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Title: CHROMOSPHERE TO 1 au SIMULATION OF THE 2011 MARCH 7th EVENT: A COMPREHENSIVE STUDY OF CORONAL MASS EJECTION PROPAGATION

Abstract

We perform and analyze the results of a global magnetohydrodynamic simulation of the fast coronal mass ejection (CME) that occurred on 2011 March 7. The simulation is made using the newly developed Alfvén Wave Solar Model (AWSoM), which describes the background solar wind starting from the upper chromosphere and extends to 24 R {sub ⊙}. Coupling AWSoM to an inner heliosphere model with the Space Weather Modeling Framework extends the total domain beyond the orbit of Earth. Physical processes included in the model are multi-species thermodynamics, electron heat conduction (both collisional and collisionless formulations), optically thin radiative cooling, and Alfvén-wave turbulence that accelerates and heats the solar wind. The Alfvén-wave description is physically self-consistent, including non-Wentzel–Kramers–Brillouin reflection and physics-based apportioning of turbulent dissipative heating to both electrons and protons. Within this model, we initiate the CME by using the Gibson-Low analytical flux rope model and follow its evolution for days, in which time it propagates beyond STEREO A . A detailed comparison study is performed using remote as well as in situ observations. Although the flux rope structure is not compared directly due to lack of relevant ejecta observation at 1 au in this event, our results show that themore » new model can reproduce many of the observed features near the Sun (e.g., CME-driven extreme ultraviolet [EUV] waves, deflection of the flux rope from the coronal hole, “double-front” in the white light images) and in the heliosphere (e.g., shock propagation direction, shock properties at STEREO A ).« less

Authors:
 [1]; ; ; ; ;  [2];  [3];  [4]
  1. Lockheed Martin Solar and Astrophysics Lab, Palo Alto, CA 94304 (United States)
  2. Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI 48109 (United States)
  3. The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 (United States)
  4. Cooperative Institute for Research in Environmental Sciences, University of Colorado, Boulder, CO 80309 (United States)
Publication Date:
OSTI Identifier:
22661374
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 834; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ALFVEN WAVES; CHROMOSPHERE; EXTREME ULTRAVIOLET RADIATION; HELIOSPHERE; MAGNETOHYDRODYNAMICS; ORBITS; RADIATIVE COOLING; REFLECTION; SOLAR ELECTRONS; SOLAR PROTONS; SOLAR WIND; STAR MODELS; SUN; THERMAL CONDUCTION; TURBULENCE; VISIBLE RADIATION; WKB APPROXIMATION

Citation Formats

Jin, M., Manchester, W. B., Holst, B. van der, Sokolov, I., Tóth, G., Gombosi, T. I., Vourlidas, A., and Koning, C. A. de, E-mail: jinmeng@lmsal.com, E-mail: chipm@umich.edu, E-mail: angelos.vourlidas@jhuapl.edu, E-mail: curt.a.dekoning@noaa.gov. CHROMOSPHERE TO 1 au SIMULATION OF THE 2011 MARCH 7th EVENT: A COMPREHENSIVE STUDY OF CORONAL MASS EJECTION PROPAGATION. United States: N. p., 2017. Web. doi:10.3847/1538-4357/834/2/172.
Jin, M., Manchester, W. B., Holst, B. van der, Sokolov, I., Tóth, G., Gombosi, T. I., Vourlidas, A., & Koning, C. A. de, E-mail: jinmeng@lmsal.com, E-mail: chipm@umich.edu, E-mail: angelos.vourlidas@jhuapl.edu, E-mail: curt.a.dekoning@noaa.gov. CHROMOSPHERE TO 1 au SIMULATION OF THE 2011 MARCH 7th EVENT: A COMPREHENSIVE STUDY OF CORONAL MASS EJECTION PROPAGATION. United States. doi:10.3847/1538-4357/834/2/172.
Jin, M., Manchester, W. B., Holst, B. van der, Sokolov, I., Tóth, G., Gombosi, T. I., Vourlidas, A., and Koning, C. A. de, E-mail: jinmeng@lmsal.com, E-mail: chipm@umich.edu, E-mail: angelos.vourlidas@jhuapl.edu, E-mail: curt.a.dekoning@noaa.gov. Tue . "CHROMOSPHERE TO 1 au SIMULATION OF THE 2011 MARCH 7th EVENT: A COMPREHENSIVE STUDY OF CORONAL MASS EJECTION PROPAGATION". United States. doi:10.3847/1538-4357/834/2/172.
@article{osti_22661374,
title = {CHROMOSPHERE TO 1 au SIMULATION OF THE 2011 MARCH 7th EVENT: A COMPREHENSIVE STUDY OF CORONAL MASS EJECTION PROPAGATION},
author = {Jin, M. and Manchester, W. B. and Holst, B. van der and Sokolov, I. and Tóth, G. and Gombosi, T. I. and Vourlidas, A. and Koning, C. A. de, E-mail: jinmeng@lmsal.com, E-mail: chipm@umich.edu, E-mail: angelos.vourlidas@jhuapl.edu, E-mail: curt.a.dekoning@noaa.gov},
abstractNote = {We perform and analyze the results of a global magnetohydrodynamic simulation of the fast coronal mass ejection (CME) that occurred on 2011 March 7. The simulation is made using the newly developed Alfvén Wave Solar Model (AWSoM), which describes the background solar wind starting from the upper chromosphere and extends to 24 R {sub ⊙}. Coupling AWSoM to an inner heliosphere model with the Space Weather Modeling Framework extends the total domain beyond the orbit of Earth. Physical processes included in the model are multi-species thermodynamics, electron heat conduction (both collisional and collisionless formulations), optically thin radiative cooling, and Alfvén-wave turbulence that accelerates and heats the solar wind. The Alfvén-wave description is physically self-consistent, including non-Wentzel–Kramers–Brillouin reflection and physics-based apportioning of turbulent dissipative heating to both electrons and protons. Within this model, we initiate the CME by using the Gibson-Low analytical flux rope model and follow its evolution for days, in which time it propagates beyond STEREO A . A detailed comparison study is performed using remote as well as in situ observations. Although the flux rope structure is not compared directly due to lack of relevant ejecta observation at 1 au in this event, our results show that the new model can reproduce many of the observed features near the Sun (e.g., CME-driven extreme ultraviolet [EUV] waves, deflection of the flux rope from the coronal hole, “double-front” in the white light images) and in the heliosphere (e.g., shock propagation direction, shock properties at STEREO A ).},
doi = {10.3847/1538-4357/834/2/172},
journal = {Astrophysical Journal},
number = 2,
volume = 834,
place = {United States},
year = {Tue Jan 10 00:00:00 EST 2017},
month = {Tue Jan 10 00:00:00 EST 2017}
}