantaneous change in the velocity vector, ∆v, is ap- ~ plied via an impulsive thrust. As a result, the position vector, r, is assumed to ~ be unaltered after the burn. This is not completely accurate for real missions with long thruster on/off times, but it is sufficient for our purposes. The over- Figure 8.1: General Manoeuvre all objective of most orbital manoeuvres is to minimize the fuel consumption by minimizing ∆v = j∆vj, and/or to minimize the time taken to complete the manoeuvre. ~ General Manoeuvres Recall the constants of orbital motion from Orbital Mechanics, namely: v · v µ µ v × h r , ~ ~ − = − ; h , r × v ; e , ~ ~ − ~ 2 r 2a ~ ~ ~ ~ µ r The general approach to determining the changes in the orbital parameters as a result of a known ∆v, ap- ~ plied when the spacecraft is at r with an initial velocity of vi, involves computing the resultant velocity vector, ~ ~ vf = vi + ∆v, and determining the constants of the new orbit.
    [Show full text]
  • Orbital Mechanics Third Edition
    Orbital Mechanics Third Edition Edited by Vladimir A. Chobotov EDUCATION SERIES J. S. Przemieniecki Series Editor-in-Chief Air Force Institute of Technology Wright-Patterson Air Force Base, Ohio Publishedby AmericanInstitute of Aeronauticsand Astronautics,Inc. 1801 AlexanderBell Drive, Reston, Virginia20191-4344 American Institute of Aeronautics and Astronautics, Inc., Reston, Virginia Library of Congress Cataloging-in-Publication Data Orbital mechanics / edited by Vladimir A. Chobotov.--3rd ed. p. cm.--(AIAA education series) Includes bibliographical references and index. 1. Orbital mechanics. 2. Artificial satellites--Orbits. 3. Navigation (Astronautics). I. Chobotov, Vladimir A. II. Series. TLI050.O73 2002 629.4/113--dc21 ISBN 1-56347-537-5 (hardcover : alk. paper) 2002008309 Copyright © 2002 by the American Institute of Aeronautics and Astronautics, Inc. All rights reserved. Printed in the United States of America. No part of this publication may be reproduced, distributed, or transmitted, in any form or by any means, or stored in a database or retrieval system, without the prior written permission of the publisher. Data and information appearing in this book are for informational purposes only. AIAA and the authors are not responsible for any injury or damage resulting from use or reliance, nor does AIAA or the authors warrant that use or reliance will be free from privately owned rights. Foreword The third edition of Orbital Mechanics edited by V. A. Chobotov complements five other space-related texts published in the Education Series of the American Institute of Aeronautics and Astronautics (AIAA): Re-Entry Vehicle Dynamics by F. J. Regan, An Introduction to the Mathematics and Methods of Astrodynamics by R.
    [Show full text]
  • Numerical Study of Earth-Mars Trajectories with Lunar Gravity Assist Manoeuvres (Versão Corrigida Após Defesa)
    UNIVERSIDADE DA BEIRA INTERIOR Engenharia Numerical study of Earth-Mars trajectories with lunar gravity assist manoeuvres (Versão corrigida após defesa) Rui Pedro Martins Oliveira Dissertação para a obtenção do Grau de Mestre em Engenharia Aeronáutica (Ciclo de estudos integrado) Orientador: Prof. Doutor Kouamana Bousson Covilhã, Dezembro de 2017 ii À minha mãe o meu muito obrigado. iii iv Resumo Um estudo numérico de trajectórias entre Terra e Marte com manobras de assistência gravita- cional é realizado. Os métodos e modelos utilizados para alcançar esse objectivo são descritos e seus resultados são comparados com os valores reais. Todas as trajectórias de transferência são calculadas pela primeira vez com a formulação do problema dos dois corpos e, em seguida, usando um software de código aberto. Este software é o General Mission Analysis Tool desen- volvido pela NASA. As manobras de assistência gravitacional são normalmente utilizadas para missões aos plane- tas exteriores, a Mercúrio ou quando são usados sistemas de propulsão de baixo impulso. As manobras lunares de assistência gravitacional nunca foram usadas com sucesso nas trajectórias Terra-Marte. Sete missões reais, com órbitas de transferência directa, são usadas para comparar os resulta- dos obtidos das trajectórias com manobras de assistência gravitacional lunar. Não foi possível aplicar essa manobra a todas as missões analisadas. Para as restantes missões foi realizada uma passagem pela Lua, que resulta na diminuição da energia de lançamento quando comparada a uma órbita de transferência directa na mesma altura de injecção. No entanto, quando se comparam com as alturas de injecção reais, apenas uma missão diminui a sua energia de lança- mento.
    [Show full text]
  • Free Energy” Associated with This Technique Is Often Vital for Conducting a Mission in the First Place
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Institute of Transport Research:Publications 66th International Astronautical Congress, Jerusalem, Israel. Copyright ©2015 by Copyright Mr. Volker Maiwald. Published by the IAF, with permission and released to the IAF to publish in all forms. IAC-15-C1.1.2 APPLICABILITY OF TISSERAND CRITERION FOR OPTIMIZATION OF GRAVITY-ASSIST SEQUENCES FOR LOW-THRUST MISSIONS Volker Maiwald German Aerospace Center (DLR), Institute of Space Systems, Department of System Analysis Space Segment, Bremen, Germany, [email protected] Missions for space exploration are becoming more ambitious and gravity-assist maneuvers act as one enabler for them. The “free energy” associated with this technique is often vital for conducting a mission in the first place. Consequently, new methods for optimizing gravity-assist maneuvers and sequences are investigated and further developed – for missions involving impulsive and low-thrust propulsion alike. The System Analysis Space Segment department of the German Aerospace Center (DLR) in Bremen is currently conducting research to combine gravity-assist sequences with low-thrust optimization. One technique, which is prominently used to sequence gravity-assist maneuvers are Tisserand Graphs, based on the Tisserand Criterion, which states that a function of certain orbit parameters of a comet (for mission design purposes spacecraft) remains approximately constant even after a close encounter with a planetary body. However one condition for the validity of the Tisserand Criterion is that the only force acting on the spacecraft is gravity, which obviously would not be the case for a low-thrust mission.
    [Show full text]
  • Circular Orbit
    Circular orbit A circular orbit is the orbit with a fixed distance around the barycenter, that is, in the shape of a circle. Below we consider a circular orbit in astrodynamics or celestial mechanics under standard assumptions. Here the centripetal force is the gravitational force, and the axis mentioned above is the line through the center of the central mass perpendicular to the plane of motion. In this case, not only the distance, but also the speed, angular speed, potential and kinetic energy are constant. There is no periapsis or apoapsis. This orbit has no radial version. A circular orbit is depicted in the top-left Contents quadrant of this diagram, where the Circular acceleration gravitational potential well of the central mass shows potential energy, and the Velocity kinetic energy of the orbital speed is Equation of motion shown in red. The height of the kinetic Angular speed and orbital period energy remains constant throughout the constant speed circular orbit. Energy Delta-v to reach a circular orbit Orbital velocity in general relativity Derivation See also Circular acceleration Transverse acceleration (perpendicular to velocity) causes change in direction. If it is constant in magnitude and changing in direction with the velocity, we get a circular motion. For this centripetal acceleration we have where: is orbital velocity of orbiting body, is radius of the circle is angular speed, measured in radians per unit time. The formula is dimensionless, describing a ratio true for all units of measure applied uniformly across the formula. If the numerical value of is measured in meters per second per second, then the numerical values for will be in meters per second, in meters, and in radians per second.
    [Show full text]
  • Law of Universal Magnetism, F = Ke × H
    Journal of High Energy Physics, Gravitation and Cosmology, 2018, 4, 471-484 http://www.scirp.org/journal/jhepgc ISSN Online: 2380-4335 ISSN Print: 2380-4327 Law of Universal Magnetism, F = ke × H Greg Poole Industrial Tests, Inc., Rocklin, CA, USA How to cite this paper: Poole, G. (2018) Abstract Law of Universal Magnetism, F = ke × H. Journal of High Energy Physics, Gravita- A new universal equation using planet magnetic pole strength is presented tion and Cosmology, 4, 471-484. and given reasoning for its assemblage. Coulomb’s Constant, normally used in https://doi.org/10.4236/jhepgc.2018.43025 calculating electrostatic force is utilized in a new magnetic dipole equation for Received: March 22, 2018 the first time, along with specific orbital energy. Results were generated for Accepted: June 26, 2018 five planets that give insight into specific orbital energy as an energy constant Published: June 29, 2018 for differing planets based on gravitational potential at the surface of a planet. Specific energy can be evaluated as both energy per unit volume (J/kg) and/or Copyright © 2018 by author and 2 2 Scientific Research Publishing Inc. specific orbital energy (m /s ). Due to a multitude of terms that lead to confu- This work is licensed under the Creative sion it is recommended that the IEEE standards committee review specific or- Commons Attribution International bital energy SI units for m2/s2. The magic number for cyclonic “lift off”, or an- License (CC BY 4.0). ti-gravity, is calculated to be ϵ = 148 m2/s2 the value at which a classical law of http://creativecommons.org/licenses/by/4.0/ magnetism appears as F = k × H.
    [Show full text]