Connecting Solar and Stellar Flares CMEs Expanding Heliophysics to Encompass Exoplanetary Space Weather BENJAMIN J. LYNCH1 BRIAN E. W OOD2 MENGJIN34 TIBOR TÖRÖK5 XUDONG SUN6

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Connecting Solar and Stellar Flares/CMEs: Expanding Heliophysics

to Encompass Exoplanetary Space Weather

BENJAMIN J. LYNCH 1, BRIAN E. WOOD 2, MENG JIN 3,4, TIBOR TÖRÖK 5, XUDONG SUN 6,

ERIKA PALMERIO 5, RACHEL A. OSTEN 7, ALINE A. VIDOTTO 8, OFER COHEN 9,

JULIÁN D. ALVARADO-GÓMEZ 10, JEREMY J. DRAKE 11, VLADIMIR S. AIRAPETIAN 12,13,

YUTA NOTSU 14,15, ASTRID VERONIG 16, KOSUKE NAMEKATA 17, RÉKA M. WINSLOW 18,

LAN K. JIAN 12, ANGELOS VOURLIDAS 19, NOÉ LUGAZ 18, NADA AL-HADDAD 18,

WARD B. MANCHESTER 20, CAMILLA SCOLINI 18, CHARLES J. FARRUGIA 18,

EMMA E. DAVIES 18, TERESA NIEVES-CHINCHILLA 12, FERNANDO CARCABOSO 12,21,

CHRISTINA O. LEE 1,AND TARIK M. SALMAN 12,22

1Space Sciences Laboratory, University of California–Berkeley, Berkeley, CA 94720, USA

2Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA

3Lockheed Martin Solar and Astrophysics Laboratory, Palo Alto, CA 94304, USA

4SETI Institute, Mountain View, CA 94043, USA

5Predictive Science Inc., San Diego, CA 92121, USA

6Institute for Astronomy, University of Hawai‘i at M¯

anoa, Pukalani, HI 96768, USA

7Space Telescope Science Institute, Baltimore, MD 21218, USA

8Leiden Observatory, Leiden University, 2300 RA, Leiden, The Netherlands

9Department of Physics and Applied Physics, University of Massachusetts–Lowell, Lowell, MA 01854, USA

10Leibniz Institute for Astrophysics, 14482 Potsdam, Germany

11Smithsonian Astrophysical Observatory, Cambridge, MA 02138, USA

12Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

13American University, Washington, DC 20016 USA

14Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO 80303, USA

15National Solar Observatory, Boulder, CO 80303, USA

16Institute of Physics, University of Graz, 8010 Graz, Austria

17National Astronomical Observatory of Japan, Tokyo 181-8588, Japan

18Space Science Center, University of New Hampshire, Durham, NH 03824, USA

19Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA

20Department of Climate and Space Research, University of Michigan, Ann Arbor, MI 48109, USA

21The Catholic University of America, Washington, DC 20064, USA

22George Mason University, Fairfax, VA 22030, USA

Synopsis

The aim of this white paper is to brieﬂy summarize some of the outstanding gaps in the

observations and modeling of stellar ﬂares, CMEs, and exoplanetary space weather, and to dis-

cuss how the theoretical and computational tools and methods that have been developed in

heliophysics can play a critical role in meeting these challenges. The maturity of data-inspired

and data-constrained modeling of the Sun-to-Earth space weather chain provides a natural

starting point for the development of new, multidisciplinary research and applications to other

stars and their exoplanetary systems. Here we present recommendations for future solar CME

research to further advance stellar ﬂare and CME studies. These recommendations will require

institutional and funding agency support for both fundamental research (e.g. theoretical consid-

erations and idealized eruptive ﬂare/CME numerical modeling) and applied research (e.g. data

inspired/constrained modeling and estimating exoplanetary space weather impacts). In short,

we recommend continued and expanded support for: (1.) Theoretical and numerical studies

of CME initiation and low coronal evolution, including conﬁnement of “failed” eruptions; (2.)

Systematic analyses of Sun-as-a-star observations to develop and improve stellar CME detection

techniques and alternatives; (3.) Improvements in data-inspired and data-constrained MHD

modeling of solar CMEs and their application to stellar systems; and (4.) Encouraging com-

prehensive solar–stellar research collaborations and conferences through new interdisciplinary

and multi-agency/division funding mechanisms.

White Paper submitted to the Heliophysics 2024–2033 Decadal Survey 1

arXiv:2210.06476v1 [astro-ph.IM] 12 Oct 2022

Connecting Solar and Stellar Flares/CMEs Lynch et al.

1 Introduction

The aim of this white paper is to discuss the importance of both fundamental and applied

coronal mass ejection (CME) research in the context of its increasing relevance to stellar as-

tronomy. Interest in detecting and modeling CMEs on other stars has increased dramatically

in recent years. The winds and CMEs of coronal stars like the Sun have always been of interest

due to their role in shedding angular momentum, leading to observed declines in stellar ro-

tation and activity with age [Vidotto 2021]. However, by far the primary driver of interest in

stellar winds and CMEs these days relates to star–planet interactions and the “space weather”

impacts on exoplanetary atmospheres [Airapetian et al. 2020, and references therein].

As of March 2022, there are over 5000 conﬁrmed exoplanet discoveries [Brennan 2022].

Most of the known exoplanets orbit very close to their parent stars, meaning they are potentially

exposed to particularly high particle ﬂuxes from stellar winds to CMEs, leading to much interest

in the long-term effects this exposure has on the atmospheres of these planets. Absorption

from material evaporating from planetary atmospheres has actually been detected in cases

of transiting exoplanets, indicating the importance of this process [Vidal-Madjar et al. 2003;

Lecavelier Des Etangs et al. 2010;Ekenbäck et al. 2010;Kislyakova et al. 2014;Bourrier et al.

2016;Schneiter et al. 2016]. In our own solar system, solar wind and CME exposure may

have signiﬁcantly affected planetary atmospheric evolution, with Mars being a particularly

interesting case [Jakosky et al. 2018].

Solar and stellar ﬂares—sudden explosive releases of energy in the solar/stellar atmo-

sphere across a wide range of electromagnetic wavelengths—occur due to the rapid release

of free magnetic energy stored in the sheared and/or twisted strong ﬁelds typically associated

with sunspots and active regions [Forbes 2000;Fletcher et al. 2011;Shibata & Magara 2011;

Kazachenko et al. 2012]. The onset and evolution of solar and stellar ﬂares are intimately

coupled to magnetic reconnection processes [Klimchuk 2001;Green et al. 2018]. The long-

standing CSHKP model [Carmichael 1964;Sturrock 1966;Hirayama 1974;Kopp & Pneuman

1976]for eruptive solar ﬂares explains many of their observational properties [e.g. Janvier

et al. 2015;Török et al. 2018;Lynch et al. 2021]. Large ﬂares are often accompanied by

CMEs [Andrews 2003;Gopalswamy et al. 2005]and CMEs are largely responsible for the most

geoeffective space-weather impacts at Earth and other solar system bodies [Zhang et al. 2021].

Magnetohydrodynamic (MHD) modeling of stellar CMEs and their interactions with exo-

planets began not long after exoplanets were discovered [Khodachenko et al. 2007;Lammer

et al. 2007]. Many of these models utilize the same codes used to model solar CME prop-

agation in the heliosphere and interaction with Earth’s magnetosphere [Cohen et al. 2011;

Garraffo et al. 2016;Cherenkov et al. 2017;Lynch et al. 2019;Hazra et al. 2022]. In this

white paper, we present a brief summary of the applications of state-of-the-art MHD models

used in heliophysics to stellar magnetic environments (Section 2) and their exoplanetary sys-

tems (Section 3) in order to discuss the current observational and modeling limitations. In

Section 4, we conclude with some recommendations for future research strategies in order to

advance our understanding of the solar–stellar connection.

2 Current Theoretical and Observational Ambiguities and/or Discrepancies

2.1 Measurements of Stellar Magnetic Fields (and their Limitations)

For decades, the magnetic ﬁelds of massive, early-type stars were analyzed assuming simple

dipole or dipole-plus-quadrupole magnetic ﬁeld geometries. For late-type active stars, the de-

velopment of Zeeman–Doppler Imaging [ZDI; Donati et al. 1997;Piskunov & Kochukhov 2002;

Kochukhov 2016]and its inversion techniques has made it possible to resolve—at least on the

largest scales—surface magnetic ﬁeld distributions that can be considerably more complex and

track their long-term evolution, e.g. the polarity reversals associated with stellar activity cycles

White Paper submitted to the Heliophysics 2024–2033 Decadal Survey 2

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ConnectingSolarandStellarFlares/CMEs:ExpandingHeliophysicstoEncompassExoplanetarySpaceWeatherBENJAMINJ.LYNCH1,BRIANE.WOOD2,MENGJIN3,4,TIBORTÖRÖK5,XUDONGSUN6,ERIKAPALMERIO5,RACHELA.OSTEN7,ALINEA.VIDOTTO8,OFERCOHEN9,JULIÁND.ALVARADO-GÓMEZ10,JEREMYJ.DRAKE11,VLADIMIRS.AIRAPETIAN12,13,YUTANOTSU14,15,ASTR...

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Connecting Solar and Stellar Flares CMEs Expanding Heliophysics to Encompass Exoplanetary Space Weather BENJAMIN J. LYNCH1 BRIAN E. W OOD2 MENGJIN34 TIBOR TÖRÖK5 XUDONG SUN6

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