Solar-MACH An open-source tool to analyze solar magnetic connection conﬁgurations Jan Gieseler1 Nina Dresing1 Christian Palmroos1 Johan L. Freiherr von

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Solar-MACH: An open-source tool to analyze

solar magnetic connection conﬁgurations

Jan Gieseler 1,∗, Nina Dresing 1, Christian Palmroos 1, Johan L. Freiherr von

Forstner 2,3, Daniel J. Price 4, Rami Vainio 1, Athanasios Kouloumvakos 5,

Laura Rodr´ıguez-Garc´ıa 6, Domenico Trotta 7, Vincent G´

enot 8, Arnaud

Masson 9, Markus Roth 10, Astrid Veronig 11

1Space Research Laboratory, Department of Physics and Astronomy, University of

Turku, Turku, Finland

2Institute of Experimental and Applied Physics, Kiel University, Kiel, Germany

3Now at Paradox Cat GmbH, M¨

unchen, Germany

4Department of Physics, University of Helsinki, Helsinki, Finland

5Applied Physics Laboratory, The Johns Hopkins University, Laurel, MD, USA

6Universidad de Alcal ´

a, Space Research Group, Alcal´

a de Henares, Madrid, Spain

The Blackett Laboratory, Department of Physics, Imperial College London, London

8Institut de Recherche en Astrophysique et Plan´

etologie, CNRS, CNES, Universit´

Paul Sabatier, Toulouse, France

9ESAC Science Data Centre, European Space Agency, Madrid, Spain

10Th ¨

uringer Landessternwarte, Tautenburg, Germany

11Institute of Physics & Kanzelh ¨

ohe Observatory for Solar and Atmospheric

Research, University of Graz, Austria

Correspondence*:

Jan Gieseler, University of Turku, 20500 Turku, Finland

jan.gieseler@utu.ﬁ

ABSTRACT

The Solar MAgnetic Connection HAUS

tool (Solar-MACH) is an open-source tool completely

written in Python that derives and visualizes the spatial conﬁguration and solar magnetic

connection of different observers (i.e., spacecraft or planets) in the heliosphere at different times.

For doing this, the magnetic connection in the interplanetary space is obtained by the classic

Parker Heliospheric Magnetic Field (HMF). In close vicinity of the Sun, a Potential Field Source

Surface (PFSS) model can be applied to connect the HMF to the solar photosphere. Solar-MACH

is especially aimed at providing publication-ready ﬁgures for the analyses of Solar Energetic

Particle events (SEPs) or solar transients such as Coronal Mass Ejections (CMEs). It is provided

as an installable Python package (listed on PyPI and conda-forge), but also as a web tool at solar-

mach.github.io that completely runs in any web browser and requires neither Python knowledge

nor installation. The development of Solar-MACH is open to everyone and takes place on GitHub,

where the source code is publicly available under the BSD 3-Clause License. Established Python

libraries like

sunpy

and

pfsspy

are utilized to obtain functionalities when possible. In this article,

1Heliophysics Archives USer group at ESA

arXiv:2210.00819v2 [astro-ph.SR] 12 Jan 2023

Gieseler et al. Solar-MACH

the Python code of Solar-MACH is explained, and its functionality is demonstrated using real

science examples. In addition, we introduce the overarching SERPENTINE project, the umbrella

under which the recent development took place.

Keywords: Python, Software Package, Solar Energetic Particle (SEP), Corona, PFSS, Coronal Mass Ejection (CME), Spacecraft,

Heliosphere

1 INTRODUCTION

The Solar energetic particle analysis platform for the inner heliosphere (SERPENTINE, 2021–2024) is a

42-month long project funded through the H2020-SPACE-2020 call of the European Union’s Horizon 2020

framework programme. The project addresses several outstanding questions on the origin of solar energetic

particle (SEP) events and provides an advanced data analysis and visualization platform that will beneﬁt

the whole heliophysics community. It utilizes the most recent European and US missions, i.e., Solar Orbiter

uller et al., 2020), Parker Solar Probe (Fox et al., 2016) and BepiColombo (Benkhoff et al., 2021). These

observations are complemented with supporting data from several current missions near Earth’s orbit as

well as ground-based radio imaging and spectroscopic observations by the European Low Frequency Array

(LOFAR; van Haarlem et al., 2013).

SEP events are large and sporadic outbursts of charged particle radiation from the solar corona that are

related to solar eruptions such as ﬂares and coronal mass ejections (CMEs; e.g., Reames, 1999). They

can be classiﬁed as impulsive and gradual events, based on their duration and the duration of the related

solar X-ray ﬂare. Impulsive SEP events are associated with impulsive ﬂares and narrow CMEs, and they

are enriched in electrons,

He isotope and heavy ions. Gradual SEP events are associated with gradual

solar X-ray ﬂares and fast and wide CMEs, and their abundances resemble nominal coronal abundances

(Reames, 2013; Desai and Giacalone, 2016). Gradual events are usually broader in their helio-longitudinal

extent than impulsive events and their intensities are also typically larger, making them the main concern

of spacecraft operations and crews (Vainio et al., 2009).

The primary reason for the broad spatial extent of some gradual events is still unresolved. It could be due

to a broad source, like a global coronal shock driven by a CME (e.g., Lario et al., 2016), due to efﬁcient

particle transport processes across the heliospheric magnetic ﬁeld, or as a result of both mechanisms (e.g.,

Dresing et al., 2012; Rodr

ıguez-Garc

ıa et al., 2021). The main objective of SERPENTINE is to pinpoint

the primary causes of large gradual and widespread SEP events. To address this objective, SERPENTINE

will answer the following open science questions:

Q1: What are the primary causes for widespread SEP events observed in the heliosphere?

Q2:

What are the shock acceleration mechanisms responsible for accelerating ions from

thermal/suprathermal energies to near-relativistic energies in the corona and in the interplanetary

medium?

Q3:

What is the role of shocks in electron acceleration in large gradual and widespread events? How does

it relate to ion acceleration and what is its importance relative to ﬂare acceleration?

To reach these goals and also to broaden the impact of the project, SERPENTINE will develop and

release to the community a platform of tools for analyzing SEP events. Furthermore, the tools may also

be useful for the broader heliospheric community looking at different aspects of solar activity or solar

wind phenomena. Part of this platform will be a JupyterHub server that provides free access to the tools

developed by the SERPENTINE project as Jupyter Notebooks, without requiring any installations beyond

Gieseler et al. Solar-MACH

a web browser. This manuscript and the accompanying papers (Kouloumvakos et al., 2022; Palmroos et al.,

2022; Trotta et al., 2022) will present the ﬁrst batch of these tools to the heliophysics community.

Because SEPs are measured in situ as enhancements of the energetic particle ﬂuxes, the presence of

multiple, well-separated observers is indispensable to study widespread SEP events (e.g., Dresing et al.,

2014; Richardson et al., 2014). The new space missions in combination with established spacecraft form a

ﬂeet that is ideal for this purpose, as it covers varying heliocentric distances and large longitudinal ranges

around the Sun. The different orbits of the multiple spacecraft, in combination with varying source regions

at the Sun, constantly form new constellations, building the baseline for in-depth SEP event analyses. The

ﬁrst released tool of SERPENTINE, Solar-MACH, provides the user with a quick overview of these speciﬁc

constellations for a selected time, as shown in the example of Fig. 1. “Solar-MACH” is an abbreviation for

Solar MAgnetic Connection HAUS, with HAUS standing for the Heliophysics Archives USer group at ESA.

“MACH” is intended to be pronounced like the Mach number.

Figure 1.

Solar-MACH plot for the time of the ground-level enhancement (GLE) event on 28 October

2021. Numbered symbols indicate the observers’ locations and the spiral lines corresponding HMF lines

connecting them to the Sun. Radial distance is provided in astronomical units (AU), and the angular

information is given in Carrington longitude. The arrow points out the freely choosable location of a

“reference” (e.g., a solar ﬂare) at the Sun, and the dashed spiral line indicates a corresponding HMF line

originating at that position.

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Solar-MACH:Anopen-sourcetooltoanalyzesolarmagneticconnectioncongurationsJanGieseler1;,NinaDresing1,ChristianPalmroos1,JohanL.FreiherrvonForstner2;3,DanielJ.Price4,RamiVainio1,AthanasiosKouloumvakos5,LauraRodr´guez-Garc´a6,DomenicoTrotta7,VincentG´enot8,ArnaudMasson9,MarkusRoth10,AstridVeronig111...

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Solar-MACH An open-source tool to analyze solar magnetic connection conﬁgurations Jan Gieseler1 Nina Dresing1 Christian Palmroos1 Johan L. Freiherr von

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