The Relationship between Ultraviolet Line Emission and Magnetic Field Strength in Magnetic Cataclysmic Variables

1999 ◽  
Vol 117 (2) ◽  
pp. 1014-1022 ◽  
Author(s):  
Steve B. Howell ◽  
Jennifer Cash ◽  
Keith O. Mason ◽  
Adrienne E. Herzog
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
Cataclysmic Variables ◽  
Line Emission ◽  
Magnetic Cataclysmic Variables ◽  
The Relationship

The Effect of Magnetic Field Strength on the Oscillatory Characteristics of Multimode Magnetoconvection

1993 ◽  
Vol 10 (4) ◽  
pp. 275-277
Author(s):  
J.O. Murphy ◽  
J.M. Lopez ◽  
C.P. Dyt
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
The Relationship ◽  
The Magnetic Field ◽  
Period Of Oscillation

AbstractThe effect of varying magnetic field strength on the frequency of oscillatory motions for cellular multimode magnetoconvection has been investigated. In addition the influence of the thermal, viscous and magnetic diffusivities have been taken into account and the range of preferred horizontal scales established. The relationship between the period of oscillation and the magnetic field strength is determined.

Defining the Relationship of Magnetohydrodynamic Voltages and Magnetic Field Strength

2017 ◽  
Author(s):  
Kevin J. Wu ◽  
T. Stan Gregory ◽  
Michael C. Lastinger ◽  
Brian Boland ◽  
Zion Tsz Ho Tse
Keyword(s):  
Magnetic Field ◽  
Blood Flow ◽  
Field Strength ◽  
Aortic Arch ◽  
Magnetic Field Strength ◽  
Quantitative Relationship ◽  
Solution Concentration ◽  
Exercise Stress ◽  
Induced Voltage ◽  
The Relationship

The magnetohydrodynamic (MHD) effect is observed in flowing electrolytic fluids and their interactions with magnetic fields. The magnetic field (B0), when perpendicular with the electrolytic fluid flow (μ), causes the shift of the charged particles in the fluid to shift across the length of the vessel (L) normal to the plane of B0 and flow, creating a voltage (VMHD) observable through voltage potential measurements across the flow (Eqn. 1)[1].(1)VMHD=∫0Lu⇀×B0⇀·dL⇀In the medical field, this phenomenon is commonly encountered inside of a human body inside of an MRI machine (Fig. 1). The effect appears most prominently inside the aortic arch due to orientation and size, and is a large contributing factor to noise observed in intra-MRI ECGs [2, 3]. Traditionally, this MHD induced voltage (VMHD) was filtered out to obtain clean intra-MRI ECGs, but recent studies have shown that the VMHD induced in a vessel is related to the blood flow through it (stroke volume in the case of the aortic arch) [4]. Further proof of this relationship can be shown from the increase in VMHD measured from periphery blood vessels during periods of elevated heart rate from exercise stress, when compared to baseline state [5]. Previously, a portable device was built to utilize induced VMHD as an indicator of flow [6]. The device was capable of showing change in blood flow, utilizing a blood flow metric obtained from VMHD, however a quantitative relationship between VMHD and blood flow has yet to be established. This study aims to define the relationship between induced VMHD and magnetic field strength in a controlled setting. Through modulating the distance between a pair of magnets around a flow channel, we hope to better realize the relationship between magnetic field strength and induced VMHD with constant flow and electrolytic solution concentration.

Stress measurement based on magnetostrictive characteristic parameters

2021 ◽  
Vol 63 (5) ◽  
pp. 283-288
Author(s):  
Entao Yao ◽  
Fei Han ◽  
Ping Wang ◽  
Yuan Zhang
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
Static Magnetic Field ◽  
Stress Measurement ◽  
Maximum Relative Error ◽  
Electromagnetic Acoustic Transducer ◽  
Wide Range ◽  
The Relationship ◽  
Non Destructive

Non-destructive testing (NDT) involving stress measurement has found a wide range of applications in rail, pipeline, bridge and other engineering areas and it is therefore necessary to find a method to measure stress. In this paper, a non-destructive method is proposed to measure stress by observation of the magnetostrictive properties of the objects. Stress in the elastic range is applied to the ferromagnetic material, changing its lattice, while stress in the plastic range changes its microstructure. These are the reasons for the magnetostrictive coefficient variation of the material. An experimental platform was set up, using a cantilever beam with a strain gauge, to study the relationship between the SH wave, the static magnetic field strength and the applied uniaxial stress. The curve obtained shows the relationship between the amplitude of the electromagnetic acoustic transducer (EMAT) signal and the static magnetic field strength. The magnetostrictive parameters, sensitive to stress, were extracted from the curve. This method is verified through trials on test samples with a maximum relative error between experimental and predicted values of 8.06%.

scholarly journals Discovery of a young pre-intermediate polar

2021 ◽  
Author(s):  
David J Wilson ◽  
Odette Toloza ◽  
John D Landstreet ◽  
Boris T Gänsicke ◽  
Jeremy J Drake ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
White Dwarf ◽  
White Dwarfs ◽  
Hubble Space Telescope ◽  
Cataclysmic Variables ◽  
Rotation Period ◽  
Field Measurements ◽  
The Magnetic Field

Abstract We present the discovery of a magnetic field on the white dwarf component in the detached post common envelope binary (PCEB) CC Cet. Magnetic white dwarfs in detached PCEBs are extremely rare, in contrast to the high incidence of magnetism in single white dwarfs and cataclysmic variables. We find Zeeman-split absorption lines in both ultraviolet Hubble Space Telescope (HST) spectra and archival optical spectra of CC Cet. Model fits to the lines return a mean magnetic field strength of 〈|B|〉 ≈ 600–700 kG. Differences in the best-fit magnetic field strength between two separate HST observations and the high v sin  i of the lines indicate that the white dwarf is rotating with a period ∼0.5 hours, and that the magnetic field is not axisymmetric about the spin axis. The magnetic field strength and rotation period are consistent with those observed among the intermediate polar class of cataclysmic variable, and we compute stellar evolution models that predict CC Cet will evolve into an intermediate polar in 7–17 Gyr. Among the small number of known PCEBs containing a confirmed magnetic white dwarf, CC Cet is the hottest (and thus youngest), with the weakest field strength, and cannot have formed via the recently proposed crystallisation/spin-up scenario. In addition to the magnetic field measurements, we update the atmospheric parameters of the CC Cet white dwarf via model spectra fits to the HST data and provide a refined orbital period and ephemeris from TESS photometry.

scholarly journals The relationship between chromospheric emissions and magnetic field strength

2009 ◽  
Vol 497 (1) ◽  
pp. 273-285 ◽  
Author(s):  
M. Loukitcheva ◽  
S. K. Solanki ◽  
S. M. White
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
The Relationship

scholarly journals X-Ray Emission from Cataclysmic Variables

1979 ◽  
Vol 53 ◽  
pp. 508-508
Author(s):  
D. Q. Lamb
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
Classification Scheme ◽  
Accretion Rate ◽  
Cataclysmic Variables ◽  
X Rays ◽  
X Ray ◽  
Stellar Radius ◽  
The Magnetic Field

Many cataclysmic variables have been found to be hard, as well as soft, X-ray sources. Emission from the boundary layer of an optically thick accretion disk extending down to the stellar surface can, at outburst, produce soft X-rays, but the production of hard X-rays from such a disk is difficult to understand. We therefore conjecture that the sources which emit hard X-rays have magnetic fields and are, in general, rotating. We then propose a classification scheme for cataclysmic variables based on the size of the Alfven radius rA relative to the stellar radius R of the degenerate dwarf and the separation α of the binary system. We show that many of the varied characteristics displayed by the cataclysmic variable X-ray sources can be understood in terms of this ordering. We suggest that the AM Her Class (AM Her, AN UMa, W Pup, and 2A0311-23) have R ≪ α ≪ rA , the DQ Her Class (DQ Her, V533 Her, and AE Aqr) have R ≪ rA ≪ α, while the SS Cyg Class (SS Cyg, U Gem, EX Hya, and GK Per) have rA ≲ R ≪ α. Although rA depends on both the magnetic field strength of the degenerate dwarf ana the accretion rate, for comparable rates of accretion the ordering that we propose is essentially one of decreasing magnetic field strength.

scholarly journals Compressed magnetized shells of atomic gas and the formation of the Corona Australis molecular cloud

2020 ◽  
Vol 644 ◽  
pp. A5
Author(s):  
A. Bracco ◽  
D. Bresnahan ◽  
P. Palmeirim ◽  
D. Arzoumanian ◽  
Ph. André ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
Molecular Cloud ◽  
Interstellar Dust ◽  
Dust Emission ◽  
Line Emission ◽  
Physical Association ◽  
Atomic Gas ◽  
The Magnetic Field

We present the identification of the previously unnoticed physical association between the Corona Australis molecular cloud (CrA), traced by interstellar dust emission, and two shell-like structures observed with line emission of atomic hydrogen (HI) at 21 cm. Although the existence of the two shells had already been reported in the literature, the physical link between the HI emission and CrA had never been highlighted until now. We used both Planck and Herschel data to trace dust emission and the Galactic All Sky HI Survey (GASS) to trace HI. The physical association between CrA and the shells is assessed based both on spectroscopic observations of molecular and atomic gas and on dust extinction data with Gaia. The shells are located at a distance between ~140 and ~190 pc, which is comparable to the distance of CrA, which we derived as (150.5 ± 6.3) pc. We also employed dust polarization observations from Planck to trace the magnetic-field structure of the shells. Both of them show patterns of magnetic-field lines following the edge of the shells consistently with the magnetic-field morphology of CrA. We estimated the magnetic-field strength at the intersection of the two shells via the Davis-Chandrasekhar-Fermi (DCF) method. Despite the many caveats that are behind the DCF method, we find a magnetic-field strength of (27 ± 8) μG, which is at least a factor of two larger than the magnetic-field strength computed off of the HI shells. This value is also significantly larger compared to the typical values of a few μG found in the diffuse HI gas from Zeeman splitting. We interpret this as the result of magnetic-field compression caused by the shell expansion. This study supports a scenario of molecular-cloud formation triggered by supersonic compression of cold magnetized HI gas from expanding interstellar bubbles.

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