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Verfasst von:Ahlborn, Felix [VerfasserIn]   i
 Bellinger, Earl Patrick [VerfasserIn]   i
 Hekker, Saskia [VerfasserIn]   i
 Basu, Sarbani [VerfasserIn]   i
 Mokrytska, Daria [VerfasserIn]   i
Titel:Improved asteroseismic inversions for red-giant surface rotation rates
Verf.angabe:F. Ahlborn, E.P. Bellinger, S. Hekker, S. Basu, and D. Mokrytska
E-Jahr:2022
Jahr:Dec 8 2022
Umfang:17 S.
Illustrationen:Illustrationen, Diagramme
Fussnoten:Gesehen am 18.10.2023
Titel Quelle:Enthalten in: Astronomy and astrophysics
Ort Quelle:Les Ulis : EDP Sciences, 1969
Jahr Quelle:2022
Band/Heft Quelle:668(2022), Artikel-ID A98, Seite 1-17
ISSN Quelle:1432-0746
Abstract:Context: Asteroseismic observations of internal stellar rotation have indicated a substantial lack of angular momentum transport in theoretical models of subgiant and red-giant stars. Accurate core and surface rotation rate measurements are therefore needed to constrain the internal transport processes included in the models.Aims. We eliminate substantial systematic errors of asteroseismic surface rotation rates found in previous studies. Methods: We propose a new objective function for the optimally localised averages method of rotational inversions for red-giant stars, which results in more accurate envelope rotation rate estimates obtained from the same data. We use synthetic observations from stellar models across a range of evolutionary stages and masses to demonstrate the improvement.Results. We find that our new inversion technique allows us to obtain estimates of the surface rotation rate that are independent of the core rotation. For a star at the base of the red-giant branch, we reduce the systematic error from about 20% to a value close to 0, assuming constant envelope rotation. We also show the equivalence between this method and the method of linearised rotational splittings.Conclusions. Our new rotational inversion method substantially reduces the systematic errors of red-giant surface rotation rates. In combination with independent measures of the surface rotation rate, this will allow better constraints to be set on the internal rotation profile. This will be a very important probe for further constraining the internal angular momentum transport along the lower part of the red-giant branch.
DOI:doi:10.1051/0004-6361/202142510
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext: https://doi.org/10.1051/0004-6361/202142510
 Volltext: https://www.webofscience.com/api/gateway?GWVersion=2&SrcAuth=DOISource&SrcApp=WOS&KeyAID=10.1051%2F0004-6361%2F202142510 ...
 DOI: https://doi.org/10.1051/0004-6361/202142510
Schlagwörter:(s)Asteroseismologie   i / (s)Sternentwicklung   i / (s)Drehimpuls   i
Datenträger:Online-Ressource
Sprache:eng
Sach-SW:ANGULAR-MOMENTUM TRANSPORT
 asteroseismology
 CORE
 interiors
 INTERNAL-ROTATION
 MIXED-MODES
 oscillations
 REDISTRIBUTION
 rotation
 SPIN-DOWN
 stars
 STARS
K10plus-PPN:1866216821
Verknüpfungen:→ Zeitschrift

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