Exploring the Earth's Magnetic Field
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An Ionospheric Remote Sensing Method Using an Array of Narrowband Vlf Transmitters and Receivers
AN IONOSPHERIC REMOTE SENSING METHOD USING AN ARRAY OF NARROWBAND VLF TRANSMITTERS AND RECEIVERS A Dissertation Presented to The Academic Faculty By Nicholas C. Gross In Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the School of Electrical and Computer Engineering Georgia Institute of Technology December 2018 Copyright © Nicholas C. Gross 2018 AN IONOSPHERIC REMOTE SENSING METHOD USING AN ARRAY OF NARROWBAND VLF TRANSMITTERS AND RECEIVERS Approved by: Dr. Morris Cohen, Advisor School of Electrical and Computer Engineering Dr. Paul Steffes Georgia Institute of Technology School of Electrical and Computer Engineering Dr. Sven Simon Georgia Institute of Technology School of Earth and Atmospheric Sciences Dr. Mark Go lkowski Georgia Institute of Technology School of Electrical Engineering University of Colorado Denver Dr. Mark Davenport School of Electrical and Computer Date Approved: September 7, 2018 Engineering Georgia Institute of Technology To my parents Theresa and Brian and to my fianc´e Shraddha ACKNOWLEDGEMENTS I would first like to share my immense gratitude to my advisor, Professor Morris Cohen. He challenged me to pursue my own original ideas and was always available to give guidance and insight. His thoughtful mentorship and sound advice have been invaluable. I am also grateful to have had such an excellent undergraduate research advisor, Professor Mark Go lkowski. Thank you for introducing me to the VLF community and helping me build a strong foundation of electromagnetics and plasma physics knowledge. Thank you to my other three thesis committee members: Professor Sven Simon for further developing my understanding of plasma physics, Professor Paul Steffes for the won- derful conversations about RF and planetary atmospheres, and Professor Mark Davenport for teaching me statistical signal processing techniques. -
The Lorentz Force
CLASSICAL CONCEPT REVIEW 14 The Lorentz Force We can find empirically that a particle with mass m and electric charge q in an elec- tric field E experiences a force FE given by FE = q E LF-1 It is apparent from Equation LF-1 that, if q is a positive charge (e.g., a proton), FE is parallel to, that is, in the direction of E and if q is a negative charge (e.g., an electron), FE is antiparallel to, that is, opposite to the direction of E (see Figure LF-1). A posi- tive charge moving parallel to E or a negative charge moving antiparallel to E is, in the absence of other forces of significance, accelerated according to Newton’s second law: q F q E m a a E LF-2 E = = 1 = m Equation LF-2 is, of course, not relativistically correct. The relativistically correct force is given by d g mu u2 -3 2 du u2 -3 2 FE = q E = = m 1 - = m 1 - a LF-3 dt c2 > dt c2 > 1 2 a b a b 3 Classically, for example, suppose a proton initially moving at v0 = 10 m s enters a region of uniform electric field of magnitude E = 500 V m antiparallel to the direction of E (see Figure LF-2a). How far does it travel before coming (instanta> - neously) to rest? From Equation LF-2 the acceleration slowing the proton> is q 1.60 * 10-19 C 500 V m a = - E = - = -4.79 * 1010 m s2 m 1.67 * 10-27 kg 1 2 1 > 2 E > The distance Dx traveled by the proton until it comes to rest with vf 0 is given by FE • –q +q • FE 2 2 3 2 vf - v0 0 - 10 m s Dx = = 2a 2 4.79 1010 m s2 - 1* > 2 1 > 2 Dx 1.04 10-5 m 1.04 10-3 cm Ϸ 0.01 mm = * = * LF-1 A positively charged particle in an electric field experiences a If the same proton is injected into the field perpendicular to E (or at some angle force in the direction of the field. -
The Van Allen Probes' Contribution to the Space Weather System
L. J. Zanetti et al. The Van Allen Probes’ Contribution to the Space Weather System Lawrence J. Zanetti, Ramona L. Kessel, Barry H. Mauk, Aleksandr Y. Ukhorskiy, Nicola J. Fox, Robin J. Barnes, Michele Weiss, Thomas S. Sotirelis, and NourEddine Raouafi ABSTRACT The Van Allen Probes mission, formerly the Radiation Belt Storm Probes mission, was renamed soon after launch to honor the late James Van Allen, who discovered Earth’s radiation belts at the beginning of the space age. While most of the science data are telemetered to the ground using a store-and-then-dump schedule, some of the space weather data are broadcast continu- ously when the Probes are not sending down the science data (approximately 90% of the time). This space weather data set is captured by contributed ground stations around the world (pres- ently Korea Astronomy and Space Science Institute and the Institute of Atmospheric Physics, Czech Republic), automatically sent to the ground facility at the Johns Hopkins University Applied Phys- ics Laboratory, converted to scientific units, and published online in the form of digital data and plots—all within less than 15 minutes from the time that the data are accumulated onboard the Probes. The real-time Van Allen Probes space weather information is publicly accessible via the Van Allen Probes Gateway web interface. INTRODUCTION The overarching goal of the study of space weather ing radiation, were the impetus for implementing a space is to understand and address the issues caused by solar weather broadcast capability on NASA’s Van Allen disturbances and the effects of those issues on humans Probes’ twin pair of satellites, which were launched in and technological systems. -
Transmittal of Geotail Prelaunch Mission Operation Report
National Aeronautics and Space Administration Washington, D.C. 20546 ss Reply to Attn of: TO: DISTRIBUTION FROM: S/Associate Administrator for Space Science and Applications SUBJECT: Transmittal of Geotail Prelaunch Mission Operation Report I am pleased to forward with this memorandum the Prelaunch Mission Operation Report for Geotail, a joint project of the Institute of Space and Astronautical Science (ISAS) of Japan and NASA to investigate the geomagnetic tail region of the magnetosphere. The satellite was designed and developed by ISAS and will carry two ISAS, two NASA, and three joint ISAS/NASA instruments. The launch, on a Delta II expendable launch vehicle (ELV), will take place no earlier than July 14, 1992, from Cape Canaveral Air Force Station. This launch is the first under NASA’s Medium ELV launch service contract with the McDonnell Douglas Corporation. Geotail is an element in the International Solar Terrestrial Physics (ISTP) Program. The overall goal of the ISTP Program is to employ simultaneous and closely coordinated remote observations of the sun and in situ observations both in the undisturbed heliosphere near Earth and in Earth’s magnetosphere to measure, model, and quantitatively assess the processes in the sun/Earth interaction chain. In the early phase of the Program, simultaneous measurements in the key regions of geospace from Geotail and the two U.S. satellites of the Global Geospace Science (GGS) Program, Wind and Polar, along with equatorial measurements, will be used to characterize global energy transfer. The current schedule includes, in addition to the July launch of Geotail, launches of Wind in August 1993 and Polar in May 1994. -
Plasma Irregularities in the D-Region Ionosphere in Association with Sprite Streamer Initiation
ARTICLE Received 22 Oct 2013 | Accepted 27 Mar 2014 | Published 7 May 2014 DOI: 10.1038/ncomms4740 Plasma irregularities in the D-region ionosphere in association with sprite streamer initiation Jianqi Qin1, Victor P. Pasko1, Matthew G. McHarg2 & Hans C. Stenbaek-Nielsen3 Sprites are spectacular optical emissions in the mesosphere induced by transient lightning electric fields above thunderstorms. Although the streamer nature of sprites has been generally accepted, how these filamentary plasmas are initiated remains a subject of active research. Here we present observational and modelling results showing solid evidence of pre-existing plasma irregularities in association with streamer initiation in the D-region ionosphere. The video observations show that before streamer initiation, kilometre-scale spatial structures descend rapidly with the overall diffuse emissions of the sprite halo, but slow down and stop to form the stationary glow in the vicinity of the streamer onset, from where streamers suddenly emerge. The modelling results reproduce the sub-millisecond halo dynamics and demonstrate that the descending halo structures are optical manifestations of the pre-existing plasma irregularities, which might have been produced by thunderstorm or meteor effects on the D-region ionosphere. 1 Communications and Space Sciences Laboratory, Department of Electrical Engineering, Pennsylvania State University, University Park, Pennsylvania 16802, USA. 2 Department of Physics, United States Air Force Academy, Colorado Springs, Colorado 80840, USA. 3 Geophysical Institute, University of Alaska Fairbanks, Fairbanks, Alaska 99775, USA. Correspondence and requests for materials should be addressed to J.Q. (email: [email protected]). NATURE COMMUNICATIONS | 5:3740 | DOI: 10.1038/ncomms4740 | www.nature.com/naturecommunications 1 & 2014 Macmillan Publishers Limited. -
Chapter 22 Magnetism
Chapter 22 Magnetism 22.1 The Magnetic Field 22.2 The Magnetic Force on Moving Charges 22.3 The Motion of Charged particles in a Magnetic Field 22.4 The Magnetic Force Exerted on a Current- Carrying Wire 22.5 Loops of Current and Magnetic Torque 22.6 Electric Current, Magnetic Fields, and Ampere’s Law Magnetism – Is this a new force? Bar magnets (compass needle) align themselves in a north-south direction. Poles: Unlike poles attract, like poles repel Magnet has NO effect on an electroscope and is not influenced by gravity Magnets attract only some objects (iron, nickel etc) No magnets ever repel non magnets Magnets have no effect on things like copper or brass Cut a bar magnet-you get two smaller magnets (no magnetic monopoles) Earth is like a huge bar magnet Figure 22–1 The force between two bar magnets (a) Opposite poles attract each other. (b) The force between like poles is repulsive. Figure 22–2 Magnets always have two poles When a bar magnet is broken in half two new poles appear. Each half has both a north pole and a south pole, just like any other bar magnet. Figure 22–4 Magnetic field lines for a bar magnet The field lines are closely spaced near the poles, where the magnetic field B is most intense. In addition, the lines form closed loops that leave at the north pole of the magnet and enter at the south pole. Magnetic Field Lines If a compass is placed in a magnetic field the needle lines up with the field. -
Observations of the Relationship Between Sprite Morphology and Incloud Lightning Processes
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111, D15203, doi:10.1029/2005JD006879, 2006 Observations of the relationship between sprite morphology and in-cloud lightning processes Oscar A. van der Velde,1 A´ gnes Mika,2 Serge Soula,1 Christos Haldoupis,2 Torsten Neubert,3 and Umran S. Inan4 Received 10 November 2005; revised 30 March 2006; accepted 25 April 2006; published 4 August 2006. [1] During a thunderstorm on 23 July 2003, 15 sprites were captured by a LLTV camera mounted at the observatory on Pic du Midi in the French Pyre´ne´es. Simultaneous observations of cloud-to-ground (CG) and intracloud (IC) lightning activity from two independent lightning detection systems and a broadband ELF/VLF receiver allow a detailed study of the relationship between electrical activity in a thunderstorm and the sprites generated in the mesosphere above. Results suggest that positive CG and IC lightning differ for the two types of sprites most frequently observed, the carrot- and column-shaped sprites. Column sprites occur after a short delay (<30 ms) from the causative +CG and are associated with little VHF activity, suggesting no direct IC action on the charge transfer process. On the other hand, carrot sprites are delayed up to about 200 ms relative to their causative +CG stroke and are accompanied by a burst of VHF activity starting 25–75 ms before the CG stroke. While column sprites associate with short-lasting (less than 30 ms) ELF/VLF sferics, carrot sprites associate with bursts of sferics initiating at the time of the causative +CG discharge and persisting for 50 to 250 ms, indicating extensive in-cloud activity. -
Permanent Magnet DC Motors Catalog
Catalog DC05EN Permanent Magnet DC Motors Drives DirectPower Series DA-Series DirectPower Plus Series SC-Series PRO Series www.electrocraft.com www.electrocraft.com For over 60 years, ElectroCraft has been helping engineers translate innovative ideas into reality – one reliable motor at a time. As a global specialist in custom motor and motion technology, we provide the engineering capabilities and worldwide resources you need to succeed. This guide has been developed as a quick reference tool for ElectroCraft products. It is not intended to replace technical documentation or proper use of standards and codes in installation of product. Because of the variety of uses for the products described in this publication, those responsible for the application and use of this product must satisfy themselves that all necessary steps have been taken to ensure that each application and use meets all performance and safety requirements, including all applicable laws, regulations, codes and standards. Reproduction of the contents of this copyrighted publication, in whole or in part without written permission of ElectroCraft is prohibited. Designed by stilbruch · www.stilbruch.me ElectroCraft DirectPower™, DirectPower™ Plus, DA-Series, SC-Series & PRO Series Drives 2 Table of Contents Typical Applications . 3 Which PMDC Motor . 5 PMDC Drive Product Matrix . .6 DirectPower Series . 7 DP20 . 7 DP25 . 9 DP DP30 . 11 DirectPower Plus Series . 13 DPP240 . 13 DPP640 . 15 DPP DPP680 . 17 DPP700 . 19 DPP720 . 21 DA-Series. 23 DA43 . 23 DA DA47 . 25 SC-Series . .27 SCA-L . .27 SCA-S . .29 SC SCA-SS . 31 PRO Series . 33 PRO-A04V36 . 35 PRO-A08V48 . 37 PRO PRO-A10V80 . -
Radiation Belt Storm Probes Launch
National Aeronautics and Space Administration PRESS KIT | AUGUST 2012 Radiation Belt Storm Probes Launch www.nasa.gov Table of Contents Radiation Belt Storm Probes Launch ....................................................................................................................... 1 Media Contacts ........................................................................................................................................................ 4 Media Services Information ..................................................................................................................................... 5 NASA’s Radiation Belt Storm Probes ...................................................................................................................... 6 Mission Quick Facts ................................................................................................................................................. 7 Spacecraft Quick Facts ............................................................................................................................................ 8 Spacecraft Details ...................................................................................................................................................10 Mission Overview ...................................................................................................................................................11 RBSP General Science Objectives ........................................................................................................................12 -
Polar Observations of Electron Density Distribution in the Earth's
c Annales Geophysicae (2002) 20: 1711–1724 European Geosciences Union 2002 Annales Geophysicae Polar observations of electron density distribution in the Earth’s magnetosphere. 1. Statistical results H. Laakso1, R. Pfaff2, and P. Janhunen3 1ESA Space Science Department, Noordwijk, Netherlands 2NASA Goddard Space Flight Center, Code 696, Greenbelt, MD, USA 3Finnish Meteorological Institute, Geophysics Research, Helsinki, Sweden Received: 3 September 2001 – Revised: 3 July 2002 – Accepted: 10 July 2002 Abstract. Forty-five months of continuous spacecraft poten- Key words. Magnetospheric physics (magnetospheric con- tial measurements from the Polar satellite are used to study figuration and dynamics; plasmasphere; polar cap phenom- the average electron density in the magnetosphere and its de- ena) pendence on geomagnetic activity and season. These mea- surements offer a straightforward, passive method for mon- itoring the total electron density in the magnetosphere, with high time resolution and a density range that covers many 1 Introduction orders of magnitude. Within its polar orbit with geocentric perigee and apogee of 1.8 and 9.0 RE, respectively, Polar en- The total electron number density is a key parameter needed counters a number of key plasma regions of the magneto- for both characterizing and understanding the structure and sphere, such as the polar cap, cusp, plasmapause, and auroral dynamics of the Earth’s magnetosphere. The spatial varia- zone that are clearly identified in the statistical averages pre- tion of the electron density and its temporal evolution dur- sented here. The polar cap density behaves quite systemati- ing different geomagnetic conditions and seasons reveal nu- cally with season. At low distance (∼2 RE), the density is an merous fundamental processes concerning the Earth’s space order of magnitude higher in summer than in winter; at high environment and how it responds to energy and momentum distance (>4 RE), the variation is somewhat smaller. -
Equivalence of Current–Carrying Coils and Magnets; Magnetic Dipoles; - Law of Attraction and Repulsion, Definition of the Ampere
GEOPHYSICS (08/430/0012) THE EARTH'S MAGNETIC FIELD OUTLINE Magnetism Magnetic forces: - equivalence of current–carrying coils and magnets; magnetic dipoles; - law of attraction and repulsion, definition of the ampere. Magnetic fields: - magnetic fields from electrical currents and magnets; magnetic induction B and lines of magnetic induction. The geomagnetic field The magnetic elements: (N, E, V) vector components; declination (azimuth) and inclination (dip). The external field: diurnal variations, ionospheric currents, magnetic storms, sunspot activity. The internal field: the dipole and non–dipole fields, secular variations, the geocentric axial dipole hypothesis, geomagnetic reversals, seabed magnetic anomalies, The dynamo model Reasons against an origin in the crust or mantle and reasons suggesting an origin in the fluid outer core. Magnetohydrodynamic dynamo models: motion and eddy currents in the fluid core, mechanical analogues. Background reading: Fowler §3.1 & 7.9.2, Lowrie §5.2 & 5.4 GEOPHYSICS (08/430/0012) MAGNETIC FORCES Magnetic forces are forces associated with the motion of electric charges, either as electric currents in conductors or, in the case of magnetic materials, as the orbital and spin motions of electrons in atoms. Although the concept of a magnetic pole is sometimes useful, it is diácult to relate precisely to observation; for example, all attempts to find a magnetic monopole have failed, and the model of permanent magnets as magnetic dipoles with north and south poles is not particularly accurate. Consequently moving charges are normally regarded as fundamental in magnetism. Basic observations 1. Permanent magnets A magnet attracts iron and steel, the attraction being most marked close to its ends. -
Permanent Magnet Design Guidelines
NOTE(2019): THIS ORGANIZATION (MMPA) IS OBSOLETE! MAGNET GUIDELINES Basic physics of magnet materials II. Design relationships, figures merit and optimizing techniques Ill. Measuring IV. Magnetizing Stabilizing and handling VI. Specifications, standards and communications VII. Bibliography INTRODUCTION This guide is a supplement to our MMPA Standard No. 0100. It relates the information in the Standard to permanent magnet circuit problems. The guide is a bridge between unit property data and a permanent magnet component having a specific size and geometry in order to establish a magnetic field in a given magnetic circuit environment. The MMPA 0100 defines magnetic, thermal, physical and mechanical properties. The properties given are descriptive in nature and not intended as a basis of acceptance or rejection. Magnetic measure- ments are difficult to make and less accurate than corresponding electrical mea- surements. A considerable amount of detailed information must be exchanged between producer and user if magnetic quantities are to be compared at two locations. MMPA member companies feel that this publication will be helpful in allowing both user and producer to arrive at a realistic and meaningful specifica- tion framework. Acknowledgment The Magnetic Materials Producers Association acknowledges the out- standing contribution of Parker to this and designers and manufacturers of products usingpermanent magnet materials. Parker the Technical Consultant to MMPA compiled and wrote this document. We also wish to thank the Standards and Engineering Com- mittee of MMPA which reviewed and edited this document. December 1987 3M July 1988 5M August 1996 December 1998 1 M CONTENTS The guide is divided into the following sections: Glossary of terms and conversion A very important starting point since the whole basis of communication in the magnetic material industry involves measurement of defined unit properties.