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Stamkos S, Patsourakos S, Vourlidas A, Daglis IA. How Magnetic Erosion Affects the Drag-Based Kinematics of Fast Coronal Mass Ejections. Sol Phys 2023; 298:88. [PMID: 37457788 PMCID: PMC10344841 DOI: 10.1007/s11207-023-02178-7] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/10/2023] [Accepted: 06/10/2023] [Indexed: 07/18/2023]
Abstract
In order to advance our understanding of the dynamic interactions between coronal mass ejections (CMEs) and the magnetized solar wind, we investigate the impact of magnetic erosion on the well-known aerodynamic drag force acting on CMEs traveling faster than the ambient solar wind. In particular, we start by generating empirical relationships for the basic physical parameters of CMEs that conserve their mass and magnetic flux. Furthermore, we examine the impact of the virtual mass on the equation of motion by studying a variable-mass system. We next implement magnetic reconnection into CME propagation, which erodes part of the CME magnetic flux and outer-shell mass, on the drag acting on CMEs, and we determine its impact on their time and speed of arrival at 1 AU. Depending on the strength of the magnetic erosion, the leading edge of the magnetic structure can reach near-Earth space up to ≈ three hours later, compared to the non-eroded case. Therefore, magnetic erosion may have a significant impact on the propagation of fast CMEs and on predictions of their arrivals at 1 AU. Finally, the modeling indicates that eroded CMEs may experience a significant mass decrease. Since such a decrease is not observed in the corona, the initiation distance of erosion may lie beyond the field-of-view of coronagraphs (i.e. 30 R ⊙ ).
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Affiliation(s)
- Sotiris Stamkos
- Department of Physics, University of Ioannina, Ioannina, Greece
| | | | - Angelos Vourlidas
- Applied Physics Laboratory, Johns Hopkins University, Laurel, MD USA
| | - Ioannis A. Daglis
- Department of Physics, National and Kapodistrian University of Athens, Athens, Greece
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Zhang J, Temmer M, Gopalswamy N, Malandraki O, Nitta NV, Patsourakos S, Shen F, Vršnak B, Wang Y, Webb D, Desai MI, Dissauer K, Dresing N, Dumbović M, Feng X, Heinemann SG, Laurenza M, Lugaz N, Zhuang B. Earth-affecting solar transients: a review of progresses in solar cycle 24. Prog Earth Planet Sci 2021; 8:56. [PMID: 34722120 PMCID: PMC8550066 DOI: 10.1186/s40645-021-00426-7] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/19/2020] [Accepted: 04/26/2021] [Indexed: 06/13/2023]
Abstract
This review article summarizes the advancement in the studies of Earth-affecting solar transients in the last decade that encompasses most of solar cycle 24. It is a part of the effort of the International Study of Earth-affecting Solar Transients (ISEST) project, sponsored by the SCOSTEP/VarSITI program (2014-2018). The Sun-Earth is an integrated physical system in which the space environment of the Earth sustains continuous influence from mass, magnetic field, and radiation energy output of the Sun in varying timescales from minutes to millennium. This article addresses short timescale events, from minutes to days that directly cause transient disturbances in the Earth's space environment and generate intense adverse effects on advanced technological systems of human society. Such transient events largely fall into the following four types: (1) solar flares, (2) coronal mass ejections (CMEs) including their interplanetary counterparts ICMEs, (3) solar energetic particle (SEP) events, and (4) stream interaction regions (SIRs) including corotating interaction regions (CIRs). In the last decade, the unprecedented multi-viewpoint observations of the Sun from space, enabled by STEREO Ahead/Behind spacecraft in combination with a suite of observatories along the Sun-Earth lines, have provided much more accurate and global measurements of the size, speed, propagation direction, and morphology of CMEs in both 3D and over a large volume in the heliosphere. Many CMEs, fast ones, in particular, can be clearly characterized as a two-front (shock front plus ejecta front) and three-part (bright ejecta front, dark cavity, and bright core) structure. Drag-based kinematic models of CMEs are developed to interpret CME propagation in the heliosphere and are applied to predict their arrival times at 1 AU in an efficient manner. Several advanced MHD models have been developed to simulate realistic CME events from the initiation on the Sun until their arrival at 1 AU. Much progress has been made on detailed kinematic and dynamic behaviors of CMEs, including non-radial motion, rotation and deformation of CMEs, CME-CME interaction, and stealth CMEs and problematic ICMEs. The knowledge about SEPs has also been significantly improved. An outlook of how to address critical issues related to Earth-affecting solar transients concludes this article.
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Affiliation(s)
- Jie Zhang
- Department of Physics and Astronomy, George Mason University, 4400 University Dr., MSN 3F3, Fairfax, VA 22030 USA
| | | | | | - Olga Malandraki
- National Observatory of Athens, Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, Penteli, Athens Greece
| | - Nariaki V. Nitta
- Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA USA
| | | | - Fang Shen
- SIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, 100190 China
| | - Bojan Vršnak
- Hvar Observatory, Faculty of Geodesy, University of Zagreb, Kaciceva 26, HR-10000 Zagreb, Croatia
| | - Yuming Wang
- CAS Key Laboratory of Geospace Environment, Department of Geophysics and Planetary Sciences, University of Science and Technology of China, Hefei, Anhui 230026 PR China
| | - David Webb
- ISR, Boston College, 140 Commonwealth Ave., Chestnut Hill, MA 02467 USA
| | - Mihir I. Desai
- Southwest Research Institute, 6220 Culebra Road, San Antonia, TX 78023 USA
- Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, TX 78249 USA
| | - Karin Dissauer
- Institute of Physics, University of Graz, Graz, Austria
- NorthWest Research Association, Boulder, CO USA
| | - Nina Dresing
- Institut fuer Experimentelle und Angewandte Physik, University of Kiel, Kiel, Germany
- Department of Physics and Astronomy, University of Turku, Turku, Finland
| | - Mateja Dumbović
- Hvar Observatory, Faculty of Geodesy, University of Zagreb, Kaciceva 26, HR-10000 Zagreb, Croatia
| | - Xueshang Feng
- SIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, 100190 China
| | - Stephan G. Heinemann
- Institute of Physics, University of Graz, Graz, Austria
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Monica Laurenza
- INAF-Istituto di Astrofisica e Planetologia Spaziali, Via del Fosso del Cavaliere, 100, I-00133 Rome, Italy
| | - Noé Lugaz
- Space Science Center and Department of Physics, University of New Hampshire, Durham, NH USA
| | - Bin Zhuang
- Space Science Center and Department of Physics, University of New Hampshire, Durham, NH USA
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Vourlidas A, Patsourakos S, Savani NP. Predicting the geoeffective properties of coronal mass ejections: current status, open issues and path forward. Philos Trans A Math Phys Eng Sci 2019; 377:20180096. [PMID: 31079585 PMCID: PMC6527953 DOI: 10.1098/rsta.2018.0096] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 03/15/2019] [Indexed: 06/09/2023]
Abstract
Much progress has been made in the study of coronal mass ejections (CMEs), the main drivers of terrestrial space weather thanks to the deployment of several missions in the last decade. The flow of energy required to power solar eruptions is beginning to be understood. The initiation of CMEs is routinely observed with cadences of tens of seconds with arc-second resolution. Their inner heliospheric evolution can now be imaged and followed routinely. Yet relatively little progress has been made in predicting the geoeffectiveness of a particular CME. Why is that? What are the issues holding back progress in medium-term forecasting of space weather? To answer these questions, we review, here, the measurements, status and open issues on the main CME geoeffective parameters; namely, their entrained magnetic field strength and configuration, their Earth arrival time and speed, and their mass (momentum). We offer strategies for improving the accuracy of the measurements and their forecasting in the near and mid-term future. To spark further discussion, we incorporate our suggestions into a top-level draft action plan that includes suggestions for sensor deployment, technology development and modelling/theory improvements. This article is part of the theme issue 'Solar eruptions and their space weather impact'.
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Affiliation(s)
- A. Vourlidas
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- IAASARS, Observatory of Athens, Penteli, Greece
| | - S. Patsourakos
- Department of Physics, Section of Astro-geophysics, University of Ioannina, Ioannina, Greece
| | - N. P. Savani
- Goddard Planetary Heliophysics Institute, University of Maryland, Baltimore, MD, USA
- NASA, Goddard Space Flight Center, Greenbelt, MD, USA
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Raouafi NE, Patsourakos S, Pariat E, Young PR, Sterling A, Savcheva A, Shimojo M, Moreno-Insertis F, DeVore CR, Archontis V, Török T, Mason H, Curdt W, Meyer K, Dalmasse K, Matsui Y. Solar Coronal Jets: Observations, Theory, and Modeling. Space Sci Rev 2016; 201:1-53. [PMID: 32908324 PMCID: PMC7477949 DOI: 10.1007/s11214-016-0260-5] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
Chromospheric and coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of "nominal" solar flares and Coronal Mass Ejections (CMEs), jets share many common properties with these major phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients close or at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broad range of solar-heliospheric problems.
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Affiliation(s)
- N. E. Raouafi
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - S. Patsourakos
- Department of Physics, University of Ioannina, Ioannina, Greece
| | - E. Pariat
- LESIA, Observatoire de Paris, Meudon, France
| | - P. R. Young
- College of Science, George Mason University, Fairfax, VA, USA. NASA/Goddard Space Flight Center, Code 671, Greenbelt, MD 20771, USA
| | - A. Sterling
- NASA/Marshall Space Flight Center, Huntsville, Alabama, USA
| | - A. Savcheva
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
| | - M. Shimojo
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | | | - C. R. DeVore
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - V. Archontis
- School of Mathematics and Statistics, University of St. Andrews, St. Andrews, UK
| | - T. Török
- Predictive Science Inc., 9990 Mesa Rim Rd., Ste. 170, San Diego, CA 92121, USA
| | - H. Mason
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Cambridge, UK
| | - W. Curdt
- Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany
| | - K. Meyer
- Division of Computing and Mathematics, Abertay University, Dundee, UK
| | - K. Dalmasse
- LESIA, Observatoire de Paris, Meudon, France
- CISL/HAO, NCAR, P.O. Box 3000, Boulder, CO 80307-3000, USA
| | - Y. Matsui
- Department of Earth and Planetary Science, University of Tokyo, Tokyo, Japan
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