Decrease in heliospheric magnetic flux in this solar minimum: Recent Ulysses magnetic field observations

By E. Smith, A. Balogh. 2008

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In Astronomy and Astrophysics

Citations in the corpus

Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval (2008, background): “Ulysses polar observations through late 2008, in particular, suggest that i) the interplanetary magnetic field (IMF) was ≈36% lower than the previous minimum (Smith and Balogh, 2008); ii) the scaled number density was ≈17% lower (Issautier et al.”
ON THE WEAKENING OF THE POLAR MAGNETIC FIELDS DURING SOLAR CYCLE 23 (2009, background): “…in the last column of Table 1, the radial IMF strength |BIMFr | measured at Earth is now 67% of its 1996 value, having decreased from 2.0 nT to 1.3 nT. Similarly, the radial IMF strength recorded by Ulysses over the south pole during 2006–2007 was 64% of its value in 1994 (Smith & Balogh 2008).”
The Heliospheric Magnetic Field (2013, background): “However, we note here that the most recent solar minimum between the end of solar cycle 23 and the start of cycle 24, centred around 2008 – 2009, has been longest and deepest of the space age, with the lowest 𝐵 and Φ directly observed (Smith and Balogh, 2008; Lockwood et al., 2009a,b).”
Near-earth solar wind flows and related geomagnetic activity during more than four solar cycles (1963-2011) (2012, background): “The unusually low values of geomagnetic activity (Tsurutani et al. 2011) and magnetic field strength (Smith & Balogh 2008; Connick et al. 2011) in the recent solar minimum are evident in Figure 7 and are observed in both slow solar wind and corotating streams.”
Anthropogenic and Natural Radiative Forcing (2014, background): “However, SC 23 showed an activity decline not previously seen in the satellite era (McComas et al., 2008; Smith and Balogh, 2008; Russell et al., 2010).”
RECORD-SETTING COSMIC-RAY INTENSITIES IN 2009 AND 2010 (2010, background): “…2010 (Figures 1(b) and (c)), and the Sun entered an unfamiliar state characterized by much weaker polar and interplanetary magnetic fields (IMFs; Smith & Balogh 2008; Lee et al. 2009; Figure 1(d)) and by greatly reduced solar-wind density and dynamic pressure (McComas et al. 2008; Figure 1(f)).”
Weaker solar wind from the polar coronal holes and the whole Sun (2008, background): “Remarkably, the average radial field strength in the PCHs during Ulysses third orbit was significantly lower (about one third) [Smith and Balogh, 2008] compared to the measured radial field in the fast wind during the first orbit [Balogh et al., 1995].”
The Open Flux Problem (2017, background): “Ulysses measurements demonstrated that the magnitude of the radial IMF is nearly independent of heliographic latitude (Smith & Balogh 1995, 2008), implying that currents in the heliosphere are primarily confined to the heliospheric current sheet (HCS) and that the field is nearly potential…”