Orientation Error Compensation for a system of Two Rubidium Atomic Clocks Placed in a Directionally Varying Magnetic Field

2021 ◽  
Author(s):  
Sergey Ermak ◽  
Vladimir Semenov
Keyword(s):  
Magnetic Field ◽  
Error Compensation ◽  
Atomic Clocks ◽  
Orientation Error

Research of Interference Field Measurement and Error Compensation for Geomagnetic Navigation

2014 ◽  
Vol 602-605 ◽  
pp. 1586-1589 ◽  
Author(s):  
Guang Sheng Liu ◽  
Zhen Zhen Guan
Keyword(s):  
Magnetic Field ◽  
Magnetic Dipole ◽  
Calculation Method ◽  
Field Measurement ◽  
Error Compensation ◽  
High Accuracy ◽  
Magnetic Field Measurement ◽  
Interference Field ◽  
Aeromagnetic Survey ◽  
Designed Experiments

Aiming at removing interference field in the geomagnetic navigation, the technology of interference magnetic field measurement and error compensation are studied. The scheme of error measuring and compensating are designed, the compensation model is established based on the magnetic dipole theory, its calculation method is designed, experiments prove that this technology is of high accuracy and its process is simpler, it provides a new way for eliminating interference in the aeromagnetic survey.

scholarly journals Magnetic Field-Induced Spectroscopy of Forbidden Optical Transitions with Application to Lattice-Based Optical Atomic Clocks

2006 ◽  
Vol 96 (8) ◽  
Author(s):  
A. Taichenachev ◽  
V. Yudin ◽  
C. Oates ◽  
C. Hoyt ◽  
Z. Barber ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Atomic Clocks ◽  
Optical Transitions

scholarly journals Detecting the gravito-magnetic field of the dark halo of the Milky Way - the LaDaHaD mission concept

2021 ◽  
Author(s):  
Angelo Tartaglia ◽  
Massimo Bassan ◽  
Lorenzo Casalino ◽  
Mariateresa Crosta ◽  
Mario Lattanzi ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Milky Way ◽  
Time Of Flight ◽  
Atomic Clocks ◽  
Dark Halo ◽  
The Sun ◽  
Lagrange Points ◽  
The Asymmetry ◽  
Electromagnetic Signals

AbstractWe propose to locate transponders and atomic clocks in at least three of the Lagrange points of the Sun-Earth pair, with the aim of exploiting the time of flight asymmetry between electromagnetic signals travelling in opposite directions along polygonal loops having the Lagrange points at their vertices. The asymmetry is due to the presence of a gravito-magnetic field partly caused by the angular momentum of the Sun, partly originating from the angular momentum of the galactic dark halo in which the Milky Way is embedded. We list also various opportunities which could be associated with the main objective of this Lagrange Dark Halo Detector (LaDaHaD).

Magnetic-field strengths from optical polarization data

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg
Keyword(s):  
Magnetic Field ◽  
Optical Polarization ◽  
Polarization Data ◽  
Term Model ◽  
Source Of Information ◽  
Field Strengths

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.

Observing the galactic magnetic field

1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst
Keyword(s):  
Magnetic Field ◽  
Fair Agreement ◽  
Solar Neighbourhood ◽  
Galactic Magnetic Field ◽  
The Magnetic Field

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.

Structure in the radiation of the galactic disk

1967 ◽  
Vol 31 ◽  
pp. 355-356
Author(s):  
R. D. Davies
Keyword(s):  
Magnetic Field ◽  
Galactic Disk ◽  
Galactic Magnetic Field ◽  
Measured Polarization

Observations at various frequencies between 136 and 1400 MHz indicate a considerable amount of structure in the galactic disk. This result appears consistent both with measured polarization percentages and with considerations of the strength of the galactic magnetic field.

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

Faint Hα Emission in the Corona and Its Relation to the Prominences

1994 ◽  
Vol 144 ◽  
pp. 339-342
Author(s):  
V. N. Dermendjiev ◽  
Z. Mouradian ◽  
J.- L. Leroy ◽  
P. Duchlev
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Essential Role ◽  
Hα Emission

AbstractThe relation between episodically observed in the solar corona faint Hαemission structures and the long lived prominences was studied. Particular consideration was given for cases in which the corresponding prominences had undergone DB process. An MHD interpretation of the phenomenon “emissions froides” (cool emission) is proposed in which an essential role plays the prominence supporting magnetic field.

Evolution of Large-Scale Coronal Structures

1994 ◽  
Vol 144 ◽  
pp. 29-33
Author(s):  
P. Ambrož
Keyword(s):  
Magnetic Field ◽  
Field Line ◽  
Large Scale ◽  
Coronal Magnetic Field ◽  
Source Surface ◽  
Solar Cycles ◽  
Characteristic Relationship ◽  
The Magnetic Field ◽  
Coronal Structures

AbstractThe large-scale coronal structures observed during the sporadically visible solar eclipses were compared with the numerically extrapolated field-line structures of coronal magnetic field. A characteristic relationship between the observed structures of coronal plasma and the magnetic field line configurations was determined. The long-term evolution of large scale coronal structures inferred from photospheric magnetic observations in the course of 11- and 22-year solar cycles is described.Some known parameters, such as the source surface radius, or coronal rotation rate are discussed and actually interpreted. A relation between the large-scale photospheric magnetic field evolution and the coronal structure rearrangement is demonstrated.

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