When the Earth’s atmosphere becomes dynamic…

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Number: xxxwarning.png"xxx" is not a number.
1st Author: Manuela Temmer
2nd Author: Sandro Krauss, Astrid Veronig
Published: 20 January 2016
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Introduction

Flares are well known to produce ionospheric effects (see Nugget 251). For large flare events, the neutral density in the thermosphere shows enhancements, mainly caused by the solar EUV flux inserted into this layer of the atmosphere (e.g., Krauss et al., 2012). Energy input via the magnetosphere is observed for the flare associated coronal mass ejections (CMEs). Especially, the CME embedded flux rope with a southward magnetic field orientation, may cause an increase in the neutral density, causing an altitude decrease of Earth-orbiting satellites. Figure 1 illustrates the thermospheric temperature response to high solar EUV flux. Enhanced ionization (IN) and photochemical processes like photo-dissociation (PD) and dissociative recombination (DR) eventually lead to heating and subsequent expansion of the upper atmosphere and to the production of suprathermal atoms which may influence the energy balance in the thermosphere. Flares and CMEs, a well-known compound of solar activity, are therefore important for a better understanding of the “dynamics” of our Earth’s atmosphere. Vice versa, by studying the atmospheric response to solar activity, we derive a deeper insight into the physics of solar flares and CMEs – a win-win situation.

Figure 1: Temperature response in the thermosphere for increased solar EUV flux. Adapted from Krauss et al. (2012).


Thermospheric response to CMEs

The Gravity Recovery And Climate Experiment (GRACE) satellites and their accelerometer measurements can be used to calculate the variations in the neutral density at altitudes of 450-500 km. We studied a set of 104 Earth-directed CMEs (see the catalogue by Richardson & Cane, 2010) that occured from July 2003 and August 2010, and compared the CME impact characteristics with the geomagnetic response. Each CME event was analyzed in detail by using in-situ plasma and magnetic field data taken from the ACE satellite. Thus, characteristic CME parameters such as the impact speed (vmax) and the southward magnetic field strength (Bz) were extracted.

The results clearly show that the majority of CMEs is able to cause a distinct density enhancement in the thermosphere, with an increase up to a factor of 8 compared to the pre-event level. The highest correlations are derived for the CME Bz component with values greater than 10nT, while the correlation with the CME impact speed is somewhat smaller (see Figure 2). We also find that the density enhancement in the thermosphere is highly correlated to the Dst index (see Figure 3).

Figure 2: Latitude-time plot of thermospheric densities derived from GRACE accelerometry. The impact of three CMEs in July 2004 inducing severe geomagnetic storms can be identified in the density increase and the magnetic field measurements observed by ACE (white line). Adapted from Krauss et al. (2015).

The response to the impacting CME was also studied separately for the shock-sheath region and the magnetic flux rope. From this it is found that the Dst and SYM-H geomagnetic indices reveal a tighter relation to the Bz minimum value in the magnetic structure of the CME, whereas the polar cap geomagnetic indices show higher correlations with the Bz minimum in the shock-sheath region (see also Huttunen and Koskinen, 2004 JGR). Since the strength of the Bz component—either in the sheath or in the magnetic structure of the ICME—is highly correlated with the neutral density enhancement, we may use this relation to estimate satellite orbital decays based on magnetic field measurements at L1, i.e., before the CME hits the Earth magnetosphere. These results are expected to further stimulate progress in space weather understanding and applications regarding satellite operations.


Figure 3: Scatterplots of the increase in the neutral thermospheric density and the geomagnetic Dst index. The correlation coefficients and the linear regression coefficients together with the standard deviation for a 90% confidence interval are given in the inset. Adapted from Krauss et al. (2015).

References

[1] Huttunen, K. and H. Koskinen (2004), Importance of post-shock streams and sheath region as drivers of intense magnetospheric storms and high-latitude activity, Annales Geophysicae, vol. 22, Issue 5, pp.1729-1738 [2] Krauss, S., M. Temmer, A. Veronig,
O. Baur, and H. Lammer (2015), Thermospheric and geomagnetic responses to interplanetary coronal mass ejections observed by ACE and GRACE: Statistical results, J. Geophys. Res. Space Physics, 120, 8848–8860, doi:10.1002/2015JA021702. 
 [3] Krauss, S., B. Fichtinger, L. Lammer, et al. (2012), Solar flares as proxy for the young Sun: satellite observed thermosphere response to an X17.2 flare of Earth's upper atmosphere, Annales Geophysicae, Volume 30, Issue 8, 2012, pp.1129-1141 [4] Richardson, I. G. and H.V. Cane (2010), Near-Earth Interplanetary Coronal Mass Ejections During Solar Cycle 23 (1996 - 2009): Catalog and Summary of Properties, Solar Physics, Volume 264, Issue 1, pp.189-237

Facts about When the Earth’s atmosphere becomes dynamic…RDF feed
RHESSI Nugget Date20 January 2016  +
RHESSI Nugget First AuthorManuela Temmer  +
RHESSI Nugget Indexwarning.png"xxx" is not a number.
RHESSI Nugget Second AuthorSandro Krauss, Astrid Veronig  +
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