Global Solar Free Magnetic Energy and Electric Current Density Distribution of Carrington Rotation 2124

Tadesse, Tilaye; Pevtsov, Alexei A.; Wiegelmann, T.; MacNeice, P. J.; Gosain, Sanjay

doi:10.1007/s11207-014-0581-z

Cited by 14 publications

(4 citation statements)

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“…Our hypothesis is partly supported by coronal decay index arguments as well as faint eruptive changes in the structure of the corona observed in the STEREO A and B EUVI 195 Å channel. In future studies, we plan to search for more such events and corroborate our results with rigorous decay index calculations employing global potential fields as well as NLFFF computations (Tadesse et al 2014a(Tadesse et al , 2014b) that use full-disk as well as synoptic vector maps (Gosain et al 2013). Further, it may be interesting to perform a numerical simulation for such a scenario and compare the results to the observations.…”

Section: Summary and Discussionmentioning

confidence: 65%

Interrupted Eruption of Large Quiescent Filament Associated With a Halo Cme

Gosain

Filippov

Maurya

et al. 2016

ApJ

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We analyze the observations of an eruptive quiescent filament associated with a halo Coronal Mass Ejection (CME). We use observations from the Atmospheric Imaging Assembly (AIA) instrument onboard the Solar Dynamics Observatory (SDO), Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO), and the Solar Terrestrial Relations Observatory (STEREO A/B) satellites. The filament exhibits a slow-rise phase followed by a gradual acceleration and then completely disappears. The filament could be traced in STEREO observations up to an altitude of about 1.44  R , where its rise speed reached ∼14 km s −1 and disappeared completely at about 10:32 UT on 2011 October 21. The CME associated with the filament eruption and two bright ribbons in the chromosphere both appeared at about 01:30 UT on October 22, i.e., 15 hr after the filament eruption was seen in He II 304 Å filtergrams. We show that this delay is abnormally large even if the slow rise speed and slow acceleration of the filament are taken into account. To understand the cause of this delay, we compute the decay index (n) of the overlying coronal magnetic field. The height distribution of the decay index, n, suggests that the zone of instability ( > n 1) at a lower altitude, 144-480 Mm, is followed by a zone of stability ( < n 1) between 540 and 660 Mm. We interpret the observed delay to be due to the presence of the latter zone, i.e., the zone of stability, which could provide a second quasi-equilibrium state to the filament until it finally erupts.

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Section: Summary and Discussionmentioning

confidence: 65%

Interrupted Eruption of Large Quiescent Filament Associated With a Halo Cme

Gosain

Filippov

Maurya

et al. 2016

ApJ

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“…Both these categories include local, i.e. limited to single active regions or to active region groups (e.g., Canou et al 2009;Gilchrist et al 2012;Jiang et al 2014), and full Sun global models (e.g., Titov et al 2011;Platten et al 2014;Tadesse et al 2014;Yeates et al 2018). In practice, local current-carrying force-free, MHS and MHD models better account for the strong electric currents developing in the vicinity of active regions and are therefore better suited to model their complex magnetic field.…”

Section: Some Challenges To Model Coronal Magnetic Fieldsmentioning

confidence: 99%

Models and data analysis tools for the Solar Orbiter mission

Rouillard

Pinto

Vourlidas

et al. 2020

A&A

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Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in-situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency (ESA)'s Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our proc...

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“…Nonlinear force‐free models were originally developed to understand the buildup of free energy in active regions. More recently, these models have been extended from cartesian to spherical geometry and applied to large field‐of‐view data and even to the global coronal field (Tadesse et al, ).…”

Section: Model Historymentioning

confidence: 99%

Assessing the Quality of Models of the Ambient Solar Wind

et al. 2018

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In this paper we present an assessment of the status of models of the global solar wind in the inner heliosphere. We limit our discussion to the class of models designed to provide solar wind forecasts, excluding those designed for the purpose of testing physical processes in idealized configurations. In addition, we limit our discussion to modeling of the ambient wind in the absence of coronal mass ejections. In this assessment we cover use of the models both in forecast mode and as tools for scientific research. We present a brief history of the development of these models, discussing the range of physical approximations in use. We discuss the limitations of the data inputs available to these models and its impact on their quality. We also discuss current model development trends. Empirical ModelsModeling of the solar coronal magnetic field began in earnest in the early 1960s with the advent of computers and the availability of photospheric magnetograms. The earliest models of the inner coronal field were based

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Global Solar Free Magnetic Energy and Electric Current Density Distribution of Carrington Rotation 2124

Cited by 14 publications

References 51 publications

Interrupted Eruption of Large Quiescent Filament Associated With a Halo Cme

Interrupted Eruption of Large Quiescent Filament Associated With a Halo Cme

Models and data analysis tools for the Solar Orbiter mission

Assessing the Quality of Models of the Ambient Solar Wind

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