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Title: Modeling solar wind with boundary conditions from interplanetary scintillations

Journal Article · · Journal of Physics. Conference Series
 [1];  [1];  [1];  [2];  [3]
  1. Univ. of Alabama, Huntsville, AL (United States). Center for Space Plasma and Aeronomic Research
  2. AFRL/RCBXS (United States)
  3. Tata Inst. of Fundamental Research, Bombay (India). Radio Astronomy Centre, NCRA
+ Show Author Affiliations

Interplanetary scintillations make it possible to create three-dimensional, time- dependent distributions of the solar wind velocity. Combined with the magnetic field observations in the solar photosphere, they help perform solar wind simulations in a genuinely time-dependent way. Interplanetary scintillation measurements from the Ooty Radio Astronomical Observatory in India provide directions to multiple stars and may assure better resolution of transient processes in the solar wind. In this paper, we present velocity distributions derived from Ooty observations and compare them with those obtained with the Wang-Sheeley-Arge (WSA) model. We also present our simulations of the solar wind flow from 0.1 AU to 1 AU with the boundary conditions based on both Ooty and WSA data.

Research Organization:
Univ. of Alabama, Huntsville, AL (United States)
Sponsoring Organization:
USDOE Office of Science (SC), Fusion Energy Sciences (FES); National Science Foundation (NSF)
Grant/Contract Number:
SC0008334; OCI-1144120
OSTI ID:
1326077
Journal Information:
Journal of Physics. Conference Series, Vol. 642; ISSN 1742-6588
Publisher:
IOP PublishingCopyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 8 works
Citation information provided by
Web of Science

References (13)

Magnetic fields and the structure of the solar corona: I: Methods of calculating coronal fields journal September 1969
Modeling the corona and solar wind using ADAPT maps that include far-side observations
  • Arge, C. Nick; Henney, Carl J.; Hernandez, Irene Gonzalez
  • SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference, AIP Conference Proceedings https://doi.org/10.1063/1.4810977
conference January 2013
Air Force Data Assimilative Photospheric Flux Transport (ADAPT) Model conference January 2010
Stream structure and coronal sources of the solar wind during the May 12th, 1997 CME journal October 2004
Improved Method for Specifying Solar Wind Speed Near the Sun conference January 2003
Improvement in the prediction of solar wind conditions using near-real time solar magnetic field updates journal May 2000
3-D reconstructions of the early-November 2004 CDAW geomagnetic storms: analysis of Ooty IPS speed and density data journal January 2009
Three-dimensional structure of the solar wind: Variation of density with the solar cycle journal November 1993
Ooty Interplanetary Scintillation – Remote-Sensing Observations and Analysis of Coronal Mass Ejections in the Heliosphere journal July 2010
THREE-DIMENSIONAL FEATURES OF THE OUTER HELIOSPHERE DUE TO COUPLING BETWEEN THE INTERSTELLAR AND INTERPLANETARY MAGNETIC FIELDS. IV. SOLAR CYCLE MODEL BASED ON ULYSSES OBSERVATIONS journal June 2013
A model of interplanetary and coronal magnetic fields journal March 1969
Large Steerable Radio Telescope at Ootacamund, India journal April 1971
On potential field models of the solar corona journal June 1992

Cited By (2)

Modeling Coronal Mass Ejections with the Multi-Scale Fluid-Kinetic Simulation Suite journal May 2017
Data-driven Modeling of the Solar Corona by a New Three-dimensional Path-conservative Osher–Solomon MHD Model journal November 2017

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79 ASTRONOMY AND ASTROPHYSICS