scholarly journals Statistics of auroral hiss and relationship to auroral boundaries and upward current regions

2016 ◽  
Vol 121 (8) ◽  
pp. 7547-7560 ◽  
Author(s):  
M. Spasojevic
Keyword(s):  
Auroral Hiss ◽  
Upward Current

scholarly journals Low-frequency impulsive auroral hiss observations at high geomagnetic latitudes

1998 ◽  
Vol 103 (A9) ◽  
pp. 20459-20468 ◽  
Author(s):  
J. LaBelle ◽  
A. T. Weatherwax ◽  
J. Perring ◽  
E. Walsh ◽  
M. L. Trimpi ◽  
...  
Keyword(s):  
Low Frequency ◽  
Auroral Hiss

Quasiperiodic Saturn Auroral Hiss Observed During a Cassini Proximal Orbit

2020 ◽  
Vol 125 (1) ◽  
Author(s):  
J. D. Menietti ◽  
B. Palmaerts ◽  
J. Zahlava ◽  
T. F. Averkamp ◽  
J. B. Groene ◽  
...  
Keyword(s):  
Auroral Hiss

III. Spectroscopic observations of the sun

1867 ◽  
Vol 15 ◽  
pp. 256-258 ◽  
Keyword(s):  
The Other ◽  
The Sun ◽  
Chemical Action ◽  
Spectroscopic Observations ◽  
Gaseous Mass ◽  
Other Hand ◽  
Sun Spots ◽  
Physical Constitution ◽  
Upward Current

The two most recent theories dealing with the physical constitution of the sun are due to M. Faye and to Messrs. De la Rue, Balfour Stewart, and Loewy. The chief point of difference in these two theories is the explanation given by each of the phenomena of sun-spots. Thus, according to M. Faye, the interior of the sun is a nebulous gaseous mass of feeble radiating-power, at a temperature of dissociation; the photosphere is, on the other hand, of a high radiating-power, and at a temperature sufficiently low to permit of chemical action. In a sunspot we see the interior nebulous mass through an opening in the photosphere, caused by an upward current, and the sun-spot is black, by reason of the feeble radiating-power of the nebulous mass.

Multipayload interferometric wave vector determination of auroral hiss

2012 ◽  
Vol 117 (A2) ◽  
pp. n/a-n/a ◽  
Author(s):  
E. T. Lundberg ◽  
P. M. Kintner ◽  
S. P. Powell ◽  
K. A. Lynch
Keyword(s):  
Wave Vector ◽  
Auroral Hiss

Estimating the Size and Location of the Region of Scattering of the Auroral Hiss, According to Data from High-Latitude Observations at Three Separated Places

2021 ◽  
Vol 85 (3) ◽  
pp. 287-291
Author(s):  
A. S. Nikitenko ◽  
O. M. Lebed ◽  
Yu. V. Fedorenko ◽  
J. Manninen ◽  
N. G. Kleimenova ◽  
...  
Keyword(s):  
High Latitude ◽  
Auroral Hiss

scholarly journals Ionospheric signatures during a magnetospheric flux rope event

2008 ◽  
Vol 26 (12) ◽  
pp. 3967-3977 ◽  
Author(s):  
L. Juusola ◽  
O. Amm ◽  
H. U. Frey ◽  
K. Kauristie ◽  
R. Nakamura ◽  
...  
Keyword(s):  
Flux Rope ◽  
Recovery Phase ◽  
Expansion Phase ◽  
Northern Fennoscandia ◽  
Ionospheric Region ◽  
Image Satellite ◽  
Imaging Camera ◽  
Flux Ropes ◽  
Field Aligned Current ◽  
Upward Current

Abstract. On 13 August 2002, during a substorm, Cluster encountered two earthward moving flux ropes (FR) in the central magnetotail. The first FR was observed during the expansion phase of the substorm, and the second FR during the recovery phase. In the conjugate ionospheric region in Northern Fennoscandia, the ionospheric equivalent currents were observed by the MIRACLE network and the auroral evolution was monitored by the Wideband Imaging Camera (WIC) on-board the IMAGE satellite. Extending the study of Amm et al. (2006), we examine and compare the possible ionospheric signatures associated with the two FRs. Amm et al. studied the first event in detail and found that the ionospheric footprint of Cluster coincided with a region of downward field-aligned current. They suggested that this region of downward current, together with a trailing region of upward current further southwestward, might correspond to the ends of the FR. Unlike during the first FR, however, we do not see any clear ionospheric features associated with the second one. In the GSM xy-plane, the first flux rope axis was tilted with respect to the y-direction by 29°, while the second flux rope axis was almost aligned in the y-direction, with an angle of 4° only. It is possible that due to the length and orientation of the second FR, any ionospheric signatures were simply mapped outside the region covered by the ground-based instruments. We suggest that the ground signatures of a FR depend on the orientation and the length of the structure.

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