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Modeling Balmer line signatures of stellar CMEs

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00558361" target="_blank" >RIV/67985815:_____/22:00558361 - isvavai.cz</a>

  • Result on the web

    <a href="https://doi.org/10.1093/mnras/stac1284" target="_blank" >https://doi.org/10.1093/mnras/stac1284</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.1093/mnras/stac1284" target="_blank" >10.1093/mnras/stac1284</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    Modeling Balmer line signatures of stellar CMEs

  • Original language description

    From the Sun, we know that coronal mass ejections (CMEs) are a transient phenomenon, often correlated with flares. They have an impact on solar mass- and angular momentum loss, and therefore solar evolution, and make a significant part of space weather. The same is true for stars, but stellar CMEs are still not well constrained, although new methodologies have been established, and new detections presented in the recent past. So far, probable detections of stellar CMEs have been presented, but their physical parameters which are not directly accessible from observations, such as electron density, optical thickness, temperature, etc., have been so far not determined for the majority of known events. We apply cloud modeling, as commonly used on the Sun, to a known event from the literature, detected on the young dMe star V374 Peg. This event manifests itself in extra emission on the blue side of the Balmer lines. By determining the line source function from 1D NLTE modeling together with the cloud model formulation, we present distributions of physical parameters of this event. We find that except for temperature and area all parameters are at the upper range of typical solar prominence parameters. The temperature and the area of the event were found to be higher than for typical solar prominences observed in Balmer lines. We find more solutions for the filament than for the prominence geometry. Moreover, we show that filaments can appear in emission on dMe stars contrary to the solar case.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - 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)

Result continuities

  • Project

    Result was created during the realization of more than one project. More information in the Projects tab.

  • Continuities

    I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Others

  • Publication year

    2022

  • Confidentiality

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

Data specific for result type

  • Name of the periodical

    Monthly Notices of the Royal Astronomical Society

  • ISSN

    0035-8711

  • e-ISSN

    1365-2966

  • Volume of the periodical

    513

  • Issue of the periodical within the volume

    4

  • Country of publishing house

    GB - UNITED KINGDOM

  • Number of pages

    16

  • Pages from-to

    6058-6073

  • UT code for WoS article

    000804922600015

  • EID of the result in the Scopus database

    2-s2.0-85133432556