A Robust Parking Detection Algorithm Against Electric Railway Magnetic Field Interference

2020 ◽  
Vol 21 (2) ◽  
pp. 882-893 ◽  
Author(s):  
Zusheng Zhang ◽  
Xianmang He ◽  
Huaqiang Yuan
Sensors ◽  
2021 ◽  
Vol 21 (4) ◽  
pp. 1502
Author(s):  
Diogo Schwerz de Lucena ◽  
Justin Rowe ◽  
Vicky Chan ◽  
David J. Reinkensmeyer

There are few wearable sensors suitable for daily monitoring of wrist and finger movements for hand-related healthcare applications. Here, we describe the development and validation of a novel algorithm for magnetically counting hand movements. We implemented the algorithm on a wristband that senses magnetic field changes produced by movement of a magnetic ring worn on the finger (the “Manumeter”). The “HAND” (Hand Activity estimated by Nonlinear Detection) algorithm assigns a “HAND count” by thresholding the real-time change in magnetic field created by wrist and/or finger movement. We optimized thresholds to achieve a HAND count accuracy of ~85% without requiring subject-specific calibration. Then, we validated the algorithm in a dexterity-impaired population by showing that HAND counts strongly correlate with clinical assessments of upper extremity (UE) function after stroke. Finally, we used HAND counts to test a recent hypothesis in stroke rehabilitation that real-world UE hand use increases only for stroke survivors who achieve a threshold level of UE functional capability. For 29 stroke survivors, HAND counts measured at home did not increase until the participants’ Box and Blocks Test scores exceeded ~50% normal. These results show that a threshold-based magnetometry approach can non-obtrusively quantify hand movements without calibration and also verify a key concept of real-world hand use after stroke.


2021 ◽  
Author(s):  
Lily Kromyda ◽  
David M. Malaspina ◽  
Robert E. Ergun ◽  
Jasper Halekas ◽  
Michael L. Stevens ◽  
...  

<p>During its first five orbits, the FIELDS plasma wave investigation on board Parker Solar Probe (PSP)  has observed a multitude of plasma waves, including electrostatic whistler and electron Bernstein waves (Malaspina et al. 2020), sunward propagating whistlers (Agapitov et al. 2020), ion-scale electromagnetic waves (Verniero et al. 2020, Bowen et al. 2020) and Alfven, slow and fast mode waves (Chaston et al. 2020).</p><p>The importance of these waves lies in their potential to redistribute the energy of the solar wind among different particles species (wave-particle interactions) or different types of waves (wave-wave interactions). The abundance of waves and instabilities observed with PSP points to their central role in the regulation of this energy exchange.</p><p>Here we present first observations of an intermittent, electrostatic and broadband plasma wave that is ubiquitous in the range of distances that PSP has probed so far. A unique feature of these waves (FDWs) is a frequency shift that occurs on millisecond timescales. In the frame of the spacecraft, FDWs usually appear between the electron cyclotron and electron plasma frequencies.</p><p>We develop a detection algorithm that identifies the FDWs in low cadence spectra. We analyze them using various statistical techniques. We establish their phenomenology and compare the magnetic fluctuations of the background magnetic field at times of FDWs and at times without FDWs. We establish their polarization with respect to the background magnetic field and search for correlations with various plasma parameters and features in the electron, proton and alpha particle distribution moments. We also investigate possible plasma wave modes that could be responsible for the growth of FDWs and the instability mechanisms that could be generating them.</p><p> </p><p>Lily Kromyda*<sup>(1)</sup>, David M. Malaspina <sup>(1,2)</sup>, Robert E. Ergun<sup>(1,2) </sup>, Jasper Halekas<sup>(3)</sup>, Michael L. Stevens<sup>(4) </sup>, Jennifer Verniero<sup>(5)</sup>, Alexandros Chasapis<sup>(2) </sup>, Daniel Vech<sup>(2) </sup>, Stuart D. Bale<sup>(5,6) </sup>, John W. Bonnell<sup>(5) </sup>, Thierry Dudok de Wit<sup>(7) </sup>, Keith Goetz<sup>(8) </sup>, Katherine Goodrich<sup>(5) </sup>, Peter R. Harvey<sup>(5) </sup>, Robert J. MacDowall<sup>(9) </sup>, Marc Pulupa<sup>(5) </sup>, Anthony W. Case<sup>(4) </sup>, Justin C. Kasper<sup>(10) </sup>, Kelly E. Korreck<sup>(4) </sup>, Davin Larson<sup>(5) </sup>, Roberto Livi<sup>(5) </sup>, Phyllis Whittlesey<sup>(5)</sup></p><p>(1) Astrophysical and Planetary Sciences Department, University of Colorado, Boulder, CO, USA</p><p>(2) Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA</p><p>(3)  University of Iowa, Iowa City, IA, USA</p><p>(4) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA</p><p>(5)  Space Sciences Laboratory, University of California, Berkeley, CA, USA</p><p>(6) Physics Department, University of California, Berkeley, CA, USA</p><p>(7)  LPC2E, CNRS, and University of Orleans, Orleans, France</p><p>(8)  School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA</p><p>(9)  NASA Goddard Space Flight Center, Greenbelt, MD, USA</p><p>(10) University of Michigan, Ann Arbor, MI, USA</p>


2018 ◽  
Vol 846 ◽  
pp. 536-562 ◽  
Author(s):  
W. Mostert ◽  
D. I. Pullin ◽  
R. Samtaney ◽  
V. Wheatley

We present an analysis that predicts the time to development of a singularity in the shape profile of a spatially periodic perturbed, planar shock wave for ideal gas dynamics. Beginning with a formulation in complex coordinates of Whitham’s approximate model geometrical shock dynamics (GSD), we apply a spectral treatment to derive the asymptotic form for the leading-order behaviour of the shock Fourier coefficients for large mode numbers and time. This is shown to determine a critical time at which the coefficients begin to decay, with respect to mode number, at an algebraic rate with an exponent of $-5/2$, indicating loss of analyticity and the formation of a singularity in the shock geometry. The critical time is found to be inversely proportional to a representative measure of perturbation amplitude $\unicode[STIX]{x1D716}$ with an explicit analytic form for the constant of proportionality in terms of gas and shock parameters. To leading order, the time to singularity formation is dependent only on the first Fourier mode. Comparison with results of numerical solutions to the full GSD equations shows that the predicted critical time somewhat underestimates the time for shock–shock (triple-point) formation, where the latter is obtained by post-processing the numerical GSD results using an edge-detection algorithm. Aspects of the analysis suggest that the appearance of loss of analyticity in the shock surface may be a precursor to the first appearance of shock–shocks, which may account for part of the discrepancy. The frequency of oscillation of the shock perturbation is accurately predicted. In addition, the analysis is extended to the evolution of a perturbed planar, fast magnetohydrodynamic shock for the case when the external magnetic field is aligned parallel to the unperturbed shock. It is found that, for a strong shock, the presence of the magnetic field produces only a higher-order correction to the GSD equations with the result that the time to loss of analyticity is the same as for the gas-dynamic flow. Limitations and improvements for the analysis are discussed, as are comparisons with the analogous appearance of singularity formation in vortex-sheet evolution in an incompressible inviscid fluid.


1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg

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.


1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst

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.


1967 ◽  
Vol 31 ◽  
pp. 355-356
Author(s):  
R. D. Davies

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.


1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora

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.


1994 ◽  
Vol 144 ◽  
pp. 339-342
Author(s):  
V. N. Dermendjiev ◽  
Z. Mouradian ◽  
J.- L. Leroy ◽  
P. Duchlev

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.


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