3,821 research outputs found
Numerical Algorithm for Detecting Ion Diffusion Regions in the Geomagnetic Tail with Applications to MMS Tail Season May 1 -- September 30, 2017
We present a numerical algorithm aimed at identifying ion diffusion regions
(IDRs) in the geomagnetic tail, and test its applicability. We use 5 criteria
applied in three stages. (i) Correlated reversals (within 90 s) of Vx and Bz
(at least 2 nT about zero; GSM coordinates); (ii) Detection of Hall electric
and magnetic field signatures; and (iii) strong (>10 mV/m) electric fields.
While no criterion alone is necessary and sufficient, the approach does provide
a robust, if conservative, list of IDRs. We use data from the Magnetospheric
Multiscale Mission (MMS) spacecraft during a 5-month period (May 1 to September
30, 2017) of near-tail orbits during the declining phase of the solar cycle. We
find 148 events satisfying step 1, 37 satisfying steps 1 and 2, and 17
satisfying all three, of which 12 are confirmed as IDRs. All IDRs were within
the X-range [-24, -15] RE mainly on the dusk sector and the majority occurred
during traversals of a tailward-moving X-line. 11 of 12 IDRs were on the
dusk-side despite approximately equal residence time in both the pre- and
post-midnight sectors (56.5% dusk vs 43.5% dawn). MMS could identify signatures
of 4 quadrants of the Hall B-structure in 3 events and 3 quadrants in 7 of the
remaining 12 confirmed IDRs identified. The events we report commonly display
Vx reversals greater than 400 km/s in magnitude, normal magnetic field
reversals often >10 nT in magnitude, maximum DC |E| which are often well in
excess of the threshold for stage 3. Our results are then compared with the set
of IDRs identified by visual examination from Cluster in the years 2000-2005.Comment: In Submission at JGR:Space Physic
Unilateral choanal atresia
Choanal atresia was first described by Otto in 1830 (Otto A., 1830). This condition is a rare one. Polson et al. (1943) found that in the period 1829-1945, only five hundred cases had been reported. A report on a case of unilateral choanal atresia is presented. The etiology, diagnosis and treatment of the condition are also discussed. The patient, a sixteen year old girl, presented at St. Luke's Hospital Malta with foul smelling discharge from the right side of the nose. As regards etiology, most of the cases are congenital, only very few being caused by syphilis, diphtheria, trauma or tuberculosis. All bilateral choanal atresia cases need emergency operation and removal of the obstruction and insertion of Aechersen's cannulae, to restore patency of the nasal airway, while unilateral cases need no urgent treatment.peer-reviewe
Kilohertz QPOs in Neutron Star Binaries modeled as Keplerian Oscillations in a Rotating Frame of Reference
Since the discovery of kHz quasi-periodic oscillations (QPO) in neutron star
binaries, the difference between peak frequencies of two modes in the upper
part of the spectrum, i.e. Delta (omega)=omega_h-omega_K has been studied
extensively. The idea that the difference Delta(omega) is constant and (as a
beat frequency) is related to the rotational frequency of the neutron star has
been tested previously. The observed decrease of Delta(omega) when omega_h and
omega_k increase has weakened the beat frequency interpretation. We put forward
a different paradigm: a Keplerian oscillator under the influence of the
Coriolis force. For such an oscillator, omega_h and the assumed Keplerian
frequency omega_k hold an upper hybrid frequency relation:
omega^2_h-omega^2_K=4*Omega^2, where Omega is the rotational frequency of the
star's magnetosphere near the equatorial plane. For three sources (Sco X-1, 4U
1608-52 and 4U 1702-429), we demonstrate that the solid body rotation
Omega=Omega_0=const. is a good first order approximation. Within the second
order approximation, the slow variation of Omega as a function of omega_K
reveals the structure of the magnetospheric differential rotation. For Sco X-1,
the QPO have frequencies approximately 45 and 90 Hz which we interpret as the
1st and 2nd harmonics of the lower branch of the Keplerian oscillations for the
rotator with vector Omega not aligned with the normal of the disk: omega_L/2
pi=(Omega/pi)(omega_K/omega_h)sin(delta) where delta is the angle between
vector Omega and the vector normal to the disk.Comment: 13 pages, 3 figures, accepted for publications in ApJ Letter
2,9,16,23-TetraÂkis(1-methylÂethÂyl)-5,6,11,12,13,14,19,20,25,26,27,28-dodecadehydroÂtetraÂbenzo[a,e,k,o]cycloÂeicosene1
The title compound, C48H40, is a tetraÂisopropyl-substituted polyannulenoenyne. The unsubstituted polyannulenoenyne, C36H16 (CSD: RICVEE; CAS: 186494-87-1), has quasi-D
2 (222) symmetry, as determined by least-squares fit (excluding H atoms) to a model optimized in D
2 symmetry by molÂecular mechanics (r.m.s. deviation = 0.239 Å). The least-squares fits of 36 common C atoms of the title compound (at 90 K) to the parent (at 295 K) and to the optimized model show r.m.s. deviations of 0.419 and 0.426 Å, respectively
Reply to comment by H. Hasegawa on "Evolution of Kelvin-Helmholtz activity on the dusk flank magnetopause"
We demonstrate, on experimental grounds, that the justifications for the comment by Hasegawa [2009], hereinafter
H09, on work done by Foullon et al. [2008], hereinafter F08, are not well founded
4-Formyl-2-nitrophenyl 3-nitro-2-methylbenzoate
In the title formyl nitro aryl benzoate derivative, CH NO, the benzene rings form a dihedral angle of 4.96(3)°. The mean plane of the central ester group, C-O-C-(=O)-C (r.m.s. deviation = 0.0484Å), is twisted away from the formyl nitro aryl and benzoate rings by 46.61(5) and 49.93(5)°, respectively. In the crystal, the molecules are packed forming C-H⋯O interactions in chains which propagate along [010]. Edge-fused R 3(15) rings are generated along this direction
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