Integrated Mass Loss for Very Metal-poor Stars: Asterosesimic Red Giant Masses of K2 Globular Cluster NGC 5897

@misc{kalup2026integrated,
  title = {{Integrated Mass Loss for Very Metal-poor Stars: Asterosesimic Red Giant Masses of K2 Globular Cluster NGC 5897}},
  author = {Csilla Kalup and László Molnár and Madeline Howell and Attila Bódi and András Pál},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.01119},
  eprint = {2609.01119},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.01119},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - Integrated Mass Loss for Very Metal-poor Stars: Asterosesimic Red Giant Masses of K2 Globular Cluster NGC 5897
AU  - Csilla Kalup
AU  - László Molnár
AU  - Madeline Howell
AU  - Attila Bódi
AU  - András Pál
PY  - 2026
DA  - 2026/09/01
PB  - arXiv
DO  - 10.48550/arxiv.2609.01119
UR  - https://arxiv.org/abs/2609.01119
AB  - Mass loss in low-mass stars during the red giant branch (RGB) and early asymptotic giant branch (EAGB) phases plays a key role in shaping stellar evolution, yet its dependence on stellar parameters such as metallicity remains poorly constrained, with observational studies yielding conflicting trends. We present the first asteroseismic analysis of RGB and EAGB stars in NGC 5897, the most distant and metal-poor globular cluster observed by the Kepler space telescope during the K2 mission. We detected solar-like oscillations and derived the frequency of maximum power excess, ν_max, for 20 RGB and 6 EAGB stars. Using asteroseismic scaling relations, we derived mean masses of M̅_RGB = 0.74±0.01 M_⊙ and M̅_EAGB=0.65± 0.03 M_⊙. The inferred integrated mass loss between the two phases is ΔM_RGB−EAGB=0.08± 0.03 M_⊙. We present an updated mass-loss--metallicity relation for Type I globular clusters, extending it to the very metal-poor regime and supporting decreasing integrated RGB mass loss with decreasing metallicity.
ER  -