High‐Speed Solar Wind Streams in 2007–2008: Turning on the Russell‐McPherron Effect

Munteanu, Costel; Hamada, Amr; Мурсула, К.

doi:10.1029/2019ja026846

Cited by 5 publications

(11 citation statements)

References 50 publications

(68 reference statements)

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“…The magnetosphere itself reacts through a series of geomagnetic storms that follows in general the periodic trends of interplanetary driving. However, some notable differences are observed as discussed by Munteanu, Hamada, and Mursula (2019). They demonstrated that the Russell-McPherron (R-M) effect (Russell & McPherron, 1973) systematically increased (decreased) the geoeffectiveness of the negative (positive) polarity HSS/CIR streams.…”

Section: Data Set and Analysis Methodologymentioning

confidence: 96%

“…However, some notable differences are observed as discussed by Munteanu et al (2019). They demonstrated that the Russell-McPherron (R-M) effect (Russell and McPherron, 1973) systematically increased (decreased) the geoeffectiveness of the negative (positive) polarity HSS/CIR streams.…”

Section: Dataset and Analysis Methodologymentioning

confidence: 96%

“…The extent of the differences in seasonal variability can be glean by comparing Panels 1a,c with 2a,c, and the differences in ionospheric response is evident by comparing Panels 1b,d with 2b,d. For example, the beginning of the negative storm phase at Millstone Hill is a full day later than at RAL for the event commencing on March 25, 2008, The variations in solar wind velocity, density, magnetic field exhibit several periodicities linked to the interaction of these structures with the Earth's magnetosphere and are subject of several studies (see e.g., Munteanu, Hamada, & Mursula, 2019). The magnetosphere itself reacts through a series of geomagnetic storms that follows in general the periodic trends of interplanetary driving.…”

Section: Data Set and Analysis Methodologymentioning

confidence: 99%

“…This can potentially give rise to discrepancies in the dynamic range and sampling characterizing each station. A sample time series spanning 4 months of data from the RAL ionosonde is displayed in Figure 1, and it shows the impact of 10 geomagnetic storms caused by recurring CIR/HSS events, where the areas shaded with red and blue denote the time periods associated with the two HSS/CIR sequences identified by Munteanu, Hamada, and Mursula (2019). Also, a 10‐day long subset from the same location highlights the ionospheric response to two particular geomagnetic events, started around March 26, 2003 and April 4, 2008 in Figures 1b and 1d.…”

Section: Data Set and Analysis Methodologymentioning

confidence: 99%

“…For example, the beginning of the negative storm phase at Millstone Hill is a full day later than at RAL for the event commencing on March 25, 2008, while for the NEGREA ET AL. The variations in solar wind velocity, density, magnetic field exhibit several periodicities linked to the interaction of these structures with the Earth's magnetosphere and are subject of several studies (see e.g., Munteanu, Hamada, & Mursula, 2019). The magnetosphere itself reacts through a series of geomagnetic storms that follows in general the periodic trends of interplanetary driving.…”

Section: Data Set and Analysis Methodologymentioning

confidence: 99%

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Global Ionospheric Response to a Periodic Sequence of HSS/CIR Events During the 2007–2008 Solar Minimum

2021

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The thermosphere-ionosphere system constitutes the upper-most layer of the Earth's atmosphere and is characterized by high variability and a strong dependence on external drivers. The two main categories of forcings are solar radiation and geomagnetic activity at high latitudes. Under normal conditions, solar radiation is the dominant source of energy and momentum, generating the standard structure, composition, and circulation of the thermosphere-ionosphere (Fuller-Rowell, 2014;Rishbeth & Garriott, 1969). During geomagnetic storms, the energy input at high latitudes can be significant, or even dominant. During such events, there is an increase of particle precipitation and Joule heating (Codrescu et al., 1995) at high latitudes, together with penetration electric fields at mid-and low-latitudes. The resulting plasma drift and associated ion-drag will heat up the neutral atmosphere, inducing pressure gradients that can alter the global neutral circulation from a dayside-nightside pattern of winds to an equatorward pattern. Additionally, since the Joule heating maximum occurs around 100-120 km altitude, the heavier molecular species dominant here (molecular oxygen and molecular nitrogen) will be displaced toward higher altitudes, while the atomic oxygen density will decrease due to equatorward winds (Fuller-Rowell et al., 1994). The resulting modified chemical composition will in turn lead to a higher plasma loss rate through charge exchange and recombination, as well as a decrease in plasma production due to the loss of atomic oxygen.The occurrence of geomagnetic storms is linked to solar activity and transient events in the solar wind. During the descending and minimum phases of a solar cycle, the near-Earth solar wind is dominated by highspeed streams (HSSs) and their associated stream interaction regions (SIRs), characterized by increased plasma density and magnetic field intensity. These structures are formed when the fast-solar wind emanating from a solar coronal hole (CH) "collides" with the slower solar wind ahead of it. Coronal holes lasting for several solar rotations will generate recurring SIRs, also known as corotating interaction regions (CIRs). The ionospheric impact of geomagnetic storms and of HSS/CIR sequences is an active area of research, with multiple recent studies employing a variety of data types and approaches: TEC (

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Section: Data Set and Analysis Methodologymentioning

confidence: 96%

Section: Dataset and Analysis Methodologymentioning

confidence: 96%

Section: Data Set and Analysis Methodologymentioning

confidence: 99%

Section: Data Set and Analysis Methodologymentioning

confidence: 99%

Section: Data Set and Analysis Methodologymentioning

confidence: 99%

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Global Ionospheric Response to a Periodic Sequence of HSS/CIR Events During the 2007–2008 Solar Minimum

2021

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Semi-annual, annual and Universal Time variations in the magnetosphere and in geomagnetic activity: 3. Modelling

Lockwood

Owens

Barnard

et al. 2020

J. Space Weather Space Clim.

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This is the third in a series of papers that investigate the semi-annual, annual and Universal Time variations in the magnetosphere. In this paper we use the Lin et al. (2010) empirical model of magnetopause locations, along with the assumption of pressure equilibrium and the Newtonian approximation of magnetosheath pressure. We show that the equinoctial pattern arises in both the cross-tail current at the tail hinge point and in the total energy stored in the tail. The model allows us to study the effects of both dipole tilt and hemispheric asymmetries. As a test of the necessary assumptions made to enable this analysis, we also study simulations by the BATSRUS global MHD magnetosphere model. These also show that the reconnection rate in the tail is greatest when the dipole tilt is small but this only applies at low solar wind dynamic pressure, p SW , and does not on its own explain why the equinoctial effect increases in amplitude with increased p SW , as demonstrated by Paper 2. Instead, the effect is consistent with the dipole tilt effect on the energy stored in the tail around the reconnection X line. A key factor is that a smaller/larger fraction of the open polar cap flux threads the tail lobe in the hemisphere that is pointed toward/away from the Sun. The analysis using the empirical model uses approximations and so is not definitive; however, because the magnetopause locations in the two hemispheres were fitted separately in generating the model, it gives an unique insight into the effect of the very different offsets of the magnetic pole from the rotational pole in the two hemispheres. It is therefore significant that our analysis using the empirical model does predict a UT variation that is highly consistent with that found in both transpolar voltage data and in geomagnetic activity.

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Properties of the solar wind parameters associated with the enhanced Russell-McPherron Effect in March 2008

Zhao

2023

Preprint

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We study the properties of the solar wind parameter associated with the enhanced Russell-McPherron (R-M) effect that occurred on 8–9 March 2008. The solar wind during the period from 01:33 UT and 05:24 UT on 9 March 2008 (hereafter Period2) makes a dominant contribution to the ring current intensity of the geomagnetic storm that occurred on 8–9 March 2008. It is usually accepted that the enhanced R-M effect is due to the negative ByGSE around the spring equinox. However, we found that ByGSE are positive during most of Period2. The enhanced R-M effect described by the enhanced ring current effect estimated by the empirical formulae created by Burton et al. (1975) and by O’Brien & McPherron (2000) for the solar wind during Period2 are −33.23 nT and −26.45 nT, respectively. However, the real ring current effect caused by the solar wind during Period2 is −88.10 nT. The reason that we find is that the solar wind dynamic pressure is high during Period2. The results of this study indicate that the enhanced R-M effect described by the enhanced ring current effect not only depends BzGSM, but also depends on the solar wind dynamic pressure. The enhanced ring current effect around the spring equinox of 2008 caused by BzGSM, is amplified by the solar wind dynamic pressure by about 3 times.

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High‐Speed Solar Wind Streams in 2007–2008: Turning on the Russell‐McPherron Effect

Cited by 5 publications

References 50 publications

Global Ionospheric Response to a Periodic Sequence of HSS/CIR Events During the 2007–2008 Solar Minimum

Global Ionospheric Response to a Periodic Sequence of HSS/CIR Events During the 2007–2008 Solar Minimum

Semi-annual, annual and Universal Time variations in the magnetosphere and in geomagnetic activity: 3. Modelling

Properties of the solar wind parameters associated with the enhanced Russell-McPherron Effect in March 2008

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