Skip to content
DraconiticResearch
Search Sources API
203,234 studies31 sourcesUpdated 22 min ago
PreprintCC BY 4.0arXiv

Exploring pulsational instabilities in the O-type supergiant HD 152249

  • Subharthi Dasgupta
  • Abhay Pratap Yadav
  • Sugyan Parida
  • Santosh Joshi
Open at sourcePDFDOICite

Abstract

Variability in O-type supergiants is a well known phenomena although their origin is not fully understood. In very massive, luminous stars, strange mode pulsations have been suggested to play a role in the variability. Here, we present a preliminary theoretical study of O-type supergiant models corresponding to the observed parameters of the star HD 152249, which shows line profile variability. Non-adiabatic linear stability analysis with respect to radial perturbations is carried out for the considered models of this star. Instabilities with growth rates of the order of dynamical timescale are found, with characteristics suggestive of strange modes. Non-linear simulations for selected models indicate that the instabilities could lead to significant envelope inflation, finite amplitude pulsation and may contribute to enhanced mass loss.

Related

  1. Hydrodynamic instabilities in long-term three-dimensional simulations of neutrino-driven supernovae of 13 red supergiant progenitors
    B. Giudici, Michael Gabler, Hans‐Thomas Janka
    Monthly Notices of the Royal Astronomical SocietyPeer-reviewedCC BY 4.0Full text18 citedHigh-energy astrophysicsCrossrefOpenAlex
  2. Study of the Ultra-Long GRB 220627A: Exploring a Possible Blue Supergiant Collapsar Origin
    Ayush Garg, Amit Shukla, Dorottya Szécsi +1
    arXivPreprintarXiv licenceFull textHigh-energy astrophysicsarXiv
  3. SN 2026dix: a nearby, transitional Type IIb/Ib supernova consistent with a warm supergiant progenitor
    Tamás Szalai, Schuyler D. Van Dyk, Dominik Bánhidi +20
    arXivPreprintCC BY 4.0Full textHigh-energy astrophysicsSolar & stellar physicsarXiv
  4. Ensemble pulsational characteristics of eclipsing binaries containing β Cep stars observed by the TESS mission
    C. I. Eze, G. Handler, M. Vanrespaille +4
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref
  5. A bright X-ray flaring event from the intermediate supergiant fast X-ray transient IGR J00370+6122 observed with NuSTAR
    L. Ducci, M. M. Serim, P. Romano +3
    Astronomy & AstrophysicsPeer-reviewedPublisher termsSolar & stellar physicsCrossref

Cite

BibTeXRIS
BibTeX
@misc{dasgupta2026exploring,
  title = {{Exploring pulsational instabilities in the O-type supergiant HD 152249}},
  author = {Subharthi Dasgupta and Abhay Pratap Yadav and Sugyan Parida and Santosh Joshi},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.09084},
  eprint = {2609.09084},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.09084},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Exploring pulsational instabilities in the O-type supergiant HD 152249
AU  - Subharthi Dasgupta
AU  - Abhay Pratap Yadav
AU  - Sugyan Parida
AU  - Santosh Joshi
PY  - 2026
DA  - 2026/09/08
PB  - arXiv
DO  - 10.48550/arxiv.2609.09084
UR  - https://arxiv.org/abs/2609.09084
AB  - Variability in O-type supergiants is a well known phenomena although their origin is not fully understood. In very massive, luminous stars, strange mode pulsations have been suggested to play a role in the variability. Here, we present a preliminary theoretical study of O-type supergiant models corresponding to the observed parameters of the star HD 152249, which shows line profile variability. Non-adiabatic linear stability analysis with respect to radial perturbations is carried out for the considered models of this star. Instabilities with growth rates of the order of dynamical timescale are found, with characteristics suggestive of strange modes. Non-linear simulations for selected models indicate that the instabilities could lead to significant envelope inflation, finite amplitude pulsation and may contribute to enhanced mass loss.
ER  -