A Review of Studies Made on the Decade Fluctuations in the Earth's Rate of Rotation
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Solar System Table of Contents Publisher's Note Editors' Introduction List of Contributors Complete List of Contents Archeaostronomy (new) Asteroids Auroras Big Bang Brown Dwarfs Callisto (new) Ceres (new) Comet Halley Comet Shoemaker-Levy 9 (new) Comets Coordinate Systems Coronal Holes and Coronal Mass Ejections (new) Cosmic Rays Cosmology Dwarf Planets (new) Earth-Moon Relations (new) Earth-Sun Relations Earth System Science Earth's Age Earth's Atmosphere Earth's Composition Earth's Core Earth's Core-Mantle Boundary Earth's Crust Earth's Crust-Mantle Boundary(new) Earth's Differentiation Earth's Magnetic Field: Origins Earth's Magnetic Field: Secular Variation Earth's Magnetic Field at Present Earth's Magnetosphere Earth's Mantle Earth's Oceans Earth's Origin Earth's Rotation Earth's Shape Earth's Structure Eclipses Electromagnetic Radiation: Thermal Emissions (new) Electromagnetic Radiation: Nonthermal Emissions (new) Enceladus (new) Eris and Dysnomia (new) Europa Extrasolar Planet Detection Methods (new) Extrasolar Planetary Systems Extraterrestrial Life in the Solar System Gamma-Ray Bursters Ganymede (new) General Relativity Gravity Measurement Greenhouse Effect Habitable Zones (new) Hertzsprung-Russell Diagram Iapetus (new) Impact Cratering Infrared Astronomy Interstellar Clouds and the Interstellar Medium Interplanetary Environment (new) Io Jovian Planets Jupiter's Atmosphere Jupiter's Great Red Spot Jupiter's Interior (new) Jupiter's Magnetic Field and Radiation Belts Jupiter's Ring System (new) Jupiter's Satellites Kuiper Belt -
Four Centuries of Geomagnetic Secular Variation from Historical Records
Fourcenturies of geomagnetic secular variationfrom historical records ByAndrewJackson 1,ArtR.T. Jonkers 2 andMatthewR.W alker 1 1School ofEarth Sciences, Leeds University,Leeds LS29JT, UK 2Departmentof History, V rijeUniversiteit, Amsterdam, The Netherlands Wepresent anewmodel of the magnetic eld at the core{mantle boundary for the interval 1590{1990. Themodel, called gufm1,is based on amassive newcompilation of historical observations of the magnetic eld. The greater part of the newdataset originates from unpublished observations taken by mariners engaged in merchant and naval shipping. Considerable attention is given to both correction of data for possible mislocation (originating from poor knowledge of longitude) and to proper allocation of error in the data. Weadopt astochastic model for uncorrected positional errors that properly accounts for the nature of the noise process based on aBrownian motion model. Thevariability of navigational errors as afunction of the duration of the voyages that wehave analysed isconsistent with this model. For the period before 1800, more than 83 000 individual observations of magnetic declination wererecorded at more than 64 000 locations; more than 8000 new observations are for the 17th century alone. Thetime-dependent eld model that weconstruct from the dataset is parametrized spatially in terms of spherical harmonics and temporally in B-splines, using atotal of 36 512 parameters. Themodel has improved the resolution of the core eld, and represents the longest continuous model of the eld available. However, full exploitation of the database may demand anew modelling methodology. Keywords: Earth’score; geom agneticsec ularvariation ; magnetic¯ eld;m aritimehistory 1.Intro duction TheEarth has possessed amagnetic eld for more than 4billion years, generated in the ®uid core. -
Chandler Wobble: Stochastic and Deterministic Dynamics 3 2 Precession and Deformation
Chandler wobble: Stochastic and deterministic dynamics Alejandro Jenkins Abstract We propose a model of the Earth’s torqueless precession, the “Chandler wobble”, as a self-oscillation driven by positive feedback between the wobble and the centrifugal deformation of the portion of the Earth’s mass contained in circu- lating fluids. The wobble may thus run like a heat engine, extracting energy from heat-powered geophysical circulations whose natural periods would otherwise be unrelated to the wobble’s observed period of about fourteen months. This can ex- plain, more plausibly than previous models based on stochastic perturbations or forced resonance, how the wobble is maintained against viscous dissipation. The self-oscillation is a deterministic process, but stochastic variations in the magnitude and distribution of the circulations may turn off the positive feedback (a Hopf bifur- cation), accounting for the occasional extinctions, followed by random phase jumps, seen in the data. This model may have implications for broader questions about the relation between stochastic and deterministic dynamics in complex systems, and the statistical analysis thereof. 1 Introduction According to Euler’s theory of the free symmetric top, the axis of rotation precesses about the axis of symmetry, unless both happen to align [1]. Applied to the Earth, this implies that the instantaneous North Pole should describe a circle about the axis of symmetry (perpendicular to the Earth’s equatorial bulge), causing a periodic change in the latitude of any fixed -
Redalyc.On a Possible Connection Between Chandler Wobble and Dark
Brazilian Journal of Physics ISSN: 0103-9733 [email protected] Sociedade Brasileira de Física Brasil Portilho, Oyanarte On a possible connection between Chandler wobble and dark matter Brazilian Journal of Physics, vol. 39, núm. 1, marzo, 2009, pp. 1-11 Sociedade Brasileira de Física Sâo Paulo, Brasil Available in: http://www.redalyc.org/articulo.oa?id=46413555001 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative Brazilian Journal of Physics, vol. 39, no. 1, March, 2009 1 On a possible connection between Chandler wobble and dark matter Oyanarte Portilho∗ Instituto de F´ısica, Universidade de Bras´ılia, 70919-970 Bras´ılia–DF, Brazil (Received on 17 july, 2007) Chandler wobble excitation and damping, one of the open problems in geophysics, is treated as a consequence in part of the interaction between Earth and a hypothetical oblate ellipsoid made of dark matter. The physical and geometrical parameters of such an ellipsoid and the interacting torque strength is calculated in such a way to reproduce the Chandler wobble component of the polar motion in several epochs, available in the literature. It is also examined the consequences upon the geomagnetic field dynamo and generation of heat in the Earth outer core. Keywords: Chandler wobble; Polar motion; Dark matter. 1. INTRODUCTION ence of a DM halo centered in the Sun and its influence upon the motion of planets; numerical simulations due to Diemand et al. -
Magnetic Power Spectrum, with Application to Planetary Dynamo Radii
Earth and Planetary Science Letters 401 (2014) 347–358 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl A new model for the (geo)magnetic power spectrum, with application to planetary dynamo radii ∗ Benoit Langlais a, , Hagay Amit a, Hugo Larnier a,b, Erwan Thébault c, Antoine Mocquet a a Laboratoire de Planétologie et Géodynamique, CNRS UMR 6112, Université de Nantes, 44322 Nantes cedex 3, France b Institut de Physique du Globe de Strasbourg, UdS–CNRS UMR7516, EOST – Université de Strasbourg, 5 rue René Descartes, 67084 Strasbourg Cedex, France c Équipe de Géomagnétisme, Institut de Physique du Globe de Paris, CNRS UMR 7154, 75252 Paris cedex 5, France a r t i c l e i n f o a b s t r a c t Article history: We propose two new analytical expressions to fit the Mauersberger–Lowes geomagnetic field spectrum Received 6 November 2013 at the core–mantle boundary. These can be used to estimate the radius of the outer liquid core where the Received in revised form 23 April 2014 geodynamo operates, or more generally the radius of the planetary dynamo regions. We show that two Accepted 10 May 2014 sub-families of the geomagnetic field are independent of spherical harmonics degree n at the core–mantle Available online 9 July 2014 boundary and exhibit flat spectra. The first is the non-zonal field, i.e., for spherical harmonics order m Editor: C. Sotin different from zero. The second is the quadrupole family, i.e., n + m even. The flatness of their spectra is Keywords: motivated by the nearly axisymmetric time-average paleomagnetic field (for the non-zonal field) and the magnetic power spectrum dominance of rotational effects in core dynamics (for the quadrupole family). -
Losing the Geomagnetic Shield: a Critical Issue for Space Settlement Philip K
Losing the Geomagnetic Shield: A Critical Issue for Space Settlement Philip K. Chapman1 February 3, 2017 Abstract. The geomagnetic field seems to be collapsing. This has happened many times in the deep past, but never since civilization began. One implication is that the cost of space settlement will increase substantially if we do not expedite deployment of initial facilities in low Earth orbit. Another implication, less certain but much more damaging, is that the collapse may lead to catastrophic global cooling before the end of this century. We must establish self-sufficient communities off Earth before that happens. 1. The ELEO Shelter As Al Globus et al have pointed out,2 the annual radiation dose in equatorial low Earth orbit (ELEO, below 600 km altitude) is less than the limit for occupational exposure that is recommended by the International Commission on Radiological Protection. The first extraterrestrial habitats and assembly plants will need little if any radiation shielding if they are located in such an orbit, reducing the mass that must be launched from Earth by orders of magnitude. These fortunate conditions create a haven in ELEO where we can develop the infrastructure for space settlement at relatively low cost. This is a major opportunity to shrink the technical and economic barriers to growth of a true interplanetary society. The most important functions of early facilities in ELEO include: 1. Assembling and launching missions to obtain radiation shielding materials at low cost (probably water or slag from a near-Earth asteroid). 2. Developing experience concerning the long-term physiological requirements for living and working in space (with or without frequent transfers to and from free fall), in order to specify acceptable rotation rates and centrifugal pseudo-gravity levels. -
Mercury's Resonant Rotation from Secular Orbital Elements
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Institute of Transport Research:Publications Mercury’s resonant rotation from secular orbital elements Alexander Stark a, Jürgen Oberst a,b, Hauke Hussmann a a German Aerospace Center, Institute of Planetary Research, D-12489 Berlin, Germany b Moscow State University for Geodesy and Cartography, RU-105064 Moscow, Russia The final publication is available at Springer via http://dx.doi.org/10.1007/s10569-015-9633-4. Abstract We used recently produced Solar System ephemerides, which incorpo- rate two years of ranging observations to the MESSENGER spacecraft, to extract the secular orbital elements for Mercury and associated uncer- tainties. As Mercury is in a stable 3:2 spin-orbit resonance these values constitute an important reference for the planet’s measured rotational pa- rameters, which in turn strongly bear on physical interpretation of Mer- cury’s interior structure. In particular, we derive a mean orbital period of (87.96934962 ± 0.00000037) days and (assuming a perfect resonance) a spin rate of (6.138506839 ± 0.000000028) ◦/day. The difference between this ro- tation rate and the currently adopted rotation rate (Archinal et al., 2011) corresponds to a longitudinal displacement of approx. 67 m per year at the equator. Moreover, we present a basic approach for the calculation of the orientation of the instantaneous Laplace and Cassini planes of Mercury. The analysis allows us to assess the uncertainties in physical parameters of the planet, when derived from observations of Mercury’s rotation. 1 1 Introduction Mercury’s orbit is not inertially stable but exposed to various perturbations which over long time scales lead to a chaotic motion (Laskar, 1989). -
Solar Activity, Earth's Rotation Rate and Climate Variations in the Secular And
Physics and Chemistry of the Earth 31 (2006) 99–108 www.elsevier.com/locate/pce Solar activity, Earth’s rotation rate and climate variations in the secular and semi-secular time scales S. Duhau * Facultad de Ciencias Exactas, Departamento de Fı´sica, Universidad de Buenos Aires, Argentina Received 17 January 2005; accepted 18 March 2005 Available online 29 March 2006 Abstract By applying the wavelet formalism to sudden storm commencements and aa geomagnetic indices and solar total irradiation, as a proxy data for solar sources of climate-forcing, we have searched the signatures of those variables on the Northern Hemisphere surface temperature. We have found that cyclical behaviour in surface temperature is not clearly related to none of these variables, so we have suggested that besides them surface temperature might be related to Earth’s rotation rate variations. Also it has been suggested that in the long-term Earth’s rotation rate variations might be excited by geomagnetic storm time variations which, in turn, depends on solar activity. The study of these phenomena and its relationships is addressed in the present paper. With this purpose we perform an analysis of the evolution during the last 350 years of the signals that conform the 11-year sunspot cycle maxima envelope for different time scales. The result is applied to analyze the relationship between long-term variations in sunspot number and excess of length of day; and to unearth the signature in surface temperature of this last from that of sudden storm commencement and aa geomagnetic indices and total solar irradiation. As solar dynamo experiments transient processes in all the time scales from seconds to centuries, Fourier analysis and its requirement for the process to be stationary is likely to produce spurious periodicities. -
Analysis of the Secular Variations of Longitudes of the Sun, Mercury and Venus from Optical Observations
Highlights of Astronomy, Vol. 12 International Astronomical Union, 2002 H. Rickman, ed. Analysis of the Secular Variations of Longitudes of the Sun, Mercury and Venus from Optical Observations Y.B. Kolesnik Institute of Astronomy of the Russian Academy of Sciences, Piatnitskaya str. 48, 109017 Moscow, Russia Abstract. About 240 000 optical observations of the Sun, Mercury and Venus, accumulated during the era of classical astrometry from Bradley up to our days, are incorporated to analyse the secular variation of the lon gitudes of innermost planets. A significant discrepancy between modern ephemerides and optical observations is discovered. The possible sources of discrepancy are discussed. The tidal acceleration of the Moon has been revised to conform the lunar theory with the ephemerides of the planets. The offset and residual rotation of Hipparcos-based system with respect to the dynamical equinox is determined. Interpretation of this rotation is given. 1. Observations and method of analysis A mass of 244960 observations of the Sun, Mercury and Venus accumulated during historical period of astronomy from 1750 to 2000 have been incorporated. In the transformation procedure a set of corrections were formed by direct comparison of standard star catalogue with ICRS-based catalogue rotated from J2000 to the respective epoch by use of modern precession constant and Hip- parcos based proper motions. The systematic differences are interpolated onto observed positions of planets and applied. Other corrections account for dif ferences in modern and historical astronomical constants. The N70E catalogue (Kolesnik 1997) rigidly rotated onto Hipparcos frame was used as a reference catalogue. Observations were compared with DE405 ephemeris. -
Improvement of the Secular Variation Curve of the Geomagnetic Field In
LETTER Earth Planets Space, 51, 1325–1329, 1999 Improvement of the secular variation curve of the geomagnetic field in Egypt during the last 6000 years Hatem Odah∗ Institute for Study of the Earth’s Interior, Okayama University, Misasa, Tottori-ken 682-0193, Japan (Received July 14, 1999; Revised October 28, 1999; Accepted November 1, 1999) A total of 115 ceramic specimens out of 41 samples from 9 archeological sites in Giza, Fayoum, Benisuef, El Minia, Malawy, and Sohag were collected. They represent 14 well-determined ages covering the last 6000 years. Rock magnetic properties such as Curie temperature and hysteresis loops have been measured for these samples to identify the magnetic carrier; it is found to be fine-grained magnetite. All specimens were investigated using the classic Thellier double heating technique (Thellier and Thellier, 1959) and the modification after Odah et al. (1995) to obtain the paleointensity data. These paleointensities and the previous results of Odah et al. (1995) were used to improve the secular variation curve of the geomagnetic field in Egypt for the last 6000 years. This curve shows a maximum of 72.8 μT at about 250 AD and a minimum of 33 μT at about 3500 BC. It also shows a general decrease of the magnetic moment during the last 2000 years. 1. Introduction the samples were collected, have been thoroughly studied by Egypt, with its long and well-documented history, pro- many egyptologists and ceramicists (e.g., Boak, 1933; Bres- vides well-dated archeological materials suitable for pale- ciani, 1968; O’Connor, 1997 and others). -
On a Possible Connection Between Chandler Wobble and Dark Matter
Brazilian Journal of Physics, vol. 39, no. 1, March, 2009 1 On a possible connection between Chandler wobble and dark matter Oyanarte Portilho∗ Instituto de F´ısica, Universidade de Bras´ılia, 70919-970 Bras´ılia–DF, Brazil (Received on 17 july, 2007) Chandler wobble excitation and damping, one of the open problems in geophysics, is treated as a consequence in part of the interaction between Earth and a hypothetical oblate ellipsoid made of dark matter. The physical and geometrical parameters of such an ellipsoid and the interacting torque strength is calculated in such a way to reproduce the Chandler wobble component of the polar motion in several epochs, available in the literature. It is also examined the consequences upon the geomagnetic field dynamo and generation of heat in the Earth outer core. Keywords: Chandler wobble; Polar motion; Dark matter. 1. INTRODUCTION ence of a DM halo centered in the Sun and its influence upon the motion of planets; numerical simulations due to Diemand et al. [8] show the presence of DM clumps surviving near A 305-day Earth free precession was predicted by Euler in the solar circle; Adler [9] suggests that internal heat produc- the 18th century and was sought since then by astronomers in tion in Neptune and hot-Jupiter exoplanets is due to accretion the form of small latitude variations. F. Kustner¨ in 1888 and of planet-bound, not self-annihilating DM. Although the na- S. C. Chandler in 1891 detected such a motion but with a pe- ture of the particles that form DM is not known precisely (see riod of approximately 435 days. -
Aas 16-495 Nonlinear Analytical Equations Of
AAS 16-495 NONLINEAR ANALYTICAL EQUATIONS OF RELATIVE MOTION ON J2-PERTURBED ECCENTRIC ORBITS Bradley Kuiack∗ and Steve Ulrichy Future spacecraft formation flying missions will require accurate autonomous guid- ance systems to calculate a reference, or desired, relative motion during reconfig- uration maneuvers. However, the efficiency in terms of propellant used for such maneuvers depends on the fidelity of the dynamics model used for calculating the reference relative motion. Therefore, an efficient method for calculating rela- tive motion should have an analytical solution, be applicable to an eccentric orbit, and should take into account the J2 perturbation. This paper accomplishes this through an exact analytical solution of the relative motion between two spacecraft based on the orbital elements of each spacecraft. Specifically, by propagating the J2-perturbed osculating orbital elements forward in time and solving the exact so- lution at each time step, an accurate representation of the true spacecraft relative motion is obtained. When compared to a numerical simulator, the proposed an- alytical solution is shown to accurately model the relative motion, with bounded errors on the order of meters over a wide range of eccentricity values. INTRODUCTION Formation flying of multiple spacecraft is a key enabling technology for many future scientific missions such as enhanced stellar optical interferometers and virtual platforms for Earth or Sun observations. However, formation flying involves several considerations beyond those of a sin- gle spacecraft mission. This is particularly true for the guidance system, which is responsible for calculating a reference, or desired, relative motion to be actively tracked during reconfiguration ma- neuvers by the on-board control system of a follower spacecraft.