---
res:
  bibo_abstract:
  - Magnetic fields in the stellar interiors are key candidates to explain observed
    core rotation rates inside solar-like stars along their evolution. Recently, asteroseismic
    estimates of radial magnetic field amplitudes near the hydrogen-burning shell
    (H-shell) inside about 24 red giants (RGs) have been obtained by measuring frequency
    splittings from their power spectra. Using general Lorentz-stress (magnetic) kernels,
    we investigated the potential for detectability of near-surface magnetism in a
    1.3 M⊙ star of supersolar metallicity as it evolves from a mid subgiant to a late
    subgiant into an RG. Based on these sensitivity kernels, we decompose an RG into
    three zones—deep core, H-shell, and near-surface. The subgiants instead required
    decomposition into an inner core, an outer core, and a near-surface layer. Additionally,
    we find that for a low-frequency g-dominated dipolar mode in the presence of a
    typical stable magnetic field, ∼25% of the frequency shift comes from the H-shell
    and the remaining from deeper layers. The ratio of the subsurface tangential field
    to the radial field in the H-burning shell decides if subsurface fields may be
    potentially detectable. For p-dominated dipole modes close to vmax, this ratio
    is around two orders of magnitude smaller in subgiant phases than the corresponding
    RG. Further, with the availability of magnetic kernels, we propose lower limits
    of field strengths in crucial layers in our stellar model during its evolutionary
    phases. The theoretical prescription outlined here provides the first formal way
    to devise inverse problems for stellar magnetism and can be seamlessly employed
    for slow rotators.@eng
  bibo_authorlist:
  - foaf_Person:
      foaf_givenName: Shatanik
      foaf_name: Bhattacharya, Shatanik
      foaf_surname: Bhattacharya
  - foaf_Person:
      foaf_givenName: Srijan B
      foaf_name: Das, Srijan B
      foaf_surname: Das
      foaf_workInfoHomepage: http://www.librecat.org/personId=9ce7c423-dacf-11ed-8942-e09c6cb27149
    orcid: 0000-0003-0896-7972
  - foaf_Person:
      foaf_givenName: Lisa Annabelle
      foaf_name: Bugnet, Lisa Annabelle
      foaf_surname: Bugnet
      foaf_workInfoHomepage: http://www.librecat.org/personId=d9edb345-f866-11ec-9b37-d119b5234501
    orcid: 0000-0003-0142-4000
  - foaf_Person:
      foaf_givenName: Subrata
      foaf_name: Panda, Subrata
      foaf_surname: Panda
  - foaf_Person:
      foaf_givenName: Shravan M.
      foaf_name: Hanasoge, Shravan M.
      foaf_surname: Hanasoge
  bibo_doi: 10.3847/1538-4357/ad4708
  bibo_issue: '1'
  bibo_volume: 970
  dct_date: 2024^xs_gYear
  dct_identifier:
  - UT:001270972500001
  dct_isPartOf:
  - http://id.crossref.org/issn/0004-637X
  - http://id.crossref.org/issn/1538-4357
  dct_language: eng
  dct_publisher: IOP Publishing@
  dct_title: Detectability of axisymmetric magnetic fields from the core to the surface
    of oscillating post-main-sequence stars@
...