Deutsch
 
Hilfe Datenschutzhinweis Impressum
  DetailsucheBrowse

Datensatz

DATENSATZ AKTIONENEXPORT
  Small-scale dynamo in cool stars. II. The effect of metallicity

Witzke, V., Duehnen, H. B., Shapiro, A. I., Przybylski, D., Bhatia, T. S., Cameron, R., et al. (2023). Small-scale dynamo in cool stars. II. The effect of metallicity. Astronomy and Astrophysics, 669, A157. doi:10.1051/0004-6361/202244771.

Item is

Basisdaten

einblenden: ausblenden:
Genre: Zeitschriftenartikel

Externe Referenzen

einblenden:
ausblenden:
externe Referenz:
https://ui.adsabs.harvard.edu/abs/2023A&A...669A.157W (beliebiger Volltext)
Beschreibung:
-
OA-Status:
Keine Angabe

Urheber

einblenden:
ausblenden:
 Urheber:
Witzke, V.1, Autor           
Duehnen, H. B., Autor
Shapiro, A. I.2, Autor           
Przybylski, D.1, Autor           
Bhatia, Tanayveer S.1, Autor           
Cameron, R.3, 4, Autor           
Solanki, S. K.1, Autor           
Affiliations:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              
2Max Planck Research Group in Solar Variability and Climate, Max Planck Institute for Solar System Research, Max Planck Society, ou_2265637              
3Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832287              
4Department Solar and Stellar Interiors, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832287              

Inhalt

einblenden:
ausblenden:
Schlagwörter: methods: numerical; magnetohydrodynamics (MHD); convection; stars: magnetic field; stars: atmospheres; stars: interiors; Astrophysics - Solar and Stellar Astrophysics
 Zusammenfassung: Context. All cool main sequence stars including our Sun are thought to have magnetic fields. Observations of the Sun revealed that small-scale turbulent magnetic fields are present even in quiet regions. Simulations further showed that such magnetic fields affect the subsurface and photospheric structure, and thus the radiative transfer and emergent flux. Since small-scale turbulent magnetic fields on other stars cannot be directly observed, it is imperative to numerically study their effects on the near surface layers.
Aims: Until recently comprehensive three-dimensional simulations capturing the effect of small-scale turbulent magnetic fields only exist for the solar case. A series of investigations extending small-scale dynamo simulations for other stars has been started. Here we aim to examine small-scale turbulent magnetic fields in stars of solar effective temperature but different metallicity.
Methods: We investigate the properties of three-dimensional simulations of the magneto-convection in boxes covering the upper convection zone and photosphere carried out with the MURaM code for metallicity values of M/H = {-1.0,0.0,0.5} with and without a small-scale dynamo.
Results: We find that small-scale turbulent magnetic fields enhanced by a small-scale turbulent dynamo noticeably affect the subsurface dynamics and significantly change the flow velocities in the photosphere. Moreover, significantly stronger magnetic field strengths are present in the convection zone for low metallicity. Instead, at the optical surface the averaged vertical magnetic field ranges from 64G for M/H = 0.5 to 85G for M/H = -1.0.

Details

einblenden:
ausblenden:
Sprache(n):
 Datum: 2023-01-272023
 Publikationsstatus: Erschienen
 Seiten: -
 Ort, Verlag, Ausgabe: -
 Inhaltsverzeichnis: -
 Art der Begutachtung: -
 Identifikatoren: DOI: 10.1051/0004-6361/202244771
ISSN: 0004-6361
 Art des Abschluß: -

Veranstaltung

einblenden:

Entscheidung

einblenden:

Projektinformation

einblenden:

Quelle 1

einblenden:
ausblenden:
Titel: Astronomy and Astrophysics
Genre der Quelle: Zeitschrift
 Urheber:
Affiliations:
Ort, Verlag, Ausgabe: -
Seiten: - Band / Heft: 669 Artikelnummer: - Start- / Endseite: A157 Identifikator: -