Relevant bibliographies by topics / Sun, CME, shocks, STEREO

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Sun, CME, shocks, STEREO'

Author: Grafiati
Published: 4 June 2021
Last updated: 3 February 2022

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Journal articles on the topic "Sun, CME, shocks, STEREO"

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Mishra, Wageesh, Kunjal Dave, Nandita Srivastava, and Luca Teriaca. "Multipoint remote and in situ observations of interplanetary coronal mass ejection structures during 2011 and associated geomagnetic storms." Monthly Notices of the Royal Astronomical Society 506, no. 1 (July 13, 2021): 1186–97. http://dx.doi.org/10.1093/mnras/stab1721.

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ABSTRACT We present multipoint remote and in situ observations of interplanetary coronal mass ejection (ICME) structures during the year 2011. The selected ICMEs arrived at Earth on 2011 March 11 and 2011 August 6, and led to geomagnetic storms. Around the launch of these CMEs from the Sun, the coronagraphs onboard STEREO-Aand-B and SOHO enabled the CMEs to be imaged from three longitudinally separated viewpoints. We attempt to identify the in situ plasma and magnetic parameters of the ICME structures at multiple locations, for example at both STEREO spacecraft and also at the ACE/Wind spacecraft near the first Sun–Earth Lagrangian point (L1), to investigate the global configuration, interplanetary propagation, arrival times and geomagnetic response of the ICMEs. The near-Earth identified ICMEs of March 11 and August 6 formed as a result of the interaction of two successive CMEs observed in the inner corona on March 7 (for the March 11 ICME) and on August 3–4 (for the August 6 ICME). Our study suggests that the structures associated with interacting CMEs, possibly as a result of deflection or large sizes, may reach to even larger longitudinally separated locations in the heliosphere. Our multipoint in situ analysis shows that the characteristics of the same shock, propagating in a pre-conditioned medium, may be different at different longitudinal locations in the heliosphere. Similarly, multiple cuts through the same ejecta/complex ejecta, formed as a result of CME–CME interaction, are found to have inhomogeneous properties. The study highlights the difficulties in connecting the local observations of an ICME from a single in situ spacecraft to its global structures.
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Morosan, D. E., E. Palmerio, B. J. Lynch, and E. K. J. Kilpua. "Extended radio emission associated with a breakout eruption from the back side of the Sun." Astronomy & Astrophysics 633 (January 2020): A141. http://dx.doi.org/10.1051/0004-6361/201936878.

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Context. Coronal mass ejections (CMEs) on the Sun are the largest explosions in the Solar System that can drive powerful plasma shocks. The eruptions, shocks, and other processes associated to CMEs are efficient particle accelerators and the accelerated electrons in particular can produce radio bursts through the plasma emission mechanism. Aims. Coronal mass ejections and associated radio bursts have been well studied in cases where the CME originates close to the solar limb or within the frontside disc. Here, we study the radio emission associated with a CME eruption on the back side of the Sun on 22 July 2012. Methods. Using radio imaging from the Nançay Radioheliograph, spectroscopic data from the Nançay Decametric Array, and extreme-ultraviolet observations from the Solar Dynamics Observatory and Solar Terrestrial Relations Observatory spacecraft, we determine the nature of the observed radio emission as well as the location and propagation of the CME. Results. We show that the observed low-intensity radio emission corresponds to a type II radio burst or a short-duration type IV radio burst associated with a CME eruption due to breakout reconnection on the back side of the Sun, as suggested by the pre-eruptive magnetic field configuration. The radio emission consists of a large, extended structure, initially located ahead of the CME, that corresponds to various electron acceleration locations. Conclusions. The observations presented here are consistent with the breakout model of CME eruptions. The extended radio emission coincides with the location of the current sheet and quasi-separatrix boundary of the CME flux and the overlying helmet streamer and also with that of a large shock expected to form ahead of the CME in this configuration.
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Lavraud, Benoit, and Alexis Rouillard. "Properties and processes that influence CME geo-effectiveness." Proceedings of the International Astronomical Union 8, S300 (June 2013): 273–84. http://dx.doi.org/10.1017/s1743921313011095.

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AbstractThe geo-effectiveness of coronal mass ejections (CME) is determined by a complex chain of processes. This paper highlights this fact by first discussing the importance of CMEs intrinsic properties set at the Sun (e.g., trajectory, eruption process, orientation, etc.). We then review other key processes that may occur during propagation (e.g., shocks, compressions, magnetic flux erosion) and in the specific interaction with Earth's magnetosphere (e.g., magnetic properties, preconditioning mechanisms). These processes sequentially have a significant influence on the final geo-effectiveness of CMEs. Their relative importance is discussed. While the CME's trajectory, magnetic field orientation, velocity and their duration as set at the Sun certainly are key ingredients to geo-effectiveness, other processes and properties, that at first appear secondary, often may be as important.
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Kahler, Stephen W. "Evidence for solar shock production of heliospheric near-relativistic and relativistic electron events." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 86. http://dx.doi.org/10.1017/s1743921307009891.

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AbstractProperties of near-relativistic (E ≳ 30 keV, NR) and relativistic (E ≳ 0.3 MeV) electron events produced near the Sun and observed within 1 AU are reviewed. Observations suggest the CME-driven shocks are the sources of many events, but flares are often sources for NR events.
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Jackson, B. V., P. P. Hick, A. Buffington, M. M. Bisi, and J. M. Clover. "SMEI direct, 3-D-reconstruction sky maps, and volumetric analyses, and their comparison with SOHO and STEREO observations." Annales Geophysicae 27, no. 11 (November 2, 2009): 4097–104. http://dx.doi.org/10.5194/angeo-27-4097-2009.

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Abstract. In this paper we present the results of the analysis of the late January 2007 Coronal Mass Ejection (CME) events recorded by the Solar Mass Ejection Imager (SMEI), the Solar TErrestrial RElations Observatory (STEREO), and the SOlar and Heliospheric Observatory (SOHO) spacecraft. This period occurs when the two STEREO spacecraft views are from close to Earth, and thus the views from both SMEI and the STEREO outer Heliospheric Imagers (HI-2s) coincide. Three-dimensional (3-D) analyses derived from SMEI data show many CMEs that have also been studied by others using short-term image subtractions (image-differencing techniques). During this interval we map several CME structures that are observed in both SMEI and the STEREO-A HI instruments. SMEI brightness analyses provided by short-term image subtractions ("difference images") and, alternatively, subtractions of a mean-brightness fit over a long-time duration, both show the extents of the CMEs travelling outward above the East limb that erupted from the Sun on 24 and 25 January 2007. The SMEI 3-D-reconstructions not only enhance distinct features within the CME events, but also reconcile difference-imaging results with those where a long-term base has been removed. In the January 2007 example the structure as mapped by CME difference images traces the sharp intensity gradients at the front of the CMEs; generally brighter ejected material follows behind the location of the CME front, but shows poorly in these because of its larger angular extent. Using the long-duration background removal enables SMEI's 3-D analysis to determine a mass for this CME sequence North of the ecliptic.
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Hewish, A. "Low Density Drivers of Strong Interplanetary Shocks." International Astronomical Union Colloquium 154 (1996): 5–13. http://dx.doi.org/10.1017/s0252921100029894.

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AbstractThe theory that most, if not all, interplanetary shocks are caused by coronal mass ejections (CMEs) faces serious problems in accounting for the strongest shocks. The difficulties include (i) a remarkable absence of very strong shocks during solar maximum 1980 when CMEs were prolific, (ii) unrealistic initial speeds near the Sun for impulsive models, (iii) the absence of rarefaction zones behind the shocks and (iv) sustained high speed flows following shocks which are not easily explained as consequences of CME eruptions. Observations of the proton temperature near 1 AU indicate that strong shock drivers have properties similar to high speed streams emitted by coronal holes. Eruptions of fast solar wind from coronal holes influenced by solar activity can explain the occurrence of the strongest interplanetary shocks.
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Lugaz, Noé, Charles J. Farrugia, and Nada Al-Haddad. "Complex Evolution of Coronal Mass Ejections in the Inner Heliosphere as Revealed by Numerical Simulations and STEREO Observations: A Review." Proceedings of the International Astronomical Union 8, S300 (June 2013): 255–64. http://dx.doi.org/10.1017/s174392131301106x.

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AbstractThe transit of coronal mass ejections (CMEs) from the Sun to 1 AU lasts on average one to five days. As they propagate, CMEs interact with the solar wind and preceding eruptions, which modify their properties. In the past ten years, the evolution of CMEs in the inner heliosphere has been investigated with the help of numerical simulations, through the analysis of remote-sensing heliospheric observations, especially with the SECCHI suite onboard STEREO, and through the analysis of multi-spacecraft in situ measurements. Most studies have focused on understanding the characteristics of the magnetic flux rope thought to form the core of the CME. Here, we first review recent work related to CME propagation in the heliosphere, which point towards the need to develop more complex models to analyze CME observations. In the second part of this article, we review some recent studies of CME-CME interaction, which also illustrate the complexity of phenomena occurring in the inner heliosphere.
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Corona-Romero, P., and J. A. Gonzalez-Esparza. "Dynamic evolution of interplanetary shock waves driven by CMEs." Proceedings of the International Astronomical Union 7, S286 (October 2011): 159–63. http://dx.doi.org/10.1017/s1743921312004784.

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AbstractWe present a study about the propagation of interplanetary shock waves driven by super magnetosonic coronal mass ejections (CMEs). The discussion focuses on a model which describes the dynamic relationship between the CME and its driven shock and the way to approximate the trajectory of shocks based on those relationships, from near the Sun to 1 AU. We apply the model to the analysis of a case study in which our calculations show quantitative and qualitative agreements with different kinds of data. We discuss the importance of solar wind and CME initial conditions on the shock wave evolution.
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Lago, A. Dal, L. E. Antunes Vieira, E. Echer, L. A. Balmaceda, M. Rockenbach, and W. D. Gonzalez. "Extreme solar-terrestrial events." Proceedings of the International Astronomical Union 12, S328 (October 2016): 233–36. http://dx.doi.org/10.1017/s1743921317004185.

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AbstractExtreme solar-terrestrial events are those in which very energetic solar ejections hit the earth?s magnetosphere, causing intense energization of the earth?s ring current. Statistically, their occurrence is approximately once per Gleissberg solar cycle (70-100yrs). The solar transient occurred on July, 23rd (2012) was potentially one of such extreme events. The associated coronal mass ejection (CME), however, was not ejected towards the earth. Instead, it hit the STEREO A spacecraft, located 120 degrees away from the Sun-Earth line. Estimates of the geoeffectiveness of such a CME point to a scenario of extreme Space Weather conditions. In terms of the ring current energization, as measured by the Disturbance Storm-Time index (Dst), had this CME hit the Earth, it would have caused the strongest geomagnetic storm in space era.
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McKenna-Lawlor, S. M. P., M. Dryer, Z. Smith, K. Kecskemety, C. D. Fry, W. Sun, C. S. Deehr, D. Berdichevsky, K. Kudela, and G. Zastenker. "Arrival times of Flare/Halo CME associated shocks at the Earth: comparison of the predictions of three numerical models with these observations." Annales Geophysicae 20, no. 7 (July 31, 2002): 917–35. http://dx.doi.org/10.5194/angeo-20-917-2002.

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Abstract. The arrival times at L1 of eleven travelling shocks associated both with X-ray flaring and with halo CMEs recorded aboard SOHO/LASCO have been considered. Close to the Sun the velocities of these events were estimated using either Type II radio records or CME speeds. Close to the Earth the shocks were detected in the data of various solar wind plasma, interplanetary magnetic field (IMF) and energetic particle experiments aboard SOHO, ACE, WIND, INTERBALL-1 and IMP-8. The real-time shock arrival predictions of three numerical models, namely the Shock Time of Arrival Model (STOA), the Interplanetary Shock Propagation Model (ISPM) and the Hakamada-Akasofu-Fry Solar Wind Model (HAFv.2) were tested against these observations. This is the first time that energetic protons (tens of keV to a few MeV) have been used to complement plasma and IMF data in validating shock propagation models. The models were all generally successful in predicting shock arrivals. STOA provided the smallest values of the "predicted minus measured" arrival times and displayed a typical predictive precision better than about 8 h. The ratio of the calculated standard deviation of the transit times to Earth to the standard deviation of the measurements was estimated for each model (treating interacting events as composite shocks) and these ratios turned out to be 0.60, 1.15 and 1.02 for STOA, ISPM and HAFv.2, respectively. If an event in the sample for which the shock velocity was not well known is omitted from consideration, these ratios become 0.36, 0.76 and 0.81, respectively. Larger statistical samples should now be tested. The ratio of the in situ shock velocity and the "Sun to L1" transit velocity (Vsh /Vtr) was in the range of 0.7–0.9 for individual, non-interacting, shock events. HAFv.2 uniquely provided information on those changes in the COBpoint (the moving Connection point on the shock along the IMF to the OBserver) which directly influenced energetic particle rise times. This model also illustrated the non-uniform upstream conditions through which the various shocks propagated; furthermore it simulated shock deformation on a scale of fractions of an AU. On the spatial scale (300 RE ), where near-Earth spacecraft are located, the passing shocks, in conformity with the models, were found to be locally planar. The shocks also showed tilting relative to the Sun-Earth line, probably reflecting the inherent directionality associated with their solar origin. Key words. Interplanetary physics (energetic particles; interplanetary shocks; solar wind plasma)
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Dissertations / Theses on the topic "Sun, CME, shocks, STEREO"

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Volpes, Laura. "On the interplanetary properties and evolution of CME-driven shocks." Doctoral thesis, 2016. http://hdl.handle.net/11858/00-1735-0000-0023-3E40-0.

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Books on the topic "Sun, CME, shocks, STEREO"

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Gallio, Nicolò. Framing Death. Bononia University Press, 2020. http://dx.doi.org/10.30682/alph02.

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"Perché siamo affascinati dalla rappresentazione della morte? Che cosa ci attrae dei contenuti audiovisivi ritenuti inaccettabili e morbosi? Partendo dalle origini del cinematografo, il volume analizza le strategie promozionali e la ricezione critica di film che in passato sono stati censurati e al tempo stesso avidamente collezionati, oggetti proibiti che sono ormai considerati prodotti di culto presso specifiche nicchie di pubblico. Uno studio che si intreccia con l’impatto che la tecnologia ha avuto sulla diffusione delle immagini di morte: dal filmato Zapruder alla nascita degli shock sites, dal fenomeno del War Porn ai killer che utilizzano ingegnosamente i social media. Dai cosiddetti snuff movies e shockumentaries a certe manifestazioni dell’arte contemporanea, dalla “necrocultura” al terrorismo, quello proposto è un percorso all’interno del caos della morte dall’era analogica a quella digitale. Nicolò Gallio è Dottore di ricerca in Studi teatrali e cinematografici e si interessa in particolare della relazione tra prodotti audiovisivi e media digitali. Ha tenuto corsi e seminari presso l’Università di Bologna, University of Brighton, Middlesex University e Birmingham City University. Ha scritto articoli e saggi pubblicati su libri e riviste italiane e internazionali, ed è co-autore de Lo spettacolo del cibo. I cooking show nella televisione italiana. È consulente di marketing e comunicazione per agenzie creative, festival e programmi di sviluppo di film indipendenti."
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Book chapters on the topic "Sun, CME, shocks, STEREO"

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Srivastava, N. "CME Observations from STEREO." In Magnetic Coupling between the Interior and Atmosphere of the Sun, 308–17. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-02859-5_25.

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Conference papers on the topic "Sun, CME, shocks, STEREO"

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Desai, Mihir, Maher Dayeh, Robert Ebert, Charles Smith, Glenn Mason, and G. Li. "Ion acceleration at CME-driven shocks near the Earth and the Sun." In SPACE WEATHER: THE SPACE RADIATION ENVIRONMENT: 11th Annual International Astrophysics Conference. AIP, 2012. http://dx.doi.org/10.1063/1.4768748.

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Journal articles
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