A census of coronal mass ejections on solar-like stars

Leitzinger, M.; Odert, P.; Greimel, R.; Vida, K.; Kriskovics, L.; Guenther, E. W.; Korhonen, H.; Koller, Florian; Hanslmeier, A.; Kővári, Zs.; Lämmer, H.

doi:10.1093/mnras/staa504

Cited by 39 publications

(26 citation statements)

References 110 publications

(174 reference statements)

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“…Although these models qualitatively agree that CMEs can contribute significantly to the total mass-loss rates at younger ages, observationally confirming the presence and amount of stellar CMEs is challenging and their detection has remained elusive (see, e.g., Leitzinger et al 2020, for an updated census). Given that type II radio bursts are related to CMEs in the Sun (not all CMEs produce type II bursts though), one possible way to detect stellar CMEs is through observations of radio bursts (see, e.g., Crosley et al 2016, and references therein).…”

Section: Detecting Coronal Mass Ejections (Cmes) Through Type II Radio Burstsmentioning

confidence: 90%

The evolution of the solar wind

Vidotto

2021

Living Rev Sol Phys

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How has the solar wind evolved to reach what it is today? In this review, I discuss the long-term evolution of the solar wind, including the evolution of observed properties that are intimately linked to the solar wind: rotation, magnetism and activity. Given that we cannot access data from the solar wind 4 billion years ago, this review relies on stellar data, in an effort to better place the Sun and the solar wind in a stellar context. I overview some clever detection methods of winds of solar-like stars, and derive from these an observed evolutionary sequence of solar wind mass-loss rates. I then link these observational properties (including, rotation, magnetism and activity) with stellar wind models. I conclude this review then by discussing implications of the evolution of the solar wind on the evolving Earth and other solar system planets. I argue that studying exoplanetary systems could open up new avenues for progress to be made in our understanding of the evolution of the solar wind.

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Section: Detecting Coronal Mass Ejections (Cmes) Through Type II Radio Burstsmentioning

confidence: 90%

The evolution of the solar wind

Vidotto

2021

Living Rev Sol Phys

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“…Somewhat surprisingly, given the number of superflares detected with Kepler, there have only been a small number of stellar CME candidate events (Argiroffi et al 2019;Moschou et al 2019;Vida et al 2019;Leitzinger et al 2020). To investigate the possibility that stellar CMEs are not as frequent as would be expected by extrapolating the solar flare-CME relation (Aarnio et al 2012;Drake et al 2013;Osten & Wolk 2015), Alvarado-Gómez et al (2018) illustrated using magnetohydrodynamic simulations that a strong large-scale stellar dipolar magnetic field (associated with fast rotators) may suppress CMEs below a certain energy threshold.…”

Section: From Solar To Stellar Cosmic Raysmentioning

confidence: 99%

Stellar versus Galactic: the intensity of cosmic rays at the evolving Earth and young exoplanets around Sun-like stars

Rodgers-Lee

Taylor²,

Vidotto

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Energetic particles, such as stellar cosmic rays, produced at a heightened rate by active stars (like the young Sun) may have been important for the origin of life on Earth and other exoplanets. Here we compare, as a function of stellar rotation rate (Ω), contributions from two distinct populations of energetic particles: stellar cosmic rays accelerated by impulsive flare events and Galactic cosmic rays. We use a 1.5D stellar wind model combined with a spatially 1D cosmic ray transport model. We formulate the evolution of the stellar cosmic ray spectrum as a function of stellar rotation. The maximum stellar cosmic ray energy increases with increasing rotation i.e. towards more active/younger stars. We find that stellar cosmic rays dominate over Galactic cosmic rays in the habitable zone at the pion threshold energy for all stellar ages considered (t* = 0.6 − 2.9 Gyr). However, even at the youngest age, t* = 0.6 Gyr, we estimate that ≳ 80MeV stellar cosmic ray fluxes may still be transient in time. At ∼1 Gyr when life is thought to have emerged on Earth, we demonstrate that stellar cosmic rays dominate over Galactic cosmic rays up to ∼4 GeV energies during flare events. Our results for t* =0.6 Gyr (Ω = 4Ω⊙) indicate that ≲GeV stellar cosmic rays are advected from the star to 1 au and are impacted by adiabatic losses in this region. The properties of the inner solar wind, currently being investigated by the Parker Solar Probe and Solar Orbiter, are thus important for accurate calculations of stellar cosmic rays around young Sun-like stars.

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“…The velocity of this ejected mass can vary from 60 to 3200 km s −1 with masses on the order of 10 12 kg (Benz & Güdel 2010). While CMEs are relatively easy to de-tect on our Sun, particularly if they directly impact Earth, they are far more difficult to detect on other stars and none have yet been conclusively identified (Vida et al 2019a;Leitzinger et al 2020). This primarily results from their diffuse nature and being outshined by the host star.…”

Section: Introductionmentioning

confidence: 99%

Simultaneous photometric and CARMENES spectroscopic monitoring of fast-rotating M dwarf GJ 3270

Johnson

Czesla

Fuhrmeister

et al. 2021

A&A

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Context. Active M dwarfs frequently exhibit large flares, which can pose an existential threat to the habitability of any planet in orbit in addition to making said planets more difficult to detect. M dwarfs do not lose angular momentum as easily as earlier-type stars, which maintain the high levels of stellar activity for far longer. Studying young, fast-rotating M dwarfs is key to understanding their near stellar environment and the evolution of activity. Aims. We study stellar activity on the fast-rotating M dwarf GJ 3270. Methods. We analyzed dedicated high cadence, simultaneous, photometric and high-resolution spectroscopic observations obtained with CARMENES of GJ 3270 over 7.7 h, covering a total of eight flares of which two are strong enough to facilitate a detailed analysis. We consult the TESS data, obtained in the month prior to our own observations, to study rotational modulation and to compare the TESS flares to those observed in our campaign. Results. The TESS data exhibit rotational modulation with a period of 0.37 d. The strongest flare covered by our observing campaign released a total energy of about 3.6 × 1032 erg, putting it close to the superflare regime. This flare is visible in the B,V, r, i, and z photometric bands, which allows us to determine a peak temperature of about 10 000 K. The flare also leaves clear marks in the spectral time series. In particular, we observe an evolving, mainly blue asymmetry in chromospheric lines, which we attribute to a post-flare, corotating feature. To our knowledge this is the first time such a feature has been seen on a star other than our Sun. Conclusions. Our photometric and spectroscopic time series covers the eruption of a strong flare followed up by a corotating feature analogous to a post-flare arcadal loop on the Sun with a possible failed ejection of material.

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A census of coronal mass ejections on solar-like stars

Cited by 39 publications

References 110 publications

The evolution of the solar wind

The evolution of the solar wind

Stellar versus Galactic: the intensity of cosmic rays at the evolving Earth and young exoplanets around Sun-like stars

Simultaneous photometric and CARMENES spectroscopic monitoring of fast-rotating M dwarf GJ 3270

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