Modeling CME encounters at Parker Solar Probe with OSPREI: Dependence on photospheric and coronal conditions

Abstract

Context: Coronal mass ejections (CMEs) are eruptions of plasma from the Sun that travel through interplanetary space and may encounter Earth. CMEs often enclose a magnetic flux rope (MFR), the orientation of which largely determines the CME's geoeffectiveness. Current operational CME models do not model MFRs, but a number of research ones do, including the Open Solar Physics Rapid Ensemble Information (OSPREI) model. Aims: We report the sensitivity of OSPREI to a range of user-selected photospheric and coronal conditions. Methods: We model four separate CMEs observed in situ by Parker Solar Probe (PSP). We vary the input photospheric conditions using four input magnetograms (HMI Synchronic, HMI Synoptic, GONG Synoptic Zero-Point Corrected, and GONG ADAPT). To vary the coronal field reconstruction, we employ the Potential-Field Source-Surface (PFSS) model and we vary its source-surface height in the range 1.5--3.0 R${}_{\odot }$ with 0.1 R${}_{\odot }$ increments. Results: We find that both the input magnetogram and PFSS source surface often affect the evolution of the CME as it propagates through the Sun's corona into interplanetary space, and therefore the accuracy of the MFR prediction compared to in-situ data at PSP. There is no obvious best combination of input magnetogram and PFSS source surface height. Conclusions: The OSPREI model is moderately sensitive to the input photospheric and coronal conditions. Based on where the source region of the CME is located on the Sun, there may be best practices when selecting an input magnetogram to use.

19 pages, 10 figures, 1 table, accepted for publication in Astronomy & Astrophysics

References in corpus (21)

• No Trace Left Behind: Stereo Observation of a Coronal Mass Ejection without Low Coronal Signatures
• The Solar Probe Cup on Parker Solar Probe
• Strong coronal channelling and interplanetary evolution of a solar storm up to Earth and Mars
• The Open Flux Problem
• JHelioviewer - Time-dependent 3D visualisation of solar and heliospheric data
• Kinematic Evolution of a Slow CME in Corona Viewed by STEREO-B on 8 October 2007
• Global Trends of CME Deflections Based on CME and Solar Parameters
• Determining the Intrinsic CME Flux Rope Type Using Remote-sensing Solar Disk Observations
• Estimation of a Coronal Mass Ejection Magnetic Field Strength using Radio Observations of Gyrosynchrotron Radiation
• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Magnetohydrodynamics Simulation Module for the Global Solar Corona
• Implementation and validation of the FRi3D flux rope model in EUHFORIA
• Deriving CME density from remote sensing data and comparison to in-situ measurements
• CMEs and SEPs During November-December 2020: A Challenge for Real-Time Space Weather Forecasting
• CME Evolution in the Structured Heliosphere and Effects at Earth and Mars During Solar Minimum
• Using the Coronal Evolution to Successfully Forward Model CMEs' In Situ Magnetic Profiles
• Assessing the Influence of Input Magnetic Maps on Global Modeling of the Solar Wind and CME-driven Shock in the 2013 April 11 Event
• An Observationally Constrained Analytical Model for Predicting the Magnetic Field Vectors of ICMEs at 1 AU
• Evolution of interplanetary coronal mass ejection complexity: a numerical study through a swarm of simulated spacecraft
• Investigating Remote-sensing Techniques to Reveal Stealth Coronal Mass Ejections
• An elliptic expansion of the potential field source surface model
• Evolution of CME Properties in the Inner Heliosphere: Prediction for Solar Orbiter and Parker Solar Probe