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Peer-reviewedCC BY 4.0The Astronomical Journal

Precise Physical and Kinematical Parameters of Massive Eclipsing Binaries in the Small Magellanic Cloud

  • M. Kaya1
  • Ö. Çakirli1
  • B. Hoyman1
  • O. Özdarcan1
  • T. Yontan2
  • R. Canbay3
  1. 1Ege University
  2. 2Istanbul University
  3. 3Akdeniz University
Open at sourcePDFDOICite

Abstract

The formation of massive stars serves as an important field of study, requiring research into whether these stars need to form together within clusters of low-mass stars or whether they are able to form independently. Recently, there has been an increase in the number of massive stars found far from clusters in the Milky Way and Small Magellanic Cloud (SMC). The existence of isolation and composition in binary systems is an uncommon phenomenon among massive stars, and their rare occurrence presents valuable insights that are regarded as evidence in this field. This research looks for ways to increase the catalog of identified massive stars in eclipsing binaries, particularly those that show significant indications of isolation. As a first step, we are analyzing the eight double-lined spectroscopic binaries in the SMC, as detailed in the OGLE variable star catalogs, with the goal of identifying their astrophysical properties. Then we examine the expected locations and characteristics of binary stars thought to be part of a cluster, using absolute parameters and a cross-validation approach to determine the connection between kinematic analysis and these parameters. If the kinematic connection with the cluster and the physical parameters match precisely with the cluster’s isochrone, such stars could act as reliable standard candles for determining the cluster’s distance and age.

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Cite

BibTeXRIS
BibTeX
@article{kaya2026precise,
  title = {{Precise Physical and Kinematical Parameters of Massive Eclipsing Binaries in the Small Magellanic Cloud}},
  author = {M. Kaya and Ö. Çakirli and B. Hoyman and O. Özdarcan and T. Yontan and R. Canbay},
  journal = {The Astronomical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-3881/aeaa57},
  url = {https://iopscience.iop.org/article/10.3847/1538-3881/aeaa57},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Precise Physical and Kinematical Parameters of Massive Eclipsing Binaries in the Small Magellanic Cloud
AU  - M. Kaya
AU  - Ö. Çakirli
AU  - B. Hoyman
AU  - O. Özdarcan
AU  - T. Yontan
AU  - R. Canbay
PY  - 2026
DA  - 2026/10/15
JO  - The Astronomical Journal
DO  - 10.3847/1538-3881/aeaa57
UR  - https://iopscience.iop.org/article/10.3847/1538-3881/aeaa57
AB  - The formation of massive stars serves as an important field of study, requiring research into whether these stars need to form together within clusters of low-mass stars or whether they are able to form independently. Recently, there has been an increase in the number of massive stars found far from clusters in the Milky Way and Small Magellanic Cloud (SMC). The existence of isolation and composition in binary systems is an uncommon phenomenon among massive stars, and their rare occurrence presents valuable insights that are regarded as evidence in this field. This research looks for ways to increase the catalog of identified massive stars in eclipsing binaries, particularly those that show significant indications of isolation. As a first step, we are analyzing the eight double-lined spectroscopic binaries in the SMC, as detailed in the OGLE variable star catalogs, with the goal of identifying their astrophysical properties. Then we examine the expected locations and characteristics of binary stars thought to be part of a cluster, using absolute parameters and a cross-validation approach to determine the connection between kinematic analysis and these parameters. If the kinematic connection with the cluster and the physical parameters match precisely with the cluster’s isochrone, such stars could act as reliable standard candles for determining the cluster’s distance and age.
SN  - 0004-6256
SN  - 1538-3881
ER  -