scholarly journals Cosmic radio noise absorption in the high-latitude ionosphere during solar wind high-speed streams

2017 ◽  
Vol 122 (5) ◽  
pp. 5203-5223 ◽  
Author(s):  
M. Grandin ◽  
A. T. Aikio ◽  
A. Kozlovsky ◽  
T. Ulich ◽  
T. Raita
Keyword(s):  
Solar Wind ◽  
High Latitude ◽  
High Speed ◽  
Cosmic Radio ◽  
Radio Noise ◽  
Noise Absorption ◽  
High Latitude Ionosphere

scholarly journals Effects of solar wind high-speed streams on the high-latitude ionosphere: Superposed epoch study

2015 ◽  
Vol 120 (12) ◽  
pp. 10,669-10,687 ◽  
Author(s):  
M. Grandin ◽  
A. T. Aikio ◽  
A. Kozlovsky ◽  
T. Ulich ◽  
T. Raita
Keyword(s):  
Solar Wind ◽  
High Latitude ◽  
High Speed ◽  
High Latitude Ionosphere

scholarly journals Cosmic radio-noise absorption bursts caused by solar wind shocks

2004 ◽  
Vol 22 (8) ◽  
pp. 2973-2987 ◽  
Author(s):  
A. Osepian ◽  
S. Kirkwood
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Geomagnetic Storms ◽  
Quantitative Description ◽  
Threshold Value ◽  
Cosmic Radio ◽  
Radio Noise ◽  
Field Perturbation ◽  
Noise Absorption ◽  
Cyclotron Instability

Abstract. Bursts of cosmic noise absorption observed at times of sudden commencements (SC) of geomagnetic storms are examined. About 300SC events in absorption for the period 1967-1990 have been considered. It is found that the response of cosmic radio-noise absorption to the passage of an interplanetary shock depends on the level of the planetary magnetic activity preceding the SC event and on the magnitude of the magnetic field perturbation associated with the SC (as measured in the equatorial magnetosphere). It is shown that for SC events observed against a quiet background (Kp<2), the effects of the SC on absorption can be seen only if the magnitude of the geomagnetic field perturbation caused by the solar wind shock exceeds a threshold value ΔBth. It is further demonstrated that the existence of this threshold value, ΔBth, deduced from experimental data, can be related to the existence of a threshold for exciting and maintaining the whistler cyclotron instability, as predicted by quasi-linear theory. SC events observed against an active background (Kp<2) are accompanied by absorption bursts for all magnetic field perturbations, however small. A quantitative description of absorption bursts associated with SC events is provided by the whistler cyclotron instability theory.

scholarly journals Cosmic radio noise absorption events associated with equatorward drifting arcs during a substorm growth phase

2004 ◽  
Vol 22 (5) ◽  
pp. 1675-1686 ◽  
Author(s):  
J. R. T. Jussila ◽  
A. T. Aikio ◽  
S. Shalimov ◽  
S. R. Marple
Keyword(s):  
Electron Temperature ◽  
Electric Fields ◽  
Growth Phase ◽  
Energetic Electron ◽  
Cosmic Radio ◽  
Radio Noise ◽  
Particle Precipitation ◽  
Noise Absorption ◽  
D Region ◽  
E Region

Abstract. Cosmic radio noise absorption (CNA) events associated with equatorward drifting arcs during a substorm growth phase are studied by using simultaneous optical auroral, IRIS imaging riometer and EISCAT incoherent scatter radar measurements. The CNA is generally attributed to energetic particle precipitation in the D-region. However, it has been argued that plasma irregularities or enhanced electron temperature (Te) in the E-region could also produce CNA. Both of the latter mechanisms are related to intense electric fields in the ionosphere. We present two events which occur during a substorm growth phase in the evening MLT sector. In both of the events, an auroral arc is drifting equatorward, together with a region of CNA (auroral absorption bay) located on the equatorward side and outside of the arc. Both of the events are associated with enhanced D-region electron density on the equatorward side of the auroral arc, but in the second event, a region of intense electric field and enhanced electron temperature in the E-region is also located on the equatorward side of the arc. We show that in the studied events neither plasma instabilities nor enhanced Te play a significant role in producing the measured CNA, but the CNA in the vicinity of the equatorward drifting arcs is produced by D-region energetic electron precipitation. Key words. Ionosphere (auroral ionosphere; particle precipitation; electric fields and currents)

scholarly journals Statistical signature of active D-region HF heating in IRIS riometer data from 1994–2004

2007 ◽  
Vol 25 (2) ◽  
pp. 407-415 ◽  
Author(s):  
A. Kero ◽  
C.-F. Enell ◽  
Th. Ulich ◽  
E. Turunen ◽  
M. T. Rietveld ◽  
...  
Keyword(s):  
Present Theory ◽  
Cosmic Radio ◽  
Radio Noise ◽  
3 Dimensional ◽  
Noise Absorption ◽  
D Region ◽  
Order Of Magnitude ◽  
Representative Model ◽  
Vertical Beam ◽  
Hf Heating

Abstract. In this paper we study the effect of artificial HF heating on cosmic radio noise absorption in the D-region ionosphere. The effect has earlier been studied theoretically in idealised cases and without experimental verification. Here we present a 3-dimensional modelling of the effect, taking into account the directivity patterns of the vertical beam of the EISCAT Heater at Tromsø, Norway, and the intersecting beam of the IRIS imaging riometer at Kilpisjärvi, Finland. The heater-induced enhancement of cosmic radio noise absorption at the IRIS frequency (38.2 MHz) is estimated to be between 0.02 dB and 0.05 dB in the most representative model cases. However, a statistical study of IRIS data from a selected set of heating experiments carried out during the years 1994–2004 shows that the median effect is between 0.002 dB and 0.004 dB, i.e. an order of magnitude less than theoretically predicted. This indicates that the actual HF heating effect at D-region altitudes is substantially overestimated by the present theory.

scholarly journals The dependence of high-latitude PcS wave power on solar wind velocity and on the phase of high-speed solar wind streams

1998 ◽  
Vol 103 (A11) ◽  
pp. 26271-26283 ◽  
Author(s):  
Mark Engebretson ◽  
Karl-Heinz Glassmeier ◽  
Martin Stellmacher ◽  
W. Jeffrey Hughes ◽  
Hermann Lühr
Keyword(s):  
Solar Wind ◽  
Wind Velocity ◽  
High Latitude ◽  
High Speed ◽  
Solar Wind Velocity ◽  
Wave Power ◽  
Speed Solar Wind ◽  
High Speed Solar Wind

scholarly journals Multi beam observations of cosmic radio noise using a VHF radar with beam forming by a Butler matrix

2011 ◽  
Vol 9 ◽  
pp. 349-357 ◽  
Author(s):  
T. Renkwitz ◽  
W. Singer ◽  
R. Latteck ◽  
M. Rapp
Keyword(s):  
Middle Atmosphere ◽  
Beam Forming ◽  
Cosmic Radio ◽  
Radio Noise ◽  
Spatiotemporal Resolution ◽  
Vhf Radar ◽  
Butler Matrix ◽  
The North ◽  
Noise Absorption ◽  
Cosmic Noise

Abstract. The Leibniz-Institute of Atmospheric Physics (IAP) in Kühlungsborn started to install a new MST radar on the North-Norwegian island Andøya (69.30° N, 16.04° E) in 2009. The new Middle Atmosphere Alomar Radar System (MAARSY) replaces the previous ALWIN radar which has been successfully operated for more than 10 years. The MAARSY radar provides increased temporal and spatial resolution combined with a flexible sequential point-to-point steering of the radar beam. To increase the spatiotemporal resolution of the observations a 16-port Butler matrix has been built and implemented to the radar. In conjunction with 64 Yagi antennas of the former ALWIN antenna array the Butler matrix simultaneously provides 16 individual beams. The beam forming capability of the Butler matrix arrangement has been verified observing the galactic cosmic radio noise of the supernova remnant Cassiopeia A. Furthermore, this multi beam configuration has been used in passive experiments to estimate the cosmic noise absorption at 53.5 MHz during events of enhanced solar and geomagnetic activity as indicators for enhanced ionization at altitudes below 90 km. These observations are well correlated with simultaneous observations of corresponding beams of the co-located imaging riometer AIRIS (69.14° N, 16.02° E) at 38.2 MHz. In addition, enhanced cosmic noise absorption goes along with enhanced electron densities at altitudes below about 90 km as observed with the co-located Saura MF radar using differential absorption and differential phase measurements.

scholarly journals Cosmic radio noise absorption related to structures in auroral luminosity

1997 ◽  
Vol 102 (A4) ◽  
pp. 7439-7447 ◽  
Author(s):  
P. H. Stoker ◽  
M. J. Mathews ◽  
M. W. J. Scourfield
Keyword(s):  
Cosmic Radio ◽  
Radio Noise ◽  
Noise Absorption ◽  
Auroral Luminosity

Recurrent high-speed solar wind co-rotating interaction region imprint on the ionosphere and atmosphere: GPS TEC variations and atmospheric gravity waves

2020 ◽  
Author(s):  
James M. Weygand ◽  
Paul Prikryl ◽  
Reza Ghoddousi-Fard ◽  
Lidia Nikitina ◽  
Bharat S. R. Kunduri
Keyword(s):  
Solar Wind ◽  
Gravity Waves ◽  
High Latitude ◽  
High Speed ◽  
Geomagnetic Storms ◽  
Coronal Holes ◽  
Lower Thermosphere ◽  
Ionospheric Currents ◽  
Atmospheric Gravity Waves ◽  
Atmospheric Gravity

&lt;p&gt;High-speed streams (HSS) from coronal holes dominate solar wind structure in the absence of coronal mass ejections during solar minimum and the descending branch of solar cycle. Prominent and long-lasting coronal holes produce intense co-rotating interaction regions (CIR) on the leading edge of high-speed plasma streams that cause recurrent ionospheric disturbances and geomagnetic storms. Through solar wind coupling to the magnetosphere-ionosphere-atmosphere (MIA) system they affect the ionosphere and neutral atmosphere at high latitudes, and, at mid to low latitudes, by the transmission of the electric fields [1] and propagation of atmospheric gravity waves from the high-latitude lower thermosphere [2].&lt;/p&gt;&lt;p&gt;The high-latitude ionospheric structure, caused by precipitation of energetic particles, strong ionospheric currents and convection, results in changes of the GPS total electron content (TEC) and rapid variations of GPS signal amplitude and phase, called scintillation [3]. The GPS phase scintillation is observed in the ionospheric cusp, polar cap and auroral zone, and is particularly intense during geomagnetic storms, substorms and auroral breakups. Phase scintillation index is computed for a sampling rate of 50 Hz by specialized GPS scintillation receivers from the Canadian High Arctic Ionospheric Network (CHAIN). A proxy index of phase variation is obtained from dual frequency measurements of geodetic-quality GPS receivers sampling at 1 Hz, which include globally distributed receivers of the RT-IGS network that are monitored by the Canadian Geodetic Survey in near-real-time [4]. Temporal and spatial changes of TEC and phase variations following the arrivals of HSS/CIRs [5] are investigated in the context of ionospheric convection and equivalent ionospheric currents derived from&amp;#160; a ground magnetometer network using the spherical elementary current system method [6,7].&lt;/p&gt;&lt;p&gt;The Joule heating and Lorentz forcing in the high-latitude lower thermosphere have long been recognized as sources of internal atmospheric gravity waves (AGWs) [2] that propagate both upward and downward, thus providing vertical coupling between atmospheric layers. In the ionosphere, they are observed as traveling ionospheric disturbances (TIDs) using various techniques, e.g., de-trended GPS TEC maps [8].&lt;/p&gt;&lt;p&gt;In this paper we examine the influence on the Earth&amp;#8217;s ionosphere and atmosphere of a long-lasting HSS/CIRs from recurrent coronal holes at the end of solar cycles 23 and 24. The solar wind MIA coupling, as represented by the coupling function [9], was strongly increased during the arrivals of these HSS/CIRs.&lt;/p&gt;&lt;p&gt;&amp;#160;&lt;/p&gt;&lt;p&gt;[1] Kikuchi, T. and K. K. Hashimoto, Geosci. Lett. , 3:4, 2016.&lt;/p&gt;&lt;p&gt;[2] Hocke, K. and K. Schlegel, Ann. Geophys., 14, 917&amp;#8211;940, 1996.&lt;/p&gt;&lt;p&gt;[3] Prikryl, P., et al., J. Geophys. Res. Space Physics, 121, 10448&amp;#8211;10465, 2016.&lt;/p&gt;&lt;p&gt;[4] Ghoddousi-Fard et al., Advances in Space Research, 52(8), 1397-1405, 2013.&lt;/p&gt;&lt;p&gt;[5] Prikryl et al. Earth, Planets and Space, 66:62, 2014.&lt;/p&gt;&lt;p&gt;[6] Amm O., and A. Viljanen, Earth Planets Space, 51, 431&amp;#8211;440, 1999.&lt;/p&gt;&lt;p&gt;[7] Weygand J.M., et al., J. Geophys. Res., 116, A03305, 2011.&lt;/p&gt;&lt;p&gt;[8] Tsugawa T., et al., Geophys. Res. Lett., 34, L22101, 2007.&lt;/p&gt;&lt;p&gt;[9] Newell P. T., et al., J. Geophys. Res., 112, A01206, 2007.&lt;/p&gt;

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