1
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Srivastava AK, Singh A, Singh B, Murawski K, Zaqarashvili TV, Yuan D, Scullion E, Mishra SK, Dwivedi BN. Alfvén pulse driven spicule-like jets in the presence of thermal conduction and ion-neutral collision in two-fluid regime. Philos Trans A Math Phys Eng Sci 2024; 382:20230220. [PMID: 38679049 DOI: 10.1098/rsta.2023.0220] [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] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/15/2023] [Accepted: 03/19/2024] [Indexed: 05/01/2024]
Abstract
We present the formation of quasi-periodic cool spicule-like jets in the solar atmosphere using 2.5-D numerical simulation in two-fluid regime (ions+neutrals) under the presence of thermal conduction and ion-neutral collision. The nonlinear, impulsive Alfvénic perturbations at the top of the photosphere trigger field aligned magnetoacoustic perturbations due to ponderomotive force. The transport of energy from Alfvén pulse to such vertical velocity perturbations due to ponderomotive force is considered as an initial trigger mechanism. Thereafter, these velocity perturbations steepen into the shocks followed by quasi-periodic rise and fall of the cool jets transporting mass in the overlying corona. This article is part of the theme issue 'Partially ionized plasma of the solar atmosphere: recent advances and future pathways'.
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Affiliation(s)
- A K Srivastava
- Department of Physics, Indian Institute of Technology (BHU), Varanasi 221005, India
| | - Anshika Singh
- Department of Physics, Indian Institute of Technology (BHU), Varanasi 221005, India
| | - Balveer Singh
- Aryabhatta Research Institute of Observational Sciences (ARIES), Manora peak, Nainital 263001, India
| | - K Murawski
- Institute of Physics, University of Maria Curie-Sklodowska,Pl. M. Curie-Sklodowskiej, 20-0531 Lublin, Poland
| | - T V Zaqarashvili
- Institut of Physics, IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
- Department of Astronomy and Astrophysics at Space Research Center, School of Natural Sciences and Medicine, Ilia State University, Kakutsa Cholokashvili Ave. 3/5, Tbilisi 0162, Georgia
- Evgeni Kharadze Georgian National Astrophysical Observatory, Abastumani, Adigeni 0301, Georgia
| | - D Yuan
- Shenzhen Key Laboratory of Numerical Prediction for Space Storm, Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, Guangdong 518055, People's Republic of China
| | - E Scullion
- Department of Mathematics, Physics and Electrical Engineering, Northumbria University, NE1 8ST Newcastle upon Tyne, UK
| | - Sudheer K Mishra
- Astronomical Observatory, Kyoto University, Sakyo, Kyoto 606-8502, Japan
| | - B N Dwivedi
- Rajiv Gandhi Institute of Petroleum Technology, Jais Amethi 229304, India
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2
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Chitta LP, Zhukov AN, Berghmans D, Peter H, Parenti S, Mandal S, Aznar Cuadrado R, Schühle U, Teriaca L, Auchère F, Barczynski K, Buchlin É, Harra L, Kraaikamp E, Long DM, Rodriguez L, Schwanitz C, Smith PJ, Verbeeck C, Seaton DB. Picoflare jets power the solar wind emerging from a coronal hole on the Sun. Science 2023; 381:867-872. [PMID: 37616348 DOI: 10.1126/science.ade5801] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/25/2022] [Accepted: 07/14/2023] [Indexed: 08/26/2023]
Abstract
Coronal holes are areas on the Sun with open magnetic field lines. They are a source region of the solar wind, but how the wind emerges from coronal holes is not known. We observed a coronal hole using the Extreme Ultraviolet Imager on the Solar Orbiter spacecraft. We identified jets on scales of a few hundred kilometers, which last 20 to 100 seconds and reach speeds of ~100 kilometers per second. The jets are powered by magnetic reconnection and have kinetic energy in the picoflare range. They are intermittent but widespread within the observed coronal hole. We suggest that such picoflare jets could produce enough high-temperature plasma to sustain the solar wind and that the wind emerges from coronal holes as a highly intermittent outflow at small scales.
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Affiliation(s)
- L P Chitta
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - A N Zhukov
- Solar-Terrestrial Centre of Excellence, Solar Influences Data Analysis Centre, Royal Observatory of Belgium, 1180 Brussels, Belgium
- Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow 119991, Russia
| | - D Berghmans
- Solar-Terrestrial Centre of Excellence, Solar Influences Data Analysis Centre, Royal Observatory of Belgium, 1180 Brussels, Belgium
| | - H Peter
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - S Parenti
- Institut d'Astrophysique Spatiale, Centre National de la Recherche Scientifique, Université Paris-Saclay, 91405 Orsay, France
| | - S Mandal
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - R Aznar Cuadrado
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - U Schühle
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - L Teriaca
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - F Auchère
- Institut d'Astrophysique Spatiale, Centre National de la Recherche Scientifique, Université Paris-Saclay, 91405 Orsay, France
| | - K Barczynski
- Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, 7260 Davos Dorf, Switzerland
- Eidgenössische Technische Hochschule Zürich, 8093 Zürich, Switzerland
| | - É Buchlin
- Institut d'Astrophysique Spatiale, Centre National de la Recherche Scientifique, Université Paris-Saclay, 91405 Orsay, France
| | - L Harra
- Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, 7260 Davos Dorf, Switzerland
- Eidgenössische Technische Hochschule Zürich, 8093 Zürich, Switzerland
| | - E Kraaikamp
- Solar-Terrestrial Centre of Excellence, Solar Influences Data Analysis Centre, Royal Observatory of Belgium, 1180 Brussels, Belgium
| | - D M Long
- Mullard Space Science Laboratory, University College London, Dorking, Surrey RH5 6NT, UK
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, Northern Ireland, UK
| | - L Rodriguez
- Solar-Terrestrial Centre of Excellence, Solar Influences Data Analysis Centre, Royal Observatory of Belgium, 1180 Brussels, Belgium
| | - C Schwanitz
- Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, 7260 Davos Dorf, Switzerland
- Eidgenössische Technische Hochschule Zürich, 8093 Zürich, Switzerland
| | - P J Smith
- Mullard Space Science Laboratory, University College London, Dorking, Surrey RH5 6NT, UK
| | - C Verbeeck
- Solar-Terrestrial Centre of Excellence, Solar Influences Data Analysis Centre, Royal Observatory of Belgium, 1180 Brussels, Belgium
| | - D B Seaton
- Southwest Research Institute, Boulder, CO 80302, USA
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3
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MacBride CD, Jess DB, Grant SDT, Khomenko E, Keys PH, Stangalini M. Accurately constraining velocity information from spectral imaging observations using machine learning techniques. Philos Trans A Math Phys Eng Sci 2021; 379:20200171. [PMID: 33342374 PMCID: PMC7780131 DOI: 10.1098/rsta.2020.0171] [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] [Subscribe] [Scholar Register] [Accepted: 07/13/2020] [Indexed: 06/12/2023]
Abstract
Determining accurate plasma Doppler (line-of-sight) velocities from spectroscopic measurements is a challenging endeavour, especially when weak chromospheric absorption lines are often rapidly evolving and, hence, contain multiple spectral components in their constituent line profiles. Here, we present a novel method that employs machine learning techniques to identify the underlying components present within observed spectral lines, before subsequently constraining the constituent profiles through single or multiple Voigt fits. Our method allows active and quiescent components present in spectra to be identified and isolated for subsequent study. Lastly, we employ a Ca ɪɪ 8542 Å spectral imaging dataset as a proof-of-concept study to benchmark the suitability of our code for extracting two-component atmospheric profiles that are commonly present in sunspot chromospheres. Minimization tests are employed to validate the reliability of the results, achieving median reduced χ2-values equal to 1.03 between the observed and synthesized umbral line profiles. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.
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Affiliation(s)
- Conor D. MacBride
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK
| | - David B. Jess
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK
- Department of Physics and Astronomy, California State University Northridge, Northridge, CA 91330, USA
| | - Samuel D. T. Grant
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK
| | - Elena Khomenko
- Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
- Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
| | - Peter H. Keys
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK
| | - Marco Stangalini
- Italian Space Agency (ASI), Via del Politecnico snc, 00133 Roma, Italy
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4
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Abstract
The solar atmosphere is full of complicated transients manifesting the reconfiguration of the solar magnetic field and plasma. Solar jets represent collimated, beam-like plasma ejections; they are ubiquitous in the solar atmosphere and important for our understanding of solar activities at different scales, the magnetic reconnection process, particle acceleration, coronal heating, solar wind acceleration, as well as other related phenomena. Recent high-spatio-temporal-resolution, wide-temperature coverage and spectroscopic and stereoscopic observations taken by ground-based and space-borne solar telescopes have revealed many valuable new clues to restrict the development of theoretical models. This review aims at providing the reader with the main observational characteristics of solar jets, physical interpretations and models, as well as unsolved outstanding questions in future studies.
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Affiliation(s)
- Yuandeng Shen
- Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People’s Republic of China
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5
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Ni L, Ji H, Murphy NA, Jara-Almonte J. Magnetic reconnection in partially ionized plasmas. Proc Math Phys Eng Sci 2020; 476:20190867. [PMID: 32398944 DOI: 10.1098/rspa.2019.0867] [Citation(s) in RCA: 14] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/13/2019] [Accepted: 03/11/2020] [Indexed: 11/12/2022] Open
Abstract
Magnetic reconnection has been intensively studied in fully ionized plasmas. However, plasmas are often partially ionized in astrophysical environments. The interactions between the neutral particles and ionized plasmas might strongly affect the reconnection mechanisms. We review magnetic reconnection in partially ionized plasmas in different environments from theoretical, numerical, observational and experimental points of view. We focus on mechanisms which make magnetic reconnection fast enough to compare with observations, especially on the reconnection events in the low solar atmosphere. The heating mechanisms and the related observational evidence of the reconnection process in the partially ionized low solar atmosphere are also discussed. We describe magnetic reconnection in weakly ionized astrophysical environments, including the interstellar medium and protostellar discs. We present recent achievements about fast reconnection in laboratory experiments for partially ionized plasmas.
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Affiliation(s)
- Lei Ni
- Yunnan Observatories, Chinese Academy of Sciences, PO Box 110, Kunming, Yunnan 650216, People's Republic of China.,Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China
| | - Hantao Ji
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA.,Princeton Plasma Physics Laboratory, Princeton, NJ 08543, USA
| | - Nicholas A Murphy
- Center for Astrophysics
- Harvard and Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA
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6
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Samanta T, Tian H, Yurchyshyn V, Peter H, Cao W, Sterling A, Erdélyi R, Ahn K, Feng S, Utz D, Banerjee D, Chen Y. Generation of solar spicules and subsequent atmospheric heating. Science 2020; 366:890-894. [PMID: 31727839 DOI: 10.1126/science.aaw2796] [Citation(s) in RCA: 68] [Impact Index Per Article: 17.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/04/2018] [Accepted: 10/24/2019] [Indexed: 11/02/2022]
Abstract
Spicules are rapidly evolving fine-scale jets of magnetized plasma in the solar chromosphere. It remains unclear how these prevalent jets originate from the solar surface and what role they play in heating the solar atmosphere. Using the Goode Solar Telescope at the Big Bear Solar Observatory, we observed spicules emerging within minutes of the appearance of opposite-polarity magnetic flux around dominant-polarity magnetic field concentrations. Data from the Solar Dynamics Observatory showed subsequent heating of the adjacent corona. The dynamic interaction of magnetic fields (likely due to magnetic reconnection) in the partially ionized lower solar atmosphere appears to generate these spicules and heat the upper solar atmosphere.
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Affiliation(s)
- Tanmoy Samanta
- School of Earth and Space Sciences, Peking University, Beijing 100871, People's Republic of China
| | - Hui Tian
- School of Earth and Space Sciences, Peking University, Beijing 100871, People's Republic of China.
| | - Vasyl Yurchyshyn
- Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314-9672, USA
| | - Hardi Peter
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, D-37077 Göttingen, Germany
| | - Wenda Cao
- Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314-9672, USA
| | | | - Robertus Erdélyi
- Solar Physics and Space Plasma Research Centre, School of Mathematics and Statistics, University of Sheffield, Hounsfield Road, Sheffield S3 7RH, UK.,Department of Astronomy, Eötvös Loránd University, Budapest, H-1117 Budapest, Hungary
| | - Kwangsu Ahn
- Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314-9672, USA
| | - Song Feng
- Faculty of Information Engineering and Automation, Kunming University of Science and Technology, Kunming 650500, People's Republic of China
| | - Dominik Utz
- Institute for Geophysics, Astrophysics and Meteorology-Institute of Physics, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
| | - Dipankar Banerjee
- Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
| | - Yajie Chen
- School of Earth and Space Sciences, Peking University, Beijing 100871, People's Republic of China
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7
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Abstract
Kelvin-Helmholtz instability (KHI) is a basic physical process in fluids and magnetized plasmas, with applications successfully modelling e.g. exponentially growing instabilities observed at magnetospheric and heliospheric boundaries, in the solar or Earth's atmosphere and within astrophysical jets. Here, we report the discovery of the KHI in solar blowout jets and analyse the detailed evolution by employing high-resolution data from the Interface Region Imaging Spectrograph (IRIS) satellite launched in 2013. The particular jet we focus on is rooted in the surrounding penumbra of the main negative polarity sunspot of Active Region 12365, where the main body of the jet is a super-penumbral structure. At its maximum, the jet has a length of 90 Mm, a width of 19.7 Mm, and its density is about 40 times higher than its surroundings. During the evolution of the jet, a cavity appears near the base of the jet, and bi-directional flows originated from the top and bottom of the cavity start to develop, indicating that magnetic reconnection takes place around the cavity. Two upward flows pass along the left boundary of the jet successively. Next, KHI develops due to a strong velocity shear (∼204 km s-1) between these two flows, and subsequently the smooth left boundary exhibits a sawtooth pattern, evidencing the onset of the instability.
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Affiliation(s)
- Xiaohong Li
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China. .,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China.
| | - Jun Zhang
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China. .,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China.
| | - Shuhong Yang
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China
| | - Yijun Hou
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China
| | - Robert Erdélyi
- Solar Physics and Space Plasma Research Centre, School of Mathematics and Statistics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK.,Department of Astronomy, Eötvös Lorand University, Pázmány Péter sétány 1/A, Budapest, H-1117, Hungary
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8
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Srivastava AK, Shetye J, Murawski K, Doyle JG, Stangalini M, Scullion E, Ray T, Wójcik DP, Dwivedi BN. High-frequency torsional Alfvén waves as an energy source for coronal heating. Sci Rep 2017; 7:43147. [PMID: 28256538 PMCID: PMC5335648 DOI: 10.1038/srep43147] [Citation(s) in RCA: 82] [Impact Index Per Article: 11.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/06/2016] [Accepted: 01/17/2017] [Indexed: 11/30/2022] Open
Abstract
The existence of the Sun’s hot atmosphere and the solar wind acceleration continues to be an outstanding problem in solar-astrophysics. Although magnetohydrodynamic (MHD) modes and dissipation of magnetic energy contribute to heating and the mass cycle of the solar atmosphere, yet direct evidence of such processes often generates debate. Ground-based 1-m Swedish Solar Telescope (SST)/CRISP, Hα 6562.8 Å observations reveal, for the first time, the ubiquitous presence of high frequency (~12–42 mHz) torsional motions in thin spicular-type structures in the chromosphere. We detect numerous oscillating flux tubes on 10 June 2014 between 07:17 UT to 08:08 UT in a quiet-Sun field-of-view of 60” × 60” (1” = 725 km). Stringent numerical model shows that these observations resemble torsional Alfvén waves associated with high frequency drivers which contain a huge amount of energy (~105 W m−2) in the chromosphere. Even after partial reflection from the transition region, a significant amount of energy (~103 W m−2) is transferred onto the overlying corona. We find that oscillating tubes serve as substantial sources of Alfvén wave generation that provide sufficient Poynting flux not only to heat the corona but also to originate the supersonic solar wind.
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Affiliation(s)
| | - Juie Shetye
- Armagh Observatory, College Hill, Armagh, BT61 9DG, N. Ireland
| | | | | | - Marco Stangalini
- INAF-OAR National Institute for Astrophysics, 00040, Monte Porzio Catone, RM, Italy
| | - Eamon Scullion
- Department of Mathematics &Information Sciences, Northumbria University, Newcastle Upon Tyne, NE1 8ST, UK
| | - Tom Ray
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | | | - Bhola N Dwivedi
- Department of Physics, Indian Institute of Technology (BHU), Varanasi-221005, India
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9
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Liu J, Wang Y, Erdélyi R, Liu R, Mcintosh SW, Gou T, Chen J, Liu K, Liu L, Pan Z. ON THE MAGNETIC AND ENERGY CHARACTERISTICS OF RECURRENT HOMOLOGOUS JETS FROM AN EMERGING FLUX. ACTA ACUST UNITED AC 2016; 833:150. [DOI: 10.3847/1538-4357/833/2/150] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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10
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Pariat E, Dalmasse K, DeVore CR, Antiochos SK, Karpen JT. A model for straight and helical solar jets: II. Parametric study of the plasma beta. Astron Astrophys Suppl Ser 2016; 596:A36. [PMID: 29371750 PMCID: PMC5779865 DOI: 10.1051/0004-6361/201629109] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
Context Jets are dynamic, impulsive, well-collimated plasma events that develop at many different scales and in different layers of the solar atmosphere. Aims Jets are believed to be induced by magnetic reconnection, a process central to many astrophysical phenomena. Within the solar atmosphere, jet-like events develop in many different environments, e.g., in the vicinity of active regions as well as in coronal holes, and at various scales, from small photospheric spicules to large coronal jets. In all these events, signatures of helical structure and/or twisting/rotating motions are regularly observed. The present study aims to establish that a single model can generally reproduce the observed properties of these jet-like events. Methods In this study, using our state-of-the-art numerical solver ARMS, we present a parametric study of a numerical tridimensional magnetohydrodynamic (MHD) model of solar jet-like events. Within the MHD paradigm, we study the impact of varying the atmospheric plasma β on the generation and properties of solar-like jets. Results The parametric study validates our model of jets for plasma β ranging from 10-3 to 1, typical of the different layers and magnetic environments of the solar atmosphere. Our model of jets can robustly explain the generation of helical solar jet-like events at various β ≤ 1. This study introduces the new original result that the plasma β modifies the morphology of the helical jet, explaining the different observed shapes of jets at different scales and in different layers of the solar atmosphere. Conclusions Our results allow us to understand the energisation, triggering, and driving processes of jet-like events. Our model allows us to make predictions of the impulsiveness and energetics of jets as determined by the surrounding environment, as well as the morphological properties of the resulting jets.
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Affiliation(s)
- E Pariat
- LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
| | - K Dalmasse
- CISL/HAO, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307-3000, USA
| | - C R DeVore
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - S K Antiochos
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - J T Karpen
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
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11
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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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13
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14
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Tian H, Young PR, Reeves KK, Chen B, Liu W, McKillop S. TEMPORAL EVOLUTION OF CHROMOSPHERIC EVAPORATION: CASE STUDIES OF THE M1.1 FLARE ON 2014 SEPTEMBER 6 AND X1.6 FLARE ON 2014 SEPTEMBER 10. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/811/2/139] [Citation(s) in RCA: 80] [Impact Index Per Article: 8.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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15
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Abstract
The solar corona, the tenuous outer atmosphere of the Sun, is orders of magnitude hotter than the solar surface. This 'coronal heating problem' requires the identification of a heat source to balance losses due to thermal conduction, radiation and (in some locations) convection. The review papers in this Theo Murphy meeting issue present an overview of recent observational findings, large- and small-scale numerical modelling of physical processes occurring in the solar atmosphere and other aspects which may affect our understanding of the proposed heating mechanisms. At the same time, they also set out the directions and challenges which must be tackled by future research. In this brief introduction, we summarize some of the issues and themes which reoccur throughout this issue.
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Affiliation(s)
- Ineke De Moortel
- School of Mathematics and Statistics, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK
| | - Philippa Browning
- Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester M13 9PL, UK
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Cranmer SR, Asgari-Targhi M, Miralles MP, Raymond JC, Strachan L, Tian H, Woolsey LN. The role of turbulence in coronal heating and solar wind expansion. Philos Trans A Math Phys Eng Sci 2015; 373:20140148. [PMID: 25848083 PMCID: PMC4394680 DOI: 10.1098/rsta.2014.0148] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 12/05/2014] [Indexed: 06/01/2023]
Abstract
Plasma in the Sun's hot corona expands into the heliosphere as a supersonic and highly magnetized solar wind. This paper provides an overview of our current understanding of how the corona is heated and how the solar wind is accelerated. Recent models of magnetohydrodynamic turbulence have progressed to the point of successfully predicting many observed properties of this complex, multi-scale system. However, it is not clear whether the heating in open-field regions comes mainly from the dissipation of turbulent fluctuations that are launched from the solar surface, or whether the chaotic 'magnetic carpet' in the low corona energizes the system via magnetic reconnection. To help pin down the physics, we also review some key observational results from ultraviolet spectroscopy of the collisionless outer corona.
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Affiliation(s)
- Steven R Cranmer
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA Laboratory for Atmospheric and Space Physics, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 8030, USA
| | | | - Mari Paz Miralles
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
| | - John C Raymond
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
| | - Leonard Strachan
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
| | - Hui Tian
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
| | - Lauren N Woolsey
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
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Abstract
The space-based IRIS telescope provides a new window to view the solar atmosphere
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Affiliation(s)
- Louise K. Harra
- Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
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18
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De Pontieu B, van der Voort LR, McIntosh SW, Pereira TMD, Carlsson M, Hansteen V, Skogsrud H, Lemen J, Title A, Boerner P, Hurlburt N, Tarbell TD, Wuelser JP, De Luca EE, Golub L, McKillop S, Reeves K, Saar S, Testa P, Tian H, Kankelborg C, Jaeggli S, Kleint L, Martinez-Sykora J. On the prevalence of small-scale twist in the solar chromosphere and transition region. Science 2014; 346:1255732. [PMID: 25324398 DOI: 10.1126/science.1255732] [Citation(s) in RCA: 99] [Impact Index Per Article: 9.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The solar chromosphere and transition region (TR) form an interface between the Sun's surface and its hot outer atmosphere. There, most of the nonthermal energy that powers the solar atmosphere is transformed into heat, although the detailed mechanism remains elusive. High-resolution (0.33-arc second) observations with NASA's Interface Region Imaging Spectrograph (IRIS) reveal a chromosphere and TR that are replete with twist or torsional motions on sub-arc second scales, occurring in active regions, quiet Sun regions, and coronal holes alike. We coordinated observations with the Swedish 1-meter Solar Telescope (SST) to quantify these twisting motions and their association with rapid heating to at least TR temperatures. This view of the interface region provides insight into what heats the low solar atmosphere.
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Affiliation(s)
- B De Pontieu
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA. Institute of Theoretical Astrophysics, University of Oslo, Post Office Box 1029, Blindern, N-0315 Oslo, Norway.
| | - L Rouppe van der Voort
- Institute of Theoretical Astrophysics, University of Oslo, Post Office Box 1029, Blindern, N-0315 Oslo, Norway
| | - S W McIntosh
- High Altitude Observatory, National Center for Atmospheric Research, Post Office Box 3000, Boulder, CO 80307, USA
| | - T M D Pereira
- Institute of Theoretical Astrophysics, University of Oslo, Post Office Box 1029, Blindern, N-0315 Oslo, Norway
| | - M Carlsson
- Institute of Theoretical Astrophysics, University of Oslo, Post Office Box 1029, Blindern, N-0315 Oslo, Norway
| | - V Hansteen
- Institute of Theoretical Astrophysics, University of Oslo, Post Office Box 1029, Blindern, N-0315 Oslo, Norway
| | - H Skogsrud
- Institute of Theoretical Astrophysics, University of Oslo, Post Office Box 1029, Blindern, N-0315 Oslo, Norway
| | - J Lemen
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA
| | - A Title
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA
| | - P Boerner
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA
| | - N Hurlburt
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA
| | - T D Tarbell
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA
| | - J P Wuelser
- Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), 3251 Hanover Street, Organization A021S, Building 252, Palo Alto, CA 94304, USA
| | - E E De Luca
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - L Golub
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - S McKillop
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - K Reeves
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - S Saar
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - P Testa
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - H Tian
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - C Kankelborg
- Department of Physics, Montana State University, Bozeman, Post Office Box 173840, Bozeman, MT 59717, USA
| | - S Jaeggli
- Department of Physics, Montana State University, Bozeman, Post Office Box 173840, Bozeman, MT 59717, USA
| | - L Kleint
- Bay Area Environmental Research Institute, 596 1st Street West, Sonoma, CA 95476, USA
| | - J Martinez-Sykora
- Bay Area Environmental Research Institute, 596 1st Street West, Sonoma, CA 95476, USA
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