Stellar coronal mass ejections - II. Constraints from spectroscopic observations

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00534615" target="_blank" >RIV/67985815:_____/20:00534615 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1093/mnras/staa1021" target="_blank" >https://doi.org/10.1093/mnras/staa1021</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staa1021" target="_blank" >10.1093/mnras/staa1021</a>

Result language

angličtina

Original language name

Stellar coronal mass ejections - II. Constraints from spectroscopic observations

Original language description

etections of stellar coronal mass ejections (CMEs) are still rare. Observations of strong Balmer line asymmetries during flare events have been interpreted as being caused by CMEs. Here, we aim to estimate the maximum possible Balmer line fluxes expected from CMEs to infer their detectability in spectroscopic observations. Moreover, we use these results together with a model of intrinsic CME rates to infer the potentially observable CME rates for stars of different spectral types under various observing conditions, as well as the minimum required observing time to detect stellar CMEs in Balmer lines. We find that generally CME detection is favoured for mid- to late-type M dwarfs, as they require the lowest signal-to-noise ratio for CME detection, and the fraction of observable-to-intrinsic CMEs is largest. They may require, however, longer observing times than stars of earlier spectral types at the same activity level, as their predicted intrinsic CME rates are lower. CME detections are generally favoured for stars close to the saturation regime, because they are expected to have the highest intrinsic rates. The predicted minimum observing time to detect CMEs on just moderately active stars is already >100h. By comparison with spectroscopic data sets including detections as well as nondetections of CMEs, we find that our modelled maximum observable CME rates are generally consistent with these observations on adopting parameters within the ranges determined by observations of solar and stellar prominences.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA19-17102S" target="_blank" >GA19-17102S: Cool structures in solar and stellar coronae</a><br>

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2020

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Monthly Notices of the Royal Astronomical Society

ISSN

1365-2966

e-ISSN

—

Volume of the periodical

494

Issue of the periodical within the volume

3

Country of publishing house

GB - UNITED KINGDOM

Number of pages

18

Pages from-to

3766-3783

UT code for WoS article

000535882100056

EID of the result in the Scopus database

2-s2.0-85094178400