Dependence of Zeeman splitting of spectral lines on the magnetic field magnitude for NO molecule

2016 ◽  
Vol 29 (2) ◽  
pp. 103-118
Author(s):  
Yu. G. Borkov ◽  
Yu. M. Klimachev ◽  
O. N. Sulakshina
Keyword(s):  
Magnetic Field ◽  
Zeeman Splitting ◽  
Spectral Lines ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
The Magnetic Field

scholarly journals New Force-Free Models of Magnetic Clouds

2005 ◽  
Vol 13 ◽  
pp. 133-133
Author(s):  
M. Vandas ◽  
E. P. Romashets ◽  
S. Watari
Keyword(s):  
Magnetic Field ◽  
Magnetic Cloud ◽  
Free Field ◽  
Flux Rope ◽  
Field Vector ◽  
Magnetic Clouds ◽  
Field Magnitude ◽  
Flux Ropes ◽  
Magnetic Field Magnitude ◽  
The Magnetic Field

AbstractMagnetic clouds are thought to be large flux ropes propagating through the heliosphere. Their twisted magnetic fields are mostly modeled by a constant-alpha force-free field in a circular cylindrical flux rope (the Lundquist solution). However, the interplanetary flux ropes are three dimensional objects. In reality they possibly have a curved shape and an oblate cross section. Recently we have found two force-free models of flux ropes which takes into account the mentioned features. These are (i) a constant-alpha force-free configuration in an elliptic flux rope (Vandas & Romashets 2003, A&A, 398, 801), and (ii) a non-constant-alpha force-free field in a toroid with arbitrary aspect ratio (Romashets & Vandas 2003, AIP Conf Ser. 679, 180). Two magnetic cloud observations were analyzed. The magnetic cloud of October 18-19, 1995 has been fitted by Lepping et al. (1997, JGR, 102, 14049) with use of the Lundquist solution. The cloud has a very flat magnetic field magnitude profile. We fitted it by the elliptic solution (i). The magnetic cloud of November 17-18, 1975 has been fitted by Marubashi (1997) with use of a toroidally adjusted Lundquist solution. The cloud has a large magnetic field vector rotation and a large magnetic field magnitude increase over the background level. We fitted it by the toroidal solution (ii). The both fits match the rotation of the magnetic field vector in a comparable quality to the former fits, but the description of the magnetic field magnitude profiles is remarkable better. It is possible to incorporate temporal effects (expansion) of magnetic clouds into the new solutions through a time-dependent alpha parameter as in Shimazu & Vandas (2002, EP&S, 54, 783).

scholarly journals Interinstrument calibration using magnetic field data from the flux-gate magnetometer (FGM) and electron drift instrument (EDI) onboard Cluster

2014 ◽  
Vol 3 (1) ◽  
pp. 1-11 ◽  
Author(s):  
R. Nakamura ◽  
F. Plaschke ◽  
R. Teubenbacher ◽  
L. Giner ◽  
W. Baumjohann ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Data ◽  
Spin Axis ◽  
Electron Drift ◽  
Magnetic Field Data ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
Flux Gate ◽  
Axis Offset ◽  
The Magnetic Field

Abstract. We compare the magnetic field data obtained from the flux-gate magnetometer (FGM) and the magnetic field data deduced from the gyration time of electrons measured by the electron drift instrument (EDI) onboard Cluster to determine the spin-axis offset of the FGM measurements. Data are used from orbits with their apogees in the magnetotail, when the magnetic field magnitude was between about 20 and 500 nT. Offset determination with the EDI–FGM comparison method is of particular interest for these orbits, because no data from solar wind are available in such orbits to apply the usual calibration methods using the Alfvén waves. In this paper, we examine the effects of the different measurement conditions, such as direction of the magnetic field relative to the spin plane and field magnitude in determining the FGM spin-axis offset, and also take into account the time-of-flight offset of the EDI measurements. It is shown that the method works best when the magnetic field magnitude is less than about 128 nT and when the magnetic field is aligned near the spin-axis direction. A remaining spin-axis offset of about 0.4 ∼ 0.6 nT was observed for Cluster 1 between July and October 2003. Using multipoint multi-instrument measurements by Cluster we further demonstrate the importance of the accurate determination of the spin-axis offset when estimating the magnetic field gradient.

scholarly journals Inter-instrument calibration using magnetic field data from Flux Gate Magnetometer (FGM) and Electron Drift Instrument (EDI) onboard Cluster

2013 ◽  
Vol 3 (2) ◽  
pp. 459-487
Author(s):  
R. Nakamura ◽  
F. Plaschke ◽  
R. Teubenbacher ◽  
L. Giner ◽  
W. Baumjohann ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Data ◽  
Spin Axis ◽  
Electron Drift ◽  
Magnetic Field Data ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
Flux Gate ◽  
Axis Offset ◽  
The Magnetic Field

Abstract. We compare the magnetic field data obtained from the Flux-Gate Magnetometer (FGM) and the magnetic field data deduced from the gyration time of electrons measured by the Electron Drift Instrument (EDI) onboard Cluster to determine the spin axis offset of the FGM measurements. Data are used from orbits with their apogees in the magnetotail, when the magnetic field magnitude was between about 20 nT and 500 nT. Offset determination with the EDI-FGM comparison method is of particular interest for these orbits, because no data from solar wind are available in such orbits to apply the usual calibration methods using the Alfvén waves. In this paper, we examine the effects of the different measurement conditions, such as direction of the magnetic field relative to the spin plane and field magnitude in determining the FGM spin-axis offset, and also take into account the time-of-flight offset of the EDI measurements. It is shown that the method works best when the magnetic field magnitude is less than about 128 nT and when the magnetic field is aligned near the spin-axis direction. A remaining spin-axis offset of about 0.4 ~ 0.6 nT was observed between July and October 2003. Using multi-point multi-instrument measurements by Cluster we further demonstrate the importance of the accurate determination of the spin-axis offset when estimating the magnetic field gradient.

Theoretical Analysis of Magnetic-Electric Prospecting Method for Piping and Seepage Detection of Dyke

2011 ◽  
Vol 103 ◽  
pp. 587-591
Author(s):  
Guo Hong Fu ◽  
Tian Chun Yang
Keyword(s):  
Magnetic Field ◽  
Theoretical Analysis ◽  
High Precision ◽  
Direct Current ◽  
Magnetic Survey ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
The Magnetic Field ◽  
Electric Prospecting

On the basis of presenting the piping and seepage detection by magnetic-electric prospecting method, the authors analyzed and testified validity of the method. According to calculated results, the magnitude of magnetic field of artificial current was smaller on section if electrodes and cables were set rationally. Usually, the magnetic field magnitude of piping had several times to more than decuple comparing with magnetic field of artificial current. So, the magnetic abnormity could be detected easily by high-precision magnetometers. At the same time, their curves’ characteristics were different evidently. The analysis result shows that the piping and seepage of dyke can be detected by combining method of direct current supplying and high-precision magnetic survey.

Influence of the magnetic field magnitude on ? particle deceleration

1980 ◽  
Vol 20 (6) ◽  
pp. 687-692
Author(s):  
I. M. Gaisinskii ◽  
A. V. Kalinin ◽  
A. E. Stepanov
Keyword(s):  
Magnetic Field ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
The Magnetic Field

scholarly journals Variations in ratio and correlation of solar magnetic fields in the Fe I 525.02 nm and Na I 589.59 nm lines according to Mount Wilson measurements during 2000–2012

2018 ◽  
Vol 4 (2) ◽  
pp. 11-34
Author(s):  
Елена Голубева ◽  
Elena Golubeva
Keyword(s):  
Magnetic Field ◽  
Solar Magnetic Field ◽  
Nonlinear Function ◽  
Spectral Lines ◽  
Magnetic Field Data ◽  
Field Magnitude ◽  
Mount Wilson Observatory ◽  
Magnetic Field Magnitude ◽  
Cross Calibration ◽  
Measured Magnetic Field

Variations in the solar magnetic-field ratio over 13 years are analyzed, relying on the comparison of simultaneous measurements in two spectral lines at the Mount Wilson Observatory. The ratio and correlation coefficient are calculated over the general working range of measured magnetic-field values and in various ranges of field magnitudes. We study variations in both the parameters. We have found the following tenden-cies: i) the parameters show changes with solar cycle in the general case; ii) their dependence on magnetic-field magnitude is a nonlinear function of time, and this is especially pronounced in the ratio behavior; iii) several separate ranges of the field magnitudes can be distin-guished based on the behavioral patterns of variations in the ratio. We discuss correspondences between these ranges and the known structural objects of the solar atmosphere. This leads to a conclusion that the dependence of the parameters on magnetic-field magnitude and time is connected with the variety of magnetic structural components and their cyclic rearrangements. The reported results may be useful for solving interpretation problems of solar magnetic-field meas-urements and for the cross-calibration of applicable instruments. They can also be used for tasks related to the creation of a uniform long temporal series of solar magnetic-field data from various sources.

scholarly journals Broadband Linear Polarization in Ap Stars

1993 ◽  
Vol 138 ◽  
pp. 305-309
Author(s):  
Marco Landolfi ◽  
Egidio Landi Degl’Innocenti ◽  
Maurizio Landi Degl’Innocenti ◽  
Jean-Louis Leroy ◽  
Stefano Bagnulo
Keyword(s):  
Magnetic Field ◽  
Circular Polarization ◽  
Linear Polarization ◽  
Rotation Axis ◽  
Spectral Lines ◽  
Line Of Sight ◽  
Long Time ◽  
Rotating Star ◽  
Ap Stars ◽  
The Magnetic Field

AbstractBroadband linear polarization in the spectra of Ap stars is believed to be due to differential saturation between σ and π Zeeman components in spectral lines. This mechanism has been known for a long time to be the main agent of a similar phenomenon observed in sunspots. Since this phenomenon has been carefully calibrated in the solar case, it can be confidently used to deduce the magnetic field of Ap stars.Given the magnetic configuration of a rotating star, it is possible to deduce the broadband polarization at any phase. Calculations performed for the oblique dipole model show that the resulting polarization diagrams are very sensitive to the values of i (the angle between the rotation axis and the line of sight) and β (the angle between the rotation and magnetic axes). The dependence on i and β is such that the four-fold ambiguity typical of the circular polarization observations ((i,β), (β,i), (π-i,π-β), (π-β,π-i)) can be removed.

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