| Name: | SHATANIK BHATTACHARYA |
| Affiliation: | Tata Institute of Fundamental Research |
| Conference ID : | ASI2024_590 |
| Title : | Detectability of axisymmetric magnetic fields from the core to the surface of oscillating post-main sequence stars |
| Authors : | Shatanik Bhattacharya, Srijan Bharati Das, Subrata Panda, Shravan M. Hanasoge, Lisa Bugnet |
| Authors Affiliation: | Shatanik Bhattacharya, Subrata Panda, Shravan M. Hanasoge Tata Institute of Fundamental Research, Mumbai-400005, India
Srijan Bharati Das Center for Astrophysics - Harvard & Smithsonian, Cambridge, Massachusettes-02138, USA
Srijan Bharati Das Institute of Science and Technology Austria, Am Campus 1, Klosterneuburg-3400, Austria
Lisa Bugnet Institute of Science and Technology Austria, Am Campus 1, Klosterneuburg-3400, Austria |
| Mode of Presentation: | Poster |
| Abstract Category : | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract : | Magnetic fields in the stellar cores are key candidates to enhance angular momentum transport, a much-needed mechanism to explain observed core rotation rates inside solar-like stars along their evolution. Very recently, estimates of core magnetic field amplitudes inside 24 red giants (RGs) were made by measuring changes in frequencies (called frequency splittings) in the eigenmodes of the stars. Such measurements have been associated with the magnitude of the radial component of the magnetic field at the hydrogen-burning shell (H-shell), as asymptotic analysis finds it dominating the asteroseismic signature. We use magnetic kernels computed using a new formalism to investigate the contribution of each component of an axisymmetric magnetic field from different layers inside post-main sequence stars to the asteroseismic signature. With access to these kernels, we selectively identify modes sensitive to different field components at different layers. This further allows us to provide critical lower amplitude limits for each field component (relative to the radial component in the H-shell) to contribute significantly to frequency splittings. We generate these kernels for a 1.3 solar mass star of super-solar metallicity in subgiant and red-giant phases and also compute magnetic splittings as expected to be observed for the different axisymmetric field configurations in these stages. |
