Elena Provornikova's research while affiliated with Johns Hopkins University and other places

Publications (4)

Article
Full-text available
We examine the different element abundances exhibited by the closed loop solar corona and the slow speed solar wind. Both are subject to the first ionization potential (FIP) effect, the enhancement in coronal abundance of elements with FIP below 10 eV (e.g., Mg, Si, Fe) with respect to high-FIP elements (e.g., O, Ne, Ar), but with subtle difference...
Preprint
We examine the different element abundances exhibited by the closed loop solar corona and the slow speed solar wind. Both are subject to the First Ionization Potential (FIP) Effect, the enhancement in coronal abundance of elements with FIP below 10 eV (e.g. Mg, Si, Fe) with respect to high FIP elements (e.g. O, Ne, Ar), but with subtle differences....
Article
Full-text available
Magnetic reconnection in the solar corona is thought to be unstable to the formation of multiple interacting plasmoids, and previous studies have shown that plasmoid dynamics can trigger MHD waves of different modes propagating outward from the reconnection site. However, variations in plasma parameters and magnetic field strength in the vicinity o...
Article
It has been proposed that particles bouncing between magnetized flows converging in a reconnection region can be accelerated by the first order Fermi mechanism. Analytical considerations of this mechanism have shown that the spectral index of accelerated particles is related to the total plasma compression within the reconnection region similarly t...

Citations

... In particular, in closed-loop systems, low (\10 eV) first ionization potential (FIP) elements are occasionally more abundant in the corona than in the photosphere, by a factor ranging from 2 to 4. In contrast, the plasma composition in open magnetic field regions remains practically unfractionated between the lower and upper solar atmosphere (Sheeley 1995(Sheeley , 1996Baker et al. 2013, to mention but a few examples). Interestingly, the FIP bias is also observed in the solar wind (Schwadron et al. 1999;Laming et al. 2019) and could, therefore, be used to infer the magnetic connectivity in the heliosphere, and possibly help to identify the sources of the solar wind itself (Brooks et al. 2015). This is of primary importance to investigate and identify the solar wind acceleration mechanisms, which is one of the fundamental questions that the Solar Orbiter mission is being specifically designed to address through a combination of both remote sensing and in-situ instruments. ...
... With such a generalization, one can study interesting subjects such as the magnetic reconnection region and the coronal plume structure. 32,51 Finally, we point out that when a giant overreflection occurs, some nonlinear effects can occur due to the large enhancement of the field amplitudes. Future work in those directions will be of great interest. ...
... Note that space plasmas, e.g., in the solar corona, the solar wind, and the Earth's magnetosheath, show variability in various characteristic parameters such as the plasma β (the ratio of thermal-tomagnetic pressure) and the corresponding compressibility. The compression effect was found to be important for reconnection and particle acceleration in low-β plasmas (Birn et al. 2012;Drury 2012;Zank et al. 2014;Provornikova et al. 2016;Montag et al. 2017;Li et al. 2018;Zenitani & Miyoshi 2020). Here we only consider incompressive effects (Drake et al. 2006), which are expected to be dominant in high-β regimes; see, for example, Chhiber et al. (2018), Eriksson et al. (2018), and Wang et al. (2021). ...